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Sample records for prominent spasmodic dysphonia

  1. Research Priorities in Spasmodic Dysphonia

    PubMed Central

    Ludlow, Christy L.; Adler, Charles H.; Berke, Gerald S.; Bielamowicz, Steven A.; Blitzer, Andrew; Bressman, Susan B.; Hallett, Mark; Jinnah, H. A.; Juergens, Uwe; Martin, Sandra B.; Perlmutter, Joel S.; Sapienza, Christine; Singleton, Andrew; Tanner, Caroline M.; Woodson, Gayle E.

    2009-01-01

    OBJECTIVE To identify research priorities for increasing understanding of the pathogenesis, diagnosis and improved treatment of spasmodic dysphonia. STUDY DESIGN AND SETTING A multidisciplinary working group was formed including both scientists and clinicians from multiple disciplines, otolaryngology, neurology, speech pathology, genetics and neuroscience, to review currently available information on spasmodic dysphonia and to identify research priorities. RESULTS Operational definitions for spasmodic dysphonia at different levels of certainty were recommended for diagnosis and recommendations made for a multi-center multidisciplinary validation study. CONCLUSIONS The highest priority is to characterize the disorder and identify risk factors that may contribute to its onset. Future research should compare and contrast spasmodic dysphonia with other forms of focal dystonia. Development of animal models is recommended to explore hypotheses related to pathogenesis. Improved understanding of the pathophysiology of SD should provide the basis for developing new treatment options and exploratory clinical trials. SIGNIFICANCE This document should foster future research to improve the care of patients with this chronic debilitating voice and speech disorder by otolaryngology, neurology, and speech pathology. PMID:18922334

  2. Speech Intelligibility in Severe Adductor Spasmodic Dysphonia

    ERIC Educational Resources Information Center

    Bender, Brenda K.; Cannito, Michael P.; Murry, Thomas; Woodson, Gayle E.

    2004-01-01

    This study compared speech intelligibility in nondisabled speakers and speakers with adductor spasmodic dysphonia (ADSD) before and after botulinum toxin (Botox) injection. Standard speech samples were obtained from 10 speakers diagnosed with severe ADSD prior to and 1 month following Botox injection, as well as from 10 age- and gender-matched…

  3. Disfluency in Spasmodic Dysphonia: A Multivariate Analysis.

    ERIC Educational Resources Information Center

    Cannito, Michael P.; Burch, Annette Renee; Watts, Christopher; Rappold, Patrick W.; Hood, Stephen B.; Sherrard, Kyla

    1997-01-01

    This study examined visual analog scaling judgments of disfluency by normal listeners in response to oral reading by 20 adults with spasmodic dysphonia (SD) and nondysphonic controls. Findings suggest that although dysfluency is not a defining feature of SD, it does contribute significantly to the overall clinical impression of severity of the…

  4. Midline lateralization thyroplasty for adductor spasmodic dysphonia.

    PubMed

    Isshiki, N; Tsuji, D H; Yamamoto, Y; Iizuka, Y

    2000-02-01

    Midline lateralization thyroplasty was successfully performed on a patient with adductor spasmodic dysphonia. The thyroid cartilage was incised at the midline, and a 3 x 2-mm perforation was made at the anterior commissure to widen it. The perforation was closed with a free composite graft taken from the upper edge of the thyroid ala, and the incised thyroid cartilage edges were kept separated 4 mm apart with silicone wedges. A part of the sternohyoid muscle was rotated to seal any leak from the perforation. The postoperative course was uneventful. The voice has been restored to normal, and there is no sign of recurrence of the symptom so far, as of 1 year 5 months postoperative. Although a longer follow-up is needed, this case indicates that midline type II thyroplasty could be a useful treatment for adductor spasmodic dysphonia. PMID:10685572

  5. Emotional Considerations in Spasmodic Dysphonia: Psychometric Quantification.

    ERIC Educational Resources Information Center

    Cannito, Michael P.

    1991-01-01

    This study examined emotional characteristics of 18 female spasmodic dysphonic subjects in comparison to matched normal controls across psychometric measures of depression, anxiety, and somatic complaints. Statistically significant differences were noted between groups for all measures and over half of the dysphonic subjects exhibited clinically…

  6. Treatment for spasmodic dysphonia: limitations of current approaches

    PubMed Central

    Ludlow, Christy L.

    2009-01-01

    Purpose of review Although botulinum toxin injection is the gold standard for treatment of spasmodic dysphonia, surgical approaches aimed at providing long-term symptom control have been advancing over recent years. Recent findings When surgical approaches provide greater long-term benefits to symptom control, they also increase the initial period of side effects of breathiness and swallowing difficulties. However, recent analyses of quality-of-life questionnaires in patients undergoing regular injections of botulinum toxin demonstrate that a large proportion of patients have limited relief for relatively short periods due to early breathiness and loss-of-benefit before reinjection. Summary Most medical and surgical approaches to the treatment of spasmodic dysphonia have been aimed at denervation of the laryngeal muscles to block symptom expression in the voice, and have both adverse effects as well as treatment benefits. Research is needed to identify the central neuropathophysiology responsible for the laryngeal muscle spasms in order target treatment towards the central neurological abnormality responsible for producing symptoms. PMID:19337127

  7. Adductor spasmodic dysphonia: Relationships between acoustic indices and perceptual judgments

    NASA Astrophysics Data System (ADS)

    Cannito, Michael P.; Sapienza, Christine M.; Woodson, Gayle; Murry, Thomas

    2003-04-01

    This study investigated relationships between acoustical indices of spasmodic dysphonia and perceptual scaling judgments of voice attributes made by expert listeners. Audio-recordings of The Rainbow Passage were obtained from thirty one speakers with spasmodic dysphonia before and after a BOTOX injection of the vocal folds. Six temporal acoustic measures were obtained across 15 words excerpted from each reading sample, including both frequency of occurrence and percent time for (1) aperiodic phonation, (2) phonation breaks, and (3) fundamental frequency shifts. Visual analog scaling judgments were also obtained from six voice experts using an interactive computer interface to quantify four voice attributes (i.e., overall quality, roughness, brokenness, breathiness) in a carefully psychoacoustically controlled environment, using the same reading passages as stimuli. Number and percent aperiodicity and phonation breaks correlated significanly with perceived overall voice quality, roughness, and brokenness before and after the BOTOX injection. Breathiness was correlated with aperidocity only prior to injection, while roughness also correlated with frequency shifts following injection. Factor analysis reduced perceived attributes to two principal components: glottal squeezing and breathiness. The acoustic measures demonstrated a strong regression relationship with perceived glottal squeezing, but no regression relationship with breathiness was observed. Implications for an analysis of pathologic voices will be discussed.

  8. Botulinum Toxin in Secondarily Nonresponsive Patients with Spasmodic Dysphonia.

    PubMed

    Mor, Niv; Tang, Christopher; Blitzer, Andrew

    2016-09-01

    Chemodenervation with botulinum toxin (BoNT) has been effective and well tolerated for all types of dystonia for >30 years. We reviewed outcomes of our patients treated with BoNT serotype A (BoNT-A) for spasmodic dysphonia (SD) who became secondarily nonresponsive. We found that 8 of 1400 patients became nonresponsive to BoNT-A (0.57%), which is lower than the secondary nonresponse rate in other dystonias. After a cessation period, 4 of our patients resumed BoNT-A injections, and recurrence of immunoresistance was not seen in any of them. When compared with patients with other dystonias, patients with SD receive extremely low doses of BoNT. Small antigen challenge may explain the lower rate of immunoresistance and long-lasting efficacy after BoNT-A is restarted among secondary nonresponsive patients with SD. PMID:27143711

  9. Spasmodic Dysphonia: a Laryngeal Control Disorder Specific to Speech

    PubMed Central

    Ludlow, Christy L.

    2016-01-01

    Spasmodic dysphonia (SD) is a rare neurological disorder that emerges in middle age, is usually sporadic, and affects intrinsic laryngeal muscle control only during speech. Spasmodic bursts in particular laryngeal muscles disrupt voluntary control during vowel sounds in adductor SD and interfere with voice onset after voiceless consonants in abductor SD. Little is known about its origins; it is classified as a focal dystonia secondary to an unknown neurobiological mechanism that produces a chronic abnormality of laryngeal motor neuron regulation during speech. It develops primarily in females and does not interfere with breathing, crying, laughter, and shouting. Recent postmortem studies have implicated the accumulation of clusters in the parenchyma and perivascular regions with inflammatory changes in the brainstem in one to two cases. A few cases with single mutations in THAP1, a gene involved in transcription regulation, suggest that a weak genetic predisposition may contribute to mechanisms causing a nonprogressive abnormality in laryngeal motor neuron control for speech but not for vocal emotional expression. Research is needed to address the basic cellular and proteomic mechanisms that produce this disorder to provide intervention that could target the pathogenesis of the disorder rather than only providing temporary symptom relief. PMID:21248101

  10. Abnormal Striatal Dopaminergic Neurotransmission during Rest and Task Production in Spasmodic Dysphonia

    PubMed Central

    Berman, Brian D.; Herscovitch, Peter; Hallett, Mark

    2013-01-01

    Spasmodic dysphonia is a primary focal dystonia characterized by involuntary spasms in the laryngeal muscles during speech production. The pathophysiology of spasmodic dysphonia is thought to involve structural and functional abnormalities in the basal ganglia–thalamo-cortical circuitry; however, neurochemical correlates underpinning these abnormalities as well as their relations to spasmodic dysphonia symptoms remain unknown. We used positron emission tomography with the radioligand [11C]raclopride (RAC) to study striatal dopaminergic neurotransmission at the resting state and during production of symptomatic sentences and asymptomatic finger tapping in spasmodic dysphonia patients. We found that patients, compared to healthy controls, had bilaterally decreased RAC binding potential (BP) to striatal dopamine D2/D3 receptors on average by 29.2%, which was associated with decreased RAC displacement (RAC ΔBP) in the left striatum during symptomatic speaking (group average difference 10.2%), but increased RAC ΔBP in the bilateral striatum during asymptomatic tapping (group average difference 10.1%). Patients with more severe voice symptoms and subclinically longer reaction time to initiate the tapping sequence had greater RAC ΔBP measures, while longer duration of spasmodic dysphonia was associated with a decrease in task-induced RAC ΔBP. Decreased dopaminergic transmission during symptomatic speech production may represent a disorder-specific pathophysiological trait involved in symptom generation, whereas increased dopaminergic function during unaffected task performance may be explained by a compensatory adaptation of the nigrostriatal dopaminergic system possibly due to decreased striatal D2/D3 receptor availability. These changes can be linked to the clinical and subclinical features of spasmodic dysphonia and may represent the neurochemical basis of basal ganglia alterations in this disorder. PMID:24027271

  11. Abnormal striatal dopaminergic neurotransmission during rest and task production in spasmodic dysphonia.

    PubMed

    Simonyan, Kristina; Berman, Brian D; Herscovitch, Peter; Hallett, Mark

    2013-09-11

    Spasmodic dysphonia is a primary focal dystonia characterized by involuntary spasms in the laryngeal muscles during speech production. The pathophysiology of spasmodic dysphonia is thought to involve structural and functional abnormalities in the basal ganglia-thalamo-cortical circuitry; however, neurochemical correlates underpinning these abnormalities as well as their relations to spasmodic dysphonia symptoms remain unknown. We used positron emission tomography with the radioligand [(11)C]raclopride (RAC) to study striatal dopaminergic neurotransmission at the resting state and during production of symptomatic sentences and asymptomatic finger tapping in spasmodic dysphonia patients. We found that patients, compared to healthy controls, had bilaterally decreased RAC binding potential (BP) to striatal dopamine D2/D3 receptors on average by 29.2%, which was associated with decreased RAC displacement (RAC ΔBP) in the left striatum during symptomatic speaking (group average difference 10.2%), but increased RAC ΔBP in the bilateral striatum during asymptomatic tapping (group average difference 10.1%). Patients with more severe voice symptoms and subclinically longer reaction time to initiate the tapping sequence had greater RAC ΔBP measures, while longer duration of spasmodic dysphonia was associated with a decrease in task-induced RAC ΔBP. Decreased dopaminergic transmission during symptomatic speech production may represent a disorder-specific pathophysiological trait involved in symptom generation, whereas increased dopaminergic function during unaffected task performance may be explained by a compensatory adaptation of the nigrostriatal dopaminergic system possibly due to decreased striatal D2/D3 receptor availability. These changes can be linked to the clinical and subclinical features of spasmodic dysphonia and may represent the neurochemical basis of basal ganglia alterations in this disorder. PMID:24027271

  12. Acoustic Variations in Adductor Spasmodic Dysphonia as a Function of Speech Task.

    ERIC Educational Resources Information Center

    Sapienza, Christine M.; Walton, Suzanne; Murry, Thomas

    1999-01-01

    Acoustic phonatory events were identified in 14 women diagnosed with adductor spasmodic dysphonia (ADSD), a focal laryngeal dystonia that disturbs phonatory function, and compared with those of 14 age-matched women with no vocal dysfunction. Findings indicated ADSD subjects produced more aberrant acoustic events than controls during tasks of…

  13. Muscle tension dysphonia and spasmodic dysphonia: the role of manual laryngeal tension reduction in diagnosis and management.

    PubMed

    Roy, N; Ford, C N; Bless, D M

    1996-11-01

    Excessive activity of the extralaryngeal muscles affects laryngeal function and contributes to a spectrum of interrelated symptoms and syndromes including muscle tension dysphonia and spasmodic dysphonia. Recognition of the role of extralaryngeal tension is helpful in ensuring proper diagnosis and selection of appropriate treatment. This report demonstrates the application of manual laryngeal musculoskeletal tension reduction techniques in the diagnosis and management of laryngeal hyperfunction syndromes. The manual technique consists of focal palpation to determine 1) extent of laryngeal elevation, 2) focal tenderness, 3) voice effect of applying downward pressure over the superior border of the thyroid lamina, and 4) extent of sustained voice improvement following circum-laryngeal massage. The clinical utility of this innovative approach is discussed. PMID:8916858

  14. Anatomic considerations in botulinum toxin type A therapy for spasmodic dysphonia.

    PubMed

    Castellanos, P F; Gates, G A; Esselman, G; Song, F; Vannier, M W; Kuo, M

    1994-06-01

    Chemodenervation by injection of botulinum toxin type A into the vocal fold(s) has become the preferred treatment for patients with adductor spasmodic dysphonia. Injection may be done either perorally or transcutaneously; each method has its advocates and advantages. The authors have used the transcutaneous transcricothyroid membrane route exclusively with satisfactory results in more than 50 patients. Temporary breathliness and aspiration are common. The preferred injection site should be as close as possible to the motor end plates of the affected muscle. The thyroarytenoid muscle end plates are distributed throughout the muscle, whereas in the lateral cricoarytenoid muscle they are located in band in the center of the muscle. The transcutaneous injection site is below and posterior to the midpoint of the vibrating vocal fold as visualized by indirect laryngoscopy. The proximity of this site to the lateral cricoarytenoid muscle suggests that postinjection breathiness and aspiration may be related to spread of botulinum toxin type A to the lateral cricoarytenoid muscle. However, it is likely that thyroarytenoid muscle paresis is mainly responsible for this side effect and that the rapid clearing of the breathy dysphonia in the face of prolonged relief of spasmodic dysphonia symptoms suggests the action of an adaptive neural response, such as axonal sprouting. Further research of this subject is warranted. PMID:8196438

  15. Spasmodic dysphonia in an adolescent patient with an autoimmune neurologic disorder.

    PubMed

    Boseley, Mark E; Gherson, Shirley; Hartnick, Christopher J

    2007-01-01

    Pediatric autoimmune neuropsychiatric disorder associated with streptococcal infections (PANDAS) has been primarily described in the neurology and psychiatry literature. The symptoms of this syndrome typically are a range of obsessive compulsive disorders and neuromuscular tics. The otolaryngologist occasionally becomes involved with these children when it is deemed that chronic tonsil infections are the source. We report here on a child diagnosed with PANDAS who presented with severe ventricular hyperfunction and adductor spasmodic dysphonia. She was treated with botulinum toxin, which resulted in a significant improvement in subjective voice as well as reduced jitter and shimmer on objective voice measurements. PMID:17362824

  16. The use of botulinum toxin in the treatment of adductor spasmodic dysphonia.

    PubMed Central

    Whurr, R; Lorch, M; Fontana, H; Brookes, G; Lees, A; Marsden, C D

    1993-01-01

    Botulinum toxin injections have been used to treat 31 patients with adductor spasmodic dysphonia. Injections of 3.00-3.75 units of botulinum toxin were performed bilaterally into the thyroarytenoid muscle. This treatment significantly decreased the standard deviation of the fundamental frequency of the speech sample, indicating a reduction in the variability of pitch amongst patients. A total of 96% of patients' subjective diary reports showed an improvement with a median of 7 days to peak effect and a 5 week duration of peak effect. Images PMID:8505645

  17. Vocal aging and adductor spasmodic dysphonia: Response to botulinum toxin injection

    PubMed Central

    Cannito, Michael P; Kahane, Joel C; Chorna, Lesya

    2008-01-01

    Aging of the larynx is characterized by involutional changes which alter its biomechanical and neural properties and create a biological environment that is different from younger counterparts. Illustrative anatomical examples are presented. This natural, non-disease process appears to set conditions which may influence the effectiveness of botulinum toxin injection and our expectations for its success. Adductor spasmodic dysphonia, a type of laryngeal dystonia, is typically treated using botulinum toxin injections of the vocal folds in order to suppress adductory muscle spasms which are disruptive to production of speech and voice. A few studies have suggested diminished response to treatment in older patients with adductor spasmodic dysphonia. This retrospective study provides a reanalysis of existing pre-to-post treatment data as function of age. Perceptual judgments of speech produced by 42 patients with ADSD were made by two panels of professional listeners with expertise in voice or fluency of speech. Results demonstrate a markedly reduced positive response to botulinum toxin treatment in the older patients. Perceptual findings are further elucidated by means of acoustic spectrography. Literature on vocal aging is reviewed to provide a specific set of biological mechanisms that best account for the observed interaction of botulinum toxin treatment with advancing age. PMID:18488884

  18. The Consequences of Spasmodic Dysphonia on Communication-Related Quality of Life: A Qualitative Study of the Insider's Experiences

    ERIC Educational Resources Information Center

    Baylor, C.R.; Yorkston, K.M.; Eadie, T.L.

    2005-01-01

    The purpose of this study was to explore the biopsychosocial consequences of spasmodic dysphonia (SD) as experienced by people with SD. Qualitative research methods were used to investigate the insider's perspective of living with SD. Six adults with SD participated in face-to-face phenomenological interviews. The results are summarized in a model…

  19. Spasmodic Dysphonia

    MedlinePlus

    ... or a printed list of organizations, contact: NIDCD Information Clearinghouse 1 Communication Avenue Bethesda, MD 20892-3456 Toll-free Voice: ( ... us on Contact ... Into Health ® National Institute on Deafness and Other Communication Disorders 31 Center Drive, MSC 2320, Bethesda, MD ...

  20. Chiropractic Care for a Patient with Spasmodic Dysphonia Associated with Cervical Spine Trauma

    PubMed Central

    Waddell, Roger K.

    2005-01-01

    Abstract Objective To discuss the diagnosis and response to treatment of spasmodic dysphonia in a 25-year-old female vocalist following an auto accident. Clinical Features The voice disorder and neck pain appeared after the traumatic incident. Examination of the cervical spine revealed moderate pain, muscle spasm and restricted joint motion at C-1 and C-5 on the left side. Cervical range of motion was reduced on left rotation. Bilateral manual muscle testing of the trapezius and sternocleidomastoid muscles, which share innervation with the laryngeal muscles by way of the spinal accessory nerve, were weak on the left side. Pre and post accident voice range profiles (phonetograms) that measure singing voice quality were examined. The pre- and post-accident phonetograms revealed significant reduction in voice intensity and fundamental frequency as measured in decibels and hertz. Intervention and Outcome Low-force chiropractic spinal manipulative therapy to C-1 and C-5 was employed. Following a course of care, the patient's singing voice returned to normal, as well as a resolution of her musculo- skeletal complaints. Conclusion It appears that in certain cases, the singing voice can be adversely affected if neck or head trauma is severe enough. This case proposes that trauma with irritation to the cervical spine nerve roots as they communicate with the spinal accessory, and in turn the laryngeal nerves, may be contributory in some functional voice disorders or muscle tension dysphonia. PMID:19674642

  1. Spasmodic dysphonia follow-up with videolaryngoscopy and voice spectrography during treatment with botulinum toxin.

    PubMed

    Esposito, Marcello; Dubbioso, R; Apisa, P; Allocca, R; Santoro, L; Cesari, U

    2015-09-01

    Spasmodic dysphonia (SD) is a focal dystonia of laryngeal muscles seriously impairing quality of voice. Adductor SD (ADSD) is the most common presentation of this disorder that can be identified by specialized phoniatricians and neurologists firstly on a clinical evaluation and then confirmed by videolaryngoscopy (VL). Botulinum toxin (BTX) injection with electromyographic guidance in muscles around vocal cords is the most effective treatment. Voice Handicap Index (VHI) questionnaire is the main tool to assess dysphonia and response to treatment. Objective of this study is to perform VL and voice spectrography (VS) to confirm the efficacy of BTX injections over time. 13 patients with ADSD were studied with VHI, VL and VS before and after 4 consecutive treatment with onobotulinumtoxin-A. For each treatment vocal improvement was proved by a significant reduction of VHI score and increase of maximum time phonation and harmonic-to-noise ratio while VL showed the absence of spasm in most of patients. No change of the response to BTX was found between injections. This study supports the efficacy of the treatment of SD with BTX with objective measurements and suggests that the efficacy of recurring treatments is stable over time. PMID:25966878

  2. Partial thyroarytenoid myectomy: an animal study investigating a proposed new treatment for adductor spasmodic dysphonia.

    PubMed

    Genack, S H; Woo, P; Colton, R H; Goyette, D

    1993-03-01

    A new surgical procedure with potential application for the treatment of adductor spasmodic dysphonia was performed on ten rabbits to assess surgical effects on laryngeal function. Using an external approach, partial unilateral thyroarytenoid (TA) muscle excision was performed through a thyroplasty cartilage window. The contralateral side was left undisturbed as a control. The animals were studied acutely and at 3 months using videolaryngoscopy. Electrophysiologic measurements were recorded at 3 months. The procedure was well tolerated by all animals, with no postoperative infection or aspiration. At 3 months, spontaneous and evoked (recurrent laryngeal nerve stimulation) TA muscle electromyographic potentials were measurable bilaterally. TA compound muscle action potential amplitudes were reduced on the side of myectomy. The threshold of recurrent laryngeal nerve stimulation needed to produce observable vocal fold adduction was increased on the side operated on. Perioperative and long-term (3 months) videolaryngoscopy demonstrated preservation of laryngeal competence with good true vocal cord adduction. Histologic analysis with whole organ sections showed replacement of excised muscle with loose fibroareolar tissue. No evidence of muscle regeneration was observed. The vocal ligament and vocal fold mucosa were intact and undistorted in all specimens. This procedure is technically simple and appears to effectively result in a functional yet weakened TA muscle. Because myectomy includes motor unit end-plate excision, problems associated with reinnervation may be circumvented. TA myectomy may be applicable in patients with focal laryngeal dystonia to decrease muscle spasm. PMID:8464639

  3. Focal white matter changes in spasmodic dysphonia: a combined DTI and neuropathological study

    PubMed Central

    Simonyan, Kristina; Tovar-Moll, Fernanda; Ostuni, John; Hallett, Mark; Kalasinsky, Victor F.; Lewin-Smith, Michael R.; Rushing, Elisabeth J.; Vortmeyer, Alexander O.; Ludlow, Christy L.

    2008-01-01

    Spasmodic dysphonia (SD) is a neurological disorder characterized by involuntary spasms in the laryngeal muscles during speech production. Although clinical symptoms of SD are well characterized, the pathophysiology of this voice disorder is unknown. We describe here, for the first time to our knowledge, disorder-specific brain abnormalities in SD patients as determined by a combined approach of diffusion tensor imaging (DTI) and postmortem histopathology. We used DTI to identify brain changes in SD and to target those brain regions for neuropathological examination. DTI showed rightsided decrease of fractional anisotropy in the genu of the internal capsule and bilateral increase of overall water diffusivity in the white matter along the corticobulbar/corticospinal tract in 20 SD patients compared to 20 healthy subjects. In addition, water diffusivity was bilaterally increased in the lentiform nucleus, ventral thalamus, and cerebellar white and gray matter in SD patients. These brain changes were substantiated with focal histopathological abnormalities presented as a loss of axonal density and myelin content in the right genu of the internal capsule and clusters of mineral depositions containing calcium, phosphorus and iron in the parenchyma and vessel walls of the posterior limb of the internal capsule, putamen, globus pallidus, and cerebellum in the postmortem brain tissue from one SD patient compared to three controls. The specificity of these brain abnormalities is confirmed by their localization limited only to the corticobulbar/corticospinal tract and its main input/output structures. We also found positive correlation between the diffusivity changes and clinical symptoms of SD (r = 0.509, p = 0.037). These brain abnormalities may alter the central control of voluntary voice production and, therefore, may underlie the pathophysiology of SD. PMID:18083751

  4. The Psychosocial Consequences of BOTOX Injections for Spasmodic Dysphonia: A Qualitative Study of Patients’ Experiences

    PubMed Central

    Baylor, Carolyn R.; Yorkston, Kathryn M.; Eadie, Tanya L.; Maronian, Nicole C.

    2009-01-01

    Summary Objectives/Hypothesis The purpose of this study is to examine the psychosocial consequences of BOTOX® (Allergan, Inc. Irvine, CA) treatment for spasmodic dysphonia (SD). This article also explores how patients judge the success of treatment and make decisions about future treatment based on psychosocial issues relevant to them. Study Design This study follows the phenomenological tradition of qualitative inquiry in which the objective is to explore the lived experiences of a group of persons who share a common phenomenon, in this case receiving BOTOX injections for SD. Methods Six adults with SD who had been receiving BOTOX injections on a long-term basis participated in face-to-face interviews. The interviews were recorded, transcribed, and analyzed according to phenomenological guidelines to identify consistent themes as well as differences among participants’ experiences. Results The results are summarized in three primary themes that suggest (1) participants’ experiences vary over time based on changes in factors such as lifestyle and personal priorities; (2) BOTOX has multidimensional psychosocial implications in physical, personal, and social domains; and (3) participants individualize their treatment regimens, taking into consideration the burden of treatment, scheduling priorities, and other strategies to maximize the benefits of BOTOX. Conclusions Based on this study, suggestions are provided for future research into a psychosocial outcome measurement, including longitudinal evaluations that accommodate changing patient priorities over time; multidimensional evaluations that incorporate physical, personal, and social issues; evaluations that include a measure of the burden of treatment; and evaluations that support a shared decision-making model with the voice clinicians. PMID:16564675

  5. Abnormal motor cortex excitability during linguistic tasks in adductor-type spasmodic dysphonia.

    PubMed

    Suppa, A; Marsili, L; Giovannelli, F; Di Stasio, F; Rocchi, L; Upadhyay, N; Ruoppolo, G; Cincotta, M; Berardelli, A

    2015-08-01

    In healthy subjects (HS), transcranial magnetic stimulation (TMS) applied during 'linguistic' tasks discloses excitability changes in the dominant hemisphere primary motor cortex (M1). We investigated 'linguistic' task-related cortical excitability modulation in patients with adductor-type spasmodic dysphonia (ASD), a speech-related focal dystonia. We studied 10 ASD patients and 10 HS. Speech examination included voice cepstral analysis. We investigated the dominant/non-dominant M1 excitability at baseline, during 'linguistic' (reading aloud/silent reading/producing simple phonation) and 'non-linguistic' tasks (looking at non-letter strings/producing oral movements). Motor evoked potentials (MEPs) were recorded from the contralateral hand muscles. We measured the cortical silent period (CSP) length and tested MEPs in HS and patients performing the 'linguistic' tasks with different voice intensities. We also examined MEPs in HS and ASD during hand-related 'action-verb' observation. Patients were studied under and not-under botulinum neurotoxin-type A (BoNT-A). In HS, TMS over the dominant M1 elicited larger MEPs during 'reading aloud' than during the other 'linguistic'/'non-linguistic' tasks. Conversely, in ASD, TMS over the dominant M1 elicited increased-amplitude MEPs during 'reading aloud' and 'syllabic phonation' tasks. CSP length was shorter in ASD than in HS and remained unchanged in both groups performing 'linguistic'/'non-linguistic' tasks. In HS and ASD, 'linguistic' task-related excitability changes were present regardless of the different voice intensities. During hand-related 'action-verb' observation, MEPs decreased in HS, whereas in ASD they increased. In ASD, BoNT-A improved speech, as demonstrated by cepstral analysis and restored the TMS abnormalities. ASD reflects dominant hemisphere excitability changes related to 'linguistic' tasks; BoNT-A returns these excitability changes to normal. PMID:26061279

  6. Alterations in CNS Activity Induced by Botulinum Toxin Treatment in Spasmodic Dysphonia: An H[subscript 2][superscript 15]O PET Study

    ERIC Educational Resources Information Center

    Ali, S. Omar; Thomassen, Michael; Schulz, Geralyn M.; Hosey, Lara A.; Varga, Mary; Ludlow, Christy L.; Braun, Allen R.

    2006-01-01

    Speech-related changes in regional cerebral blood flow (rCBF) were measured using H[subscript 2][superscript 15]O positron-emission tomography in 9 adults with adductor spasmodic dysphonia (ADSD) before and after botulinum toxin (BTX) injection and 10 age- and gender-matched volunteers without neurological disorders. Scans were acquired at rest…

  7. The consequences of spasmodic dysphonia on communication-related quality of life: A qualitative study of the insider's experiences

    PubMed Central

    Baylor, Carolyn R.; Yorkston, Kathryn M.; Eadie, Tanya L.

    2009-01-01

    The purpose of this study was to explore the biopsychosocial consequences of spasmodic dysphonia (SD) as experienced by people with SD. Qualitative research methods were used to investigate the insider's perspective of living with SD. Six adults with SD participated in face-to-face phenomenological interviews. The results are summarized in a model of personal experiences of SD which shows that communication-related quality of life (QOL) is shaped by experiences with multiple physiologic (voice quality, effort, voice dependability); personal (affective responses, changes in self-view, coping strategies) and social (physical environment, other people, participation in social roles) factors. Communication-related QOL is a complex and individualized construct with multidimensional contributors. This study suggests that understanding the nature of communication-related QOL for each individual requires exploration of each component of the model, exploration of the unique relationships among components for each person, and recognition of the multidimensional factors that shape the experience of SD. Learning outcomes As a result of this activity the reader will be able to (1) identify general features of the phenomenological research method; (2) identify the three general categories of psychosocial consequences of SD; (3) identify those psychosocial consequences of SD that are under-represented in the literature; and (4) identify key conclusions of the communication-related quality of life model. PMID:15963338

  8. Spasmodic Torticollis: Treatment Options

    MedlinePlus

    ... Join NSTA Today! NSTA Support Groups NSTA Message Forum Spasmodic Torticollis What is Spasmodic Torticollis Signs and ... Patient Support Photo Galleries Contact NSTA NSTA Message Forum Search Internet and Help NSTA Support the NSTA ...

  9. National Spasmodic Torticollis Association

    MedlinePlus

    ... alone anymore. Welcome to National Spasmodic Torticollis Association web site The mission of the National Spasmodic Torticollis ... Signs and Symptoms Treatment Options Medications Botulinum Toxin Deep Brain Stimulation (DBS) Selective Denervation Surgery Physical Therapy ...

  10. Remission in spasmodic torticollis.

    PubMed Central

    Jayne, D; Lees, A J; Stern, G M

    1984-01-01

    In 26 patients with spasmodic torticollis followed up for a median period of 12 years, the frequency of sustained remission was 23%, the median duration of remission was 8 years and duration of torticollis before remission 3 years. These results are more favourable than stated in the literature and should be taken into consideration before recommending surgical treatment. PMID:6502180

  11. Spasmodic torticollis: the dental connection.

    PubMed

    Sims, Anthony B; Stack, Brendan C; Demerjian, G Gary

    2012-07-01

    Spasmodic torticollis or cervical dystonia (CD) is the most common form of focal dystonia and is characterized by sustained abnormal muscle contractions in the head and neck area resulting in abnormal positioning or posturing of the head. The dystonic muscle spasms associated with spasmodic torticollis may affect any combination of neck muscles. Three cases are reported of spasmodic torticollis that were treated by a dental appliance with individual varying occlusal heights to open the maxillomandibular vertical dimension. Upon increasing the vertical dimension of occlusion, there was a slowing and/or discontinuance of the symptoms of cervical dystonia. The proposed hypothesis for this reversal is that there may be neuritis of the auriculotemporal branch of the trigeminal nerve, which has direct input into the reticular formation (RF), and it may activate the cells of the pontine region of the RF known for the control and deviation of head posture. There is growing clinical evidence that temporomandibular joint (TMJ) dysfunction may be a factor in this neurological and painful disorder when it coexists. PMID:22916671

  12. Dysphonia risk screening protocol

    PubMed Central

    Nemr, Katia; Simões-Zenari, Marcia; da Trindade Duarte, João Marcos; Lobrigate, Karen Elena; Bagatini, Flavia Alves

    2016-01-01

    OBJECTIVE: To propose and test the applicability of a dysphonia risk screening protocol with score calculation in individuals with and without dysphonia. METHOD: This descriptive cross-sectional study included 365 individuals (41 children, 142 adult women, 91 adult men and 91 seniors) divided into a dysphonic group and a non-dysphonic group. The protocol consisted of 18 questions and a score was calculated using a 10-cm visual analog scale. The measured value on the visual analog scale was added to the overall score, along with other partial scores. Speech samples allowed for analysis/assessment of the overall degree of vocal deviation and initial definition of the respective groups and after six months, the separation of the groups was confirmed using an acoustic analysis. RESULTS: The mean total scores were different between the groups in all samples. Values ranged between 37.0 and 57.85 in the dysphonic group and between 12.95 and 19.28 in the non-dysphonic group, with overall means of 46.09 and 15.55, respectively. High sensitivity and specificity were demonstrated when discriminating between the groups with the following cut-off points: 22.50 (children), 29.25 (adult women), 22.75 (adult men), and 27.10 (seniors). CONCLUSION: The protocol demonstrated high sensitivity and specificity in differentiating groups of individuals with and without dysphonia in different sample groups and is thus an effective instrument for use in voice clinics. PMID:27074171

  13. Spasmodic torticollis: a behavioral perspective

    SciTech Connect

    Martin, P.R.

    1982-06-01

    The literature on spasmodic torticollis is critically reviewed. The currently most popular etiological hypothesis characterizes torticollis as an extrapyramidal disorder, the symptoms of which are aggravated by stress, but there is no unequivocal evidence available to support this view. Psychological mechanisms have been suggested but not elaborated or tested in any detail. A wide range of treatments has been advocated but controlled studies have not been reported, and the problems of assessing outcome have never been tackled adequately. Behavioral treatments have been evaluated more rigorously than other approaches (particularly EMG feedback training), and the literature suggests that they benefit some patients. It is argued that psychologists have the potential for making a very significant contribution to the understanding and management of torticollis. In discussing outcome measures, the more promising techniques that have been used are summarized and a list is presented of the factors which must be considered when assessing torticollis symptoms. Directions for future research are outlined and priorities suggested.

  14. Current Endoscopic Treatment of Dysphonia

    PubMed Central

    Ossoff, Robert H.

    2000-01-01

    Benign laryngeal disorders result in dysphonia because of effects on glottic closure and the vibratory characteristics of the true vocal fold. Treatment is initially directed at reversing medical conditions and patterns of abuse with surgery reserved for unresolving lesions resulting in troublesome dysphonia. Benign lesions that require surgery are excised as precisely as possible sparing overlying mucosa and the underlying vocal ligament. Vocal fold scarring is currently best treated by augmentation procedures, and atrophy may be compensated for by medialization thyroplasty or by adding bulk to the affected folds. Application of current knowledge of laryngeal histology and physiology is prerequisite to endoscopic surgical intervention. PMID:18493531

  15. Posterior cricoarytenoid myoplasty with medialization thyroplasty in the management of refractory abductor spasmodic dysphonia.

    PubMed

    Shaw, Gary Y; Sechtem, Phillip R; Rideout, Benji

    2003-04-01

    Of the approximately 100,000 Americans with primary (idiopathic) laryngeal dystonia, 10% to 15% are thought to havethe abductor form. Botulinum A toxin injected into the posterior cricoarytenoid muscle and/or cricothyroid muscle has been employed as the "gold standard" for therapeutic management; however, successful results are significantly less frequent than with injections for the adductor form. This report describes a new phonosurgical procedure, posterior cricoarytenoid myoplasty with medialization thyroplasty, designed for these refractory patients. Posterior cricoarytenoid myoplasty with medialization thyroplasty has been performed on 3 patients with abductor laryngeal dystonia. All patients had failed at least 5 previous botulinum A injections to the posterior cricoarytenoid and cricothyroid muscles. All patients underwent preoperative and 3 postoperative (2 weeks, 3 months, and 1 year) phonatory analyses. Analysis consisted of recording an aloud reading of a standard passage while a blinded trained speech pathologist counted prolonged voiceless consonants. The patients also completed a satisfaction survey at 1 year. The results demonstrated significant, long-lasting, uniform reduction in breathy breaks in all subjects. The participants all judged their symptoms as greatly improved. Bilateral procedures may be necessary, but should be staged to prevent possible airway compromise. When applied appropriately, posterior cricoarytenoid myoplasty with medialization thyroplasty is a viable tool in the management of refractory abductor laryngeal dystonia. PMID:12731624

  16. Developing the Communicative Participation Item Bank: Rasch Analysis Results from a Spasmodic Dysphonia Sample

    ERIC Educational Resources Information Center

    Baylor, Carolyn R.; Yorkston, Kathryn M.; Eadie, Tanya L.; Miller, Robert M.; Amtmann, Dagmar

    2009-01-01

    Purpose: The purpose of this study was to conduct the initial psychometric analyses of the Communicative Participation Item Bank--a new self-report instrument designed to measure the extent to which communication disorders interfere with communicative participation. This item bank is intended for community-dwelling adults across a range of…

  17. Prominence Dynamics

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly; Kucera, Terry; Kawashima, Rei; DeVore, C.; Karpen, Judy; Antiochos, Spiro

    2011-01-01

    Fine structure prominence dynamics are visible in the majority of high-spatial resolution data from Solar Dynamics Observatory (SDO) and Hinode Solar Optical Telescope (SOT). We present the results of a study investigating the nature of these horizontal and vertical flows and discuss them in the context of ion-neutral coupling in a partially ionized prominence plasma. We also discuss how models can help in the interpretation of these observations.

  18. Is perceived dysphonia related to perceived healthiness?

    PubMed

    Maryn, Youri; Debo, Kim

    2015-10-01

    Literature has shown that voice-disordered persons are at higher risk for negative attitudes on several personality and physical appearance traits than vocally normal persons. This study investigated general perceptions of health in subjects with various degrees of dysphonia. Recordings from 100 normophonic and dysphonic subjects were auditorily rated on dysphonia severity by five experienced clinicians and on degree of healthiness/unhealthiness by seven unexperienced listeners. Results revealed strong correlation between auditory ratings of dysphonia severity and unhealthiness severity. Dysphonic subjects are rated significantly unhealthier than normophonic subjects, and the receiver-operating characteristics curve showed that even slight dysphonia induces negative attributions of unhealthiness. This study provides additional evidence for the negative attitudes with which dysphonic speakers are confronted, especially in terms of health. PMID:24850269

  19. Vocal dose in teachers: correlation with dysphonia.

    PubMed

    Gama, Ana Cristina Côrtes; Santos, Juliana Nunes; Pedra, Elisângela de Fátima Pereira; Rabelo, Alessandra Terra Vasconcelos; Magalhães, Max de Castro; Casas, Estevam Barbosa de Las

    2016-04-01

    Teachers are professionals with high prevalence of dysphonia, whose main risk factors are the large work hours in classrooms with the presence of background noise. The purpose of the study was to calculate the phonation time and the cycle dose of teachers with dysphonia and teachers without voice disorders during the class. There were two groups analyzed: five teachers with functional dysphonia were the first group and five teachers without voice disorders were the second group. For the data was used the VoxLog® dosimeter and the parameters were: intensity; fundamental frequency; phonation time and cycle dose. The statistical analysis used ANOVA, Student's T-test, and Kruskal-Wallis test. Dysphonic teachers showed major values of phonation time and cycle dose compared with teachers without voice disorders. The dysphonia is related to extended period of speech time and greater exposure of the tissue of the vocal fold to phonotrauma. PMID:27191884

  20. Management of Dysphonia After Radiation Therapy.

    PubMed

    Villari, Craig R; Courey, Mark S

    2015-08-01

    Radiation-induced dysphonia can develop after radiation for primary laryngeal cancer or when the larynx is in the radiation field for nonlaryngeal malignancy. The effects are dose dependent and lead to variable degrees of dysphonia in both short- and long-term follow-up. Rehabilitation of the irradiated larynx can prove frustrating but can be facilitated through behavioral, pharmacologic, or surgical interventions. PMID:26092762

  1. Factors Associated with Dysphonia in High School Cheerleaders.

    ERIC Educational Resources Information Center

    Campbell, Shari L.; And Others

    1988-01-01

    Questionnaire responses from 146 high school cheerleaders indicated that acute, cheering-related dysphonia may be preceded or accompanied by a set of clinical signs that could be incorporated easily into a screening protocol for prospective cheerleaders. (Author/DB)

  2. Coronal and Prominence Plasmas

    NASA Technical Reports Server (NTRS)

    Poland, Arthur I. (Editor)

    1986-01-01

    Various aspects of solar prominences and the solar corona are discussed. The formation of prominences, prominence diagnostics and structure, prominence dissappearance, large scale coronal structure, coronal diagnostics, small scale coronal structure, and non-equilibrium/coronal heating are among the topics covered.

  3. Quantitative evaluation of phonetograms in the case of functional dysphonia.

    PubMed

    Airainer, R; Klingholz, F

    1993-06-01

    According to the laryngeal clinical findings, figures making up a scale were assigned to vocally trained and vocally untrained persons suffering from different types of functional dysphonia. The different types of dysphonia--from the manifested hypofunctional to the extreme hyperfunctional dysphonia--were classified by means of this scale. Besides, the subjects' phonetograms were measured and approximated by three ellipses, what rendered possible the definition of phonetogram parameters. The combining of selected phonetogram parameters to linear combinations served the purpose of a phonetographic evaluation. The linear combinations were to bring phonetographic and clinical evaluations into correspondence as accurately as possible. It was necessary to use different kinds of linear combinations for male and female singers and nonsingers. As a result of the reclassification of 71 and the new classification of 89 patients, it was possible to graduate the types of functional dysphonia by means of computer-aided phonetogram evaluation with a clinically acceptable error rate. This method proved to be an important supplement to the conventional diagnostics of functional dysphonia. PMID:8353627

  4. Muscle tension dysphonia in Vietnamese female teachers.

    PubMed

    Nguyen, Duong Duy; Kenny, Dianna T; Tran, Ninh Duy; Livesey, Jonathan R

    2009-03-01

    There has been no published research on muscle tension dysphonia (MTD) in speakers who use a tonal language. Using a sample of 47 Northern Vietnamese female primary school teachers with MTD, we aimed to discover whether professional voice users of tonal languages presented with the same symptoms of MTD as speakers of nontonal languages and whether they presented with additional symptoms as a result of speaking a tonal language. The vocal characteristics were assessed by use of a questionnaire and expert perceptual evaluation. Laryngeal features were assessed by photolaryngoscopy. The results showed that MTD was associated with a larger number of vocal symptoms than previously reported. However, the participants did not have the same vocal symptoms reported in English speakers, for example, hard glottal attack, pitch breaks, unusual speech rate, and glottal fry. Factor analysis of the vocal symptoms revealed three factors: "vocal fatigue/hyperfunction," "physical discomfort," and "voice quality," all of which demonstrated high reliability. The major laryngeal characteristic was a glottal gap. The glottal shapes observed included: 44.7% had an incomplete closure, 29.8% a posterior gap, 12.8% an hourglass-shaped gap, 8.5% a spindle-shaped gap, and 4.3% had complete glottal closure. The findings implied a potential contribution of linguistic-specific factors and teaching-related factors to the presentation of this voice disorder in this group of teachers. PMID:18207359

  5. Functional dysphonia: strategies to improve patient outcomes.

    PubMed

    Behlau, Mara; Madazio, Glaucya; Oliveira, Gisele

    2015-01-01

    Functional dysphonia (FD) refers to a voice problem in the absence of a physical condition. It is a multifaceted voice disorder. There is no consensus with regard to its definition and inclusion criteria for diagnosis. FD has many predisposing and precipitating factors, which may include genetic susceptibility, psychological traits, and the vocal behavior itself. The assessment of voice disorders should be multidimensional. In addition to the clinical examination, auditory-perceptual, acoustic, and self-assessment analyses are very important. Self-assessment was introduced in the field of voice 25 years ago and has produced a major impact in the clinical and scientific scenario. The choice of treatment for FD is vocal rehabilitation by means of direct therapy; however, compliance has been an issue, except for cases of functional aphonia or when an intensive training is administered. Nevertheless, there are currently no controlled studies that have explored the different options of treatment regimens for these patients. Strategies to improve patient outcome involve proper multidisciplinary diagnosis in order to exclude neurological and psychiatric disorders, careful voice documentation with quantitative measurement and qualitative description of the vocal deviation for comparison after treatment, acoustic evaluation to gather data on the mechanism involved in voice production, self-assessment questionnaires to map the impact of the voice problem on the basis of the patient's perspective, referral to psychological evaluation in cases of suspected clinical anxiety and/or depression, identification of dysfunctional coping strategies, self-regulation data to assist patients with their vocal load, and direct and intensive vocal rehabilitation to reduce psychological resistance and to reassure patient's recovery. An international multicentric effort, involving a large population of voice-disordered patients with no physical pathology, could produce enough data for

  6. Functional dysphonia: strategies to improve patient outcomes

    PubMed Central

    Behlau, Mara; Madazio, Glaucya; Oliveira, Gisele

    2015-01-01

    Functional dysphonia (FD) refers to a voice problem in the absence of a physical condition. It is a multifaceted voice disorder. There is no consensus with regard to its definition and inclusion criteria for diagnosis. FD has many predisposing and precipitating factors, which may include genetic susceptibility, psychological traits, and the vocal behavior itself. The assessment of voice disorders should be multidimensional. In addition to the clinical examination, auditory-perceptual, acoustic, and self-assessment analyses are very important. Self-assessment was introduced in the field of voice 25 years ago and has produced a major impact in the clinical and scientific scenario. The choice of treatment for FD is vocal rehabilitation by means of direct therapy; however, compliance has been an issue, except for cases of functional aphonia or when an intensive training is administered. Nevertheless, there are currently no controlled studies that have explored the different options of treatment regimens for these patients. Strategies to improve patient outcome involve proper multidisciplinary diagnosis in order to exclude neurological and psychiatric disorders, careful voice documentation with quantitative measurement and qualitative description of the vocal deviation for comparison after treatment, acoustic evaluation to gather data on the mechanism involved in voice production, self-assessment questionnaires to map the impact of the voice problem on the basis of the patient’s perspective, referral to psychological evaluation in cases of suspected clinical anxiety and/or depression, identification of dysfunctional coping strategies, self-regulation data to assist patients with their vocal load, and direct and intensive vocal rehabilitation to reduce psychological resistance and to reassure patient’s recovery. An international multicentric effort, involving a large population of voice-disordered patients with no physical pathology, could produce enough data for

  7. Dynamics of quiescent prominences

    NASA Astrophysics Data System (ADS)

    Heinzel, Petr

    2012-07-01

    We review the state-of-the-art of the observations and modeling of prominence fine structures, with special emphasis on the dynamics. Fine structures of quiescent prominences have been recently observed by Hinode/SOT and these observations revealed a rather complex dynamics of bright threads and blobs and of dark plumes originating from large prominence bubbles. SOHO/SUMER spectra of hydrogen Lyman lines, together with H-alpha observations from MSDP, provide us with constraints on the dynamics of cool fine structures. 2D non-LTE modeling is used for analysis of the line profiles and their asymmetries. On the contrary, the SDO/AIA images, together with RHD modeling of dipped magnetic loops, lead to a better understanding of the dynamics and energetics of hotter prominence plasmas. Finally, some more global dynamics is revealed by the spectroscopic detection of quiescent prominence oscillations. We show recent results of such observations and new radiative-transfer modeling.

  8. Aerodynamic Profiles of Women with Muscle Tension Dysphonia/Aphonia

    ERIC Educational Resources Information Center

    Gillespie, Amanda I.; Gartner-Schmidt, Jackie; Rubinstein, Elaine N.; Abbott, Katherine Verdolini

    2013-01-01

    Purpose: In this study, the authors aimed to (a) determine whether phonatory airflows and estimated subglottal pressures (est-P[subscript sub]) for women with primary muscle tension dysphonia/aphonia (MTD/A) differ from those for healthy speakers; (b) identify different aerodynamic profile patterns within the MTD/A subject group; and (c) determine…

  9. Comprehensive Management of Psychogenic Dysphonia: A Case Illustration

    ERIC Educational Resources Information Center

    Sudhir, Paulomi M.; Chandra, Prabha S.; Shivashankar, N.; Yamini, B. K.

    2009-01-01

    Psychogenic dysphonia refers to the loss of voice, in the absence of apparent structural or neurological pathology. It is a disorder seen more often in women and is usually associated with significant life events and emotional difficulties that may lead to conflict over speaking. Therapeutic interventions in voice disorders recommend the adoption…

  10. Exploring Genetic and Environmental Effects in Dysphonia: A Twin Study

    ERIC Educational Resources Information Center

    Simberg, Susanna; Santtila, Pekka; Soveri, Anna; Varjonen, Markus; Sala, Eeva; Sandnabba, N. Kenneth

    2009-01-01

    Purpose: To explore the existence of genetic effects as well as the interaction between potential genetic effects and a voice-demanding occupation on dysphonia. Method: One thousand seven hundred and twenty-eight Finnish twins (555 male; 1,173 female) born between 1961 and 1989 completed a questionnaire concerning vocal symptoms and occupation.…

  11. Dysphonia Detected by Pattern Recognition of Spectral Composition.

    ERIC Educational Resources Information Center

    Leinonen, Lea; And Others

    1992-01-01

    This study analyzed production of a long vowel sound within Finnish words by normal or dysphonic voices, using the Self-Organizing Map, the artificial neural network algorithm of T. Kohonen which produces two-dimensional representations of speech. The method was found to be both sensitive and specific in the detection of dysphonia. (Author/JDD)

  12. Psychosocial Aspects of Adolescent Dysphonia: An Approach to Treatment.

    ERIC Educational Resources Information Center

    Beery, Quinter C.

    1991-01-01

    This paper presents an approach to voice therapy with adolescents, emphasizing the importance of psychosocial and family influences as they relate to vocal behavior. The goals of therapy for the adolescent with dysphonia usually follow an orderly sequence, first dealing with individual behavior and later with family and peer group influences. (JDD)

  13. [Incidence of dysphonia in teaching staff of schools].

    PubMed

    Bellia, S; Serafino, L; Luca, N; Farruggia, E; Bellia, M

    2007-01-01

    Some categories of workers (actors, teachers, singers) use a particular working tool: their voice. In order to assess the spread of dysphonia and its possible causes across a specific class of workers--the teachers of some schools in the city of Catania--we have set up a ad hoc questionnaire. A special database has been subsequently arranged, aimed at the statistical analysis of the responses obtained. The analysis of the responses shows that the phenomenon is more present in female than male teachers, 48% versus 30%. The dysphonia occurs mainly at the end of the working day, lasts throughout the school year and improves in summer, demonstrating the importance of teaching activity in its pathogenesis. One aspect especially stands out: dysphonia occurs exclusively in those individuals suffering from diseases with possible alterations of the voice, such as allergopathies, tireopathies and gastropathies. Therefore, work activity alone does not seem able to cause a chronic dysphonia, whereas the presence of diseases causing disability of vocal cords appears to play an important role. PMID:18409864

  14. First Light Prominence

    NASA Video Gallery

    Soon after the instruments opened their doors, the Sun began performing for SDO with this beautiful prominence eruption. This AIA data is from March 30, 2010, showing a wavelength band that is cent...

  15. Arching Solar Prominence

    NASA Video Gallery

    NASA’s STEREO (Ahead) spacecraft watched as an eruptive prominence rose up and arched out in a horseshoe shape far above the Sun’s surface (Aug. 25, 2010). The image and movie show the action in a...

  16. Prominence Formation Processes

    NASA Astrophysics Data System (ADS)

    Welsch, B. T.; DeVore, C. R.; Antiochos, S. K.

    2005-01-01

    Martens and Zwaan (ApJ v. 558 872) have proposed a prominence/ filament formation model in which differential rotation drives reconnection between two initially unconnected active regions to form helical field lines that support mass and are held down by overlying field. Using an MHD solver with adaptive refinement we simulated this process by imposing a shear flow meant to mimic differential rotation on two bipolar flux distributions meant to mimic distinct active regions. In some runs the flux systems are initially potential while in others they have been twisted by footpoint rotation to inject helicity prior to imposing the shear flow. The resulting structures are studied to understand the role of helicity in the formation of prominence-like structures.

  17. Solar Prominence Eruption

    NASA Technical Reports Server (NTRS)

    Moore, Ronald L.

    1998-01-01

    The prominence that erupts in a prominence eruption is a magnetic structure in the chromosphere and corona. It is visible in chromospheric images by virtue of chromospheric-temperature plasma suspended in the magnetic field, and belongs to that large class of magnetic structures appropriately called filaments because of their characteristic sinewy sigmoidal form. Hence, the term "filament eruption" is used interchangeably with the term "prominence eruption". The magnetic field holding a filament is prone to undergo explosive changes in configuration. In these upheavals, because the filament material is compelled by its high conductivity to ride with the magnetic field that threads it, this material is a visible tracer of the field motion. The part of the magnetic explosion displayed by the entrained filament material is the phenomenon known as a filament eruption, the topic of this article. This article begins with a description of basic observed characteristics of filament eruptions, with attention to the magnetic fields, flares, and coronal mass ejections in which erupting filaments are embedded. The present understanding of these characteristics in terms of the form and action of the magnetic field is then laid out by means of a rudimentary three-dimensional model of the field. The article ends with basic questions that this picture leaves unresolved and with remarks on the observations needed to probe these questions.

  18. The Effect of Listener Experience and Anchors on Judgments of Dysphonia

    ERIC Educational Resources Information Center

    Eadie, Tanya L.; Kapsner-Smith, Mara

    2011-01-01

    Purpose: To determine the effect of auditory anchors on judgments of overall severity (OS) and vocal effort (VE) in dysphonic speech when judgments are made by experienced and inexperienced listeners, and when self-rated by individuals with dysphonia (speaker-listeners). Method: Twenty individuals with dysphonia and 4 normal controls provided…

  19. Toward the Development of an Objective Index of Dysphonia Severity: A Four-Factor Acoustic Model

    ERIC Educational Resources Information Center

    Awan, Shaheen N.; Roy, Nelson

    2006-01-01

    During assessment and management of individuals with voice disorders, clinicians routinely attempt to describe or quantify the severity of a patient's dysphonia. This investigation used acoustic measures derived from sustained vowel samples to predict dysphonia severity (as determined by auditory-perceptual ratings), for a diverse set of voice…

  20. Prominence Structure and Dynamics

    NASA Technical Reports Server (NTRS)

    Karpen, Judy T.

    2009-01-01

    Nonerupting prominences are not dull, static objects. Rather, they are composed of fine-scale blobs and threads that are highly dynamic, often appearing to travel in opposite directions on adjacent tracks (denoted counterstreaming). Because the plasma is largely constrained to travel along the magnetic field, these cool, dense features can serve as tracers of the prominence magnetic structure, a valuable resource in view of the long-standing difficulty of observing the coronal field. Conversely, greater understanding of the fundamental magnetic geometry of filament channels can provide important constraints on the physical processes governing the accumulation, support, motion, and eruption of the cool plasma. Despite over a century of detailed observations, large gaps remain in our knowledge of filament channel/plasma formation and evolution. Resolving these issues will shed light on the physics of coronal heating, helicity transport throughout the solar cycle, and the origins of eruptive activity on the Sun. I will discuss the leading models for the magnetic and plasma structure, and outline how new observations and theory /modeling could solve long-standing uncertainties regarding this majestic solar phenomenon.

  1. Formation and support of prominence

    NASA Technical Reports Server (NTRS)

    Forbes, T. G.

    1986-01-01

    A short introduction is given to the concepts discussed by the group on the formation and support of prominences. Only quiescent and long-lived active region prominences were considered, since transient prominence phenomena, such as sprays, surges, H alpha flare-loops, and coronal rain, are dynamically distinct from long-lived, prominences. Stable prominences (which are often referred to as filaments when seen against the disk) can be subdivided into three categories, namely active region prominences, quiescent prominences and polar crown prominences. The third category is closely related to the second since a quiescent prominence will eventually evolve into a polar crown prominence if it lasts long enough. The distinction between the first and second categories is not sharp either since intermediates exist here as well (Martin, 1973).

  2. [Pressure-related dysphonia, recurring pneumonia and supraglottic tumor].

    PubMed

    Jahn, K; Straehler-Pohl, H-J; Fischer, H-P; Schade, G

    2010-09-01

    Urbach-Wiethe syndrome (hyalinosis cutis et mucosae) is an autosomal-recessive inherited disease. It often presents with typical symptoms such as skin lesions (especially in the face and neck area), dyspnea, and maldigestion. Hoarseness is a leading symptom in young children. These manifestations are caused by the assimilation of glycoproteins in mesenchymal tissue. Our case report shows that hoarseness does not necessarily appear only in children, but can also appear later. Furthermore, the assimilation of glycoproteins in the supraglottic area may also cause dysphonia. Due to the varied features of this disease, interdisciplinary check-ups are necessary at regular intervals. PMID:20464358

  3. Prominent rocks - 3D

    NASA Technical Reports Server (NTRS)

    1997-01-01

    Many prominent rocks near the Sagan Memorial Station are featured in this image, taken in stereo by the Imager for Mars Pathfinder (IMP) on Sol 3. 3D glasses are necessary to identify surface detail. Wedge is at lower left; Shark, Half-Dome, and Pumpkin are at center. Flat Top, about four inches high, is at lower right. The horizon in the distance is one to two kilometers away.

    Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is an operating division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator.

    Click below to see the left and right views individually. [figure removed for brevity, see original site] Left [figure removed for brevity, see original site] Right

  4. Solar Prominence - Sept 24, 2013

    NASA Video Gallery

    These movies show the highly dynamic motions in solar prominences. The movie on the right side shows the prominence motions of material at 65,000K. The vertical stripe in the center of the image is...

  5. Differential diagnosis problems in a patient with dysphonia and chronic lymphocytic leukemia

    PubMed Central

    Gavrila, Gabriela-Ariadna; Mihaila, Romeo-Gabriel; Manitiu, Ioan

    2015-01-01

    Dysphonia is frequently an expression of laryngitis, especially when it comes in the evolution of an immunosuppressed patient, as happens in chronic lymphoproliferation. But other causes of dysphonia should also not be forgotten, including the possibility of new malignancies, especially due to the fact that these patients have genomic instability that predisposes to appearance of a second or even a third cancer. We present the case of a patient who developed dysphonia during chronic lymphocytic leukemia evolution. Its etiology was a mediastinal compression through lymph nodes, not linked to leukemia, but produced by metastases of a bronchopulmonary cancer, appeared recently. Dysphonia condition due to vocal cord dysfunction must include diseases of the mediastinum, the neck and the brain stem. The rapid and correct diagnosis and the prompt start of an appropriate treatment are of paramount importance for clinician who manage their care and for patient survival. PMID:25878649

  6. Investigation of Solar Eruptive Prominences

    NASA Astrophysics Data System (ADS)

    Su, Yingna; McCauley, Patrick; van Ballegooijen, Adriaan; Ji, Haisheng; Reeves, Katharine; DeLuca, Edward

    2015-08-01

    At first, we will present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by SDO/AIA (end-on view) and displays a quasi vertical-thread structure. Bright U-shape (horn-like) structure is observed surrounding the upper portion of the prominence (171 Angstrom) before the eruption and becomes more prominent during the eruption. When viewed on the disk, STEREO-B shows that this long prominence is composed of a series of vertical threads and displays a half loop-like structure during the eruption. We focus on the magnetic support of the prominence by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO. We construct a series of magnetic field models (including sheared arcade model, twisted flux rope model, and model with HFT), then compare with observations. Various observational characteristics appear to support the twisted flux rope model. Our study suggests that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast rise phase, and signature of reconnection appears about one hour later. In the second part, we will present a statistical study on the kinematics of limb eruptive prominences observed by SDO/AIA. A brief introduction on an online catalog of prominence eruptions observed by SDO/AIA will also be presented.

  7. Prolonged dysphonia as a complication of interscalene block.

    PubMed

    Villar, Tania; Pacreu, Susana; Zalbidea, Maite; Montes, Antonio

    2015-07-01

    The interscalene block (ISB) of the brachial plexus is a common technique for anaesthesia and the treatment of postoperative pain in shoulder surgery. Despite the well-known advantages of this technique, it is not without risks that need to be identified and taken into account. The most frequent complications associated with it are of a neurological nature and most are transient. It has been shown that the use of nerve stimulation does not guarantee a safe block. Ultrasound guidance now makes it possible to visualise potentially dangerous structures, thus allowing us to reduce the risk of associated complications. We present the case of a patient with transient dysphonia secondary to recurrent laryngeal nerve palsy. We also discuss briefly the most common complications associated with the technique. PMID:25817166

  8. New perspectives on solar prominences

    NASA Astrophysics Data System (ADS)

    Schmieder, B.; Aulanier, G.

    2012-06-01

    Recent observations of prominences obtained with high spatial and temporal resolution instruments, on board satellites (Hinode, SDO) as well as on the ground (SST) have provided very intriguing movies and open a new area for understanding the nature of prominences. The main topics are still debate: formation, dynamics, and characteristics of the plasma in the core and in the transition zone between the prominence and corona. We will review briefly the recent advances made in these topics, observationally as well as theoretically.

  9. Description and Classification of Prominences

    NASA Astrophysics Data System (ADS)

    Engvold, Oddbjørn

    Solar prominences are bright cloud-like structures when observed beyond the solar limb and they appear as dark filamentary objects which are termed filaments when seen against the solar disk. The aims of prominence classifications were from the start to establish references and frameworks for understanding the physical conditions for their formation and development through interplay with the solar magnetic environment. The multi-thermal nature of solar prominences became fully apparent once observations from space in UV, VUV, EUV and X-rays could be made. The cool prominence plasma is thermally shielded from the much hotter corona and supported in the field of gravity by small- and large-scale magnetic fields of the filament channels. High cadence, subarcsecond observing facilities on ground and in space have firmly proven the highly dynamic nature of solar prominences down to the smallest observed structural sizes of 100 km. The origin of the ubiquitous oscillations and flowing of the plasma over a variety of spatial and temporal scales, whether the cool dense plasma originates from below via levitation, injections by reconnection or results from condensation processes, are central issues in prominence research today. The unveiling of instabilities leading to prominences eruptions and Coronal Mass Ejections is another important challenge. The objective of this chapter is to review the main characteristics of various types of prominences and their associated magnetic environments, which will all be addressed in details in the following chapters of this book.

  10. Magnetic fields in quiescent prominences

    NASA Technical Reports Server (NTRS)

    Van Ballegooijen, A. A.; Martens, P. C. H.

    1990-01-01

    The origin of the axial fields in high-latitude quiescent prominences is considered. The fact that almost all quiescent prominences obey the same hemisphere-dependent rule strongly suggests that the solar differential rotation plays an important role in producing the axial fields. However, the observations are inconsistent with the hypothesis that the axial fields are produced by differential rotation acting on an existing coronal magnetic field. Several possible explanations for this discrepancy are considered. The possibility that the sign of the axial field depends on the topology of the magnetic field in which the prominence is embedded is examined, as is the possibility that the neutral line is tilted with respect to the east-west direction, so that differential rotation causes the neutral line also to rotate with time. The possibility that the axial fields of quiescent prominences have their origin below the solar surface is also considered.

  11. Increase of glucose consumption in basal ganglia, thalamus and frontal cortex of patients with spasmodic torticollis

    SciTech Connect

    Grassi, F.; Bressi, S.; Antoni, M.

    1994-05-01

    The pathophysiology of spasmodic torticollis, a focal dystonia involving neck muscles, is still unclear. Positron emission tomography (PET) studies showed either an increase as well as a decrease of regional cerebral metabolic rate of glucose (rCMRglu) in basal ganglia. In the present study, [18F]FDG and PET was used to measure rCMRglu in 10 patients with spasmodic torticollis (mean age 50.37 {plus_minus} 11.47) and 10 age matched controls. All cases with a short disease duration, were untreated. A factorial analysis of variance revealed a significant bilateral increase of glucose consumption in caudate nucleus and pallidum/putamen complex (p>0.004) and in the cerebellum (p>0.001). The rCMRglu increase in the motor/premotor cortex and in the thalamus reached a trend towards significance (p<0.05). These preliminary data show enhanced metabolism in basal ganglia and cerebellum as the functional correlate of focal dystonia. A recently proposed model suggests that dystonia would be the consequence of a putaminal hyperactivity, leading to the breakdown of the pallidal inhibitory control on thalamus and thalamo-cortical projections.

  12. The dynamics of funnel prominences

    SciTech Connect

    Keppens, R.; Xia, C.

    2014-07-01

    We present numerical simulations in 2.5D settings where large-scale prominences form in situ out of coronal condensation in magnetic dips, in close agreement with early as well as recent reporting of funnel prominences. Our simulation uses full thermodynamic magnetohydrodynamics with anisotropic thermal conduction, optically thin radiative losses, and parameterized heating as main ingredients to establish a realistic arcade configuration from chromosphere to corona. The chromospheric evaporation, especially from transition region heights, ultimately causes thermal instability, and we witness the growth of a prominence suspended well above the transition region, continuously gaining mass and cross-sectional area. Several hours later, the condensation has grown into a structure connecting the prominence-corona transition region with the underlying transition region, and a continuous downward motion from the accumulated mass represents a drainage that matches observational findings. A more dynamic phase is found as well, with coronal rain, induced wave trains, and even a reconnection event when the core prominence plasma weighs down the field lines until a flux rope is formed. The upper part of the prominence is then trapped in a flux-rope structure, and we argue for its violent kink-unstable eruption as soon as the (ignored) length dimension would allow for ideal kink deformations.

  13. Greenhouse effect in quiescent prominences

    NASA Astrophysics Data System (ADS)

    Ryutova, M.; Berger, T. E.; Title, A. M.

    2010-12-01

    Quiescent prominences, by definition, are huge ``clouds'' of cool, dense plasma overlying rarefied hot corona and supported by a complex magnetic field anchored in the photosphere along the magnetic polarity inversion line. One of the most prominent features in their dynamics is formation, growth and collapse of bubble/cavities filled by coronal plasma and emerging, often repeatedly, under a prominence body. As such, prominence/corona interface itself is subject of fundamental plasma instabilities, which include development of a regular series of plumes and spikes typical to the Rayleigh-Taylor instability, the Kelvin-Helmholtz instability, often followed by a sudden collimated mass upflow, which, in nonlinear stage having an explosive character may be responsible for CMEs. These were only recently studied in detail with high cadence, high resolution data obtained from the Hinode satellite. Even more surprises are brought by the SDO/AIA instrument showing the Sun's atmosphere in 12 visible and EUV wavelengths. AIA multi-wavelength images in a temperature range from 105 ~K to 2 × 106 ~K combined with the Hinode/SOT data show that plasma inside the prominence cavity, being as expected, at coronal temperatures, in fact exceeds the temperature of the ambient corona. We suggest that an energetically open highly dynamic processes releasing energy at the prominence/cavity interface accompanied by the ``radiative exchange'', may cause additional increase of temperature and/or density inside cavity. Given pervasive character of prominences, future studies will allow us to perform quantitative and statistical analysis, and reveal relations between the size of cavity, its temperature, and magnetic properties.

  14. Voice disorders (dysphonia) in public school female teachers working in Belo Horizonte: prevalence and associated factors.

    PubMed

    de Medeiros, Adriane Mesquita; Barreto, Sandhi Maria; Assunção, Ada Avila

    2008-11-01

    The objective of this study is to establish the prevalence of dysphonia and associated factors in public school female teachers working in Belo Horizonte. This cross-sectional study was conducted on a random sample of schools between May 2004 and July 2005. There were 2103 elementary education daytime teachers from 83 schools included in the study. Self-applied questionnaires were used for data collection. These included questions on social and demographic matters, general health and mental health (General Health Questionnaire-12 [GHQ-12]), the environment and organization of work, and voice-related aspects. The variable dysphonia was classified as absent, possible, or probable based on the association between frequency of fatigue when speaking and worsened voice quality during the past 15 days. Multinomial logistic regression was used to analyze factors independently associated with dysphonia in each response subgroup and in total. One third of the female teachers did not report voice symptoms during the past 15 days (33%). The prevalence of probable dysphonia was 15%, and the prevalence for possible dysphonia was 52%. Factors associated with probable dysphonia were presence of recent upper airway problems (odds ratio [OR]=5.95, 95% confidence interval [CI]=4.06-8.71), problems at work because of voice (OR=65.30, 95% CI=19.33-220.59), other activities with intense voice use (OR=1.71, 95% CI=1.08-2.71), high noise levels (OR=2.55, 95% CI=1.72-3.76), poor ventilation in the classroom (OR=2.00, 95% CI=1.24-3.22), current mental disorder (OR=3.20, 95% CI=2.18-4.70), sedentary life style (OR=1.94, 95% CI=1.21-3.09), and marriage (OR=1.70, 95% CI=1.16-2.47). Associations between probable dysphonia, poor working conditions, health-related aspects, and professional jeopardy indicate the complexity of dysphonia in female teachers and the need for collective intervention strategies. PMID:17981015

  15. The perception of prominence patterns.

    PubMed

    Kohler, Klaus J

    2008-01-01

    The term 'stress' is used to refer to the perceptual salience at certain places in strings of syllables, but it has several different referents: (a) relative syllable salience in an utterance; this is syllable-, not word-oriented; (b) stress in a word; this is part of the lexical phonology; (c) stressing of words in utterances for various aspects of propositional and expressive meaning, often called 'accent(uation)'. Referents b and c are word- and meaning-oriented. In this article, the terms are more stringently defined. 'Stress' is only used to refer to a lexical stress position (referent b), i.e. a syllable in a word that becomes the docking place for various types of 'accent' to weight words in utterances (referent c). 'Stress' has no physical attributes by itself. 'Prominence' refers to the patterns of salience in syllable strings (referent a). The article reports results of an experiment in prominence perception of the logatome baba, in which the physical parameters F0, syllabic duration, and overall acoustic energy were systematically varied across the bisyllable. Sixteen German subjects had to indicate, by pressing buttons of a computerized reaction time device, whether the first or the second syllable was more prominent. F(0) was a more powerful cue than the other two. Equal syllable duration on a monotone resulted in more first-syllable judgements, which could be counteracted by a slightly falling F(0) contour on the second syllable to reach equal response frequencies for the two syllables. This ties in with Lehiste's earlier findings that F(0) movement increases the perception of duration. Extrapolating from the results, a research programme for prominence perception is developed that will eventually shed new light on the investigation into the nature and manifestation of speech rhythm. PMID:19221454

  16. Intensified Voice Therapy: A New Model for the Rehabilitation of Patients Suffering from Functional Dysphonias

    ERIC Educational Resources Information Center

    Fischer, Michael J.; Gutenbrunner, Christoph; Ptok, Martin

    2009-01-01

    The objective of this study was to evaluate a new intervention for chronic dysphonias, consisting of a 2-week outpatient treatment period using intensified voice therapy combined with elements of physical medicine, including physiotherapy (orthotherapy, detonisation and training of the trunk muscles, respiratory therapy and others), manual therapy…

  17. Articulatory Changes Following Treatment of Muscle Tension Dysphonia: Preliminary Acoustic Evidence

    ERIC Educational Resources Information Center

    Dromey, Christopher; Nissen, Shawn L.; Roy, Nelson; Merrill, Ray M.

    2008-01-01

    Purpose: Primary muscle tension dysphonia (MTD), a voice disturbance that occurs in the absence of structural or neurological pathology, may respond to manual circumlaryngeal techniques, which ostensibly alter the posture of the larynx and/or the configuration of the vocal folds without directly targeting supralaryngeal articulatory structures.…

  18. Functional Dysphonia during Mental Imagery: Testing the Trait Theory of Voice Disorders

    ERIC Educational Resources Information Center

    van Mersbergen, Miriam; Patrick, Christopher; Glaze, Leslie

    2008-01-01

    Purpose: Previous research has proposed that persons with functional dysphonia (FD) present with temperamental traits that predispose them to their voice disorder. We investigated this theory in a controlled experiment and compared them with social anxiety (SA) and healthy control (HC) groups. Method: Twelve participants with FD, 19 participants…

  19. Early Motor Unit Disease Masquerading as Psychogenic Breathy Dysphonia: A Clinical Case Presentation

    ERIC Educational Resources Information Center

    Aronson, Arnold E.

    1971-01-01

    Presented is a study of a 20-year-old girl with mild, breathy dysphonia, previously diagnosed as psychogenic. In actuality, her voice change was a sign of early myasthenia gravis. It is pointed out that voice changes can be a first and only sign of early neurologic disease. (Author/KW)

  20. Articulatory Changes in Muscle Tension Dysphonia: Evidence of Vowel Space Expansion Following Manual Circumlaryngeal Therapy

    ERIC Educational Resources Information Center

    Roy, Nelson; Nissen, Shawn L.; Dromey, Christopher; Sapir, Shimon

    2009-01-01

    In a preliminary study, we documented significant changes in formant transitions associated with successful manual circumlaryngeal treatment (MCT) of muscle tension dysphonia (MTD), suggesting improvement in speech articulation. The present study explores further the effects of MTD on vowel articulation by means of additional vowel acoustic…

  1. Featured Image: Solar Prominence Eruptions

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2016-02-01

    In these images from the Solar Dynamics Observatorys AIA instrument (click for the full resolution!), two solar prominence eruptions (one from June 2011 and one from August 2012) are shown in pre- and post-eruption states. The images at the top are taken in the Fe XII 193 bandpass and the images at the bottom are taken in the He II 304 bandpass. When a team of scientists searched through seven years of solar images taken by the STEREO (Solar Terrestrial Relations Observatory) spacecraft, these two eruptions were found to extend all the way out to a distance of 1 AU. They were the only two examples of clear, bright, and compact prominence eruptions found to do so. The scientists, led by Brian Wood (Naval Research Laboratory), used these observations to reconstruct the motion of the eruption and model how prominences expand as they travel away from the Sun. Theimage to the rightshowsa STEREO observation compared to the teams 3D model of theprominences shape and expansion. To learn more about theresults from this study, check out the paper below.CitationBrian E. Wood et al 2016 ApJ 816 67. doi:10.3847/0004-637X/816/2/67

  2. The Chromosphere and Prominence Magnetometer

    NASA Astrophysics Data System (ADS)

    de Wijn, Alfred; Bethge, Christian; McIntosh, Scott; Tomczyk, Steven; Burkepile, Joan

    2013-04-01

    The Chromosphere and Prominence Magnetometer (ChroMag) is a synoptic instrument with the goal of quantifying the intertwined dynamics and magnetism of the solar chromosphere and in prominences through imaging spectro-polarimetry of the full solar disk in a synoptic fashion. The picture of chromospheric magnetism and dynamics is rapidly developing, and a pressing need exists for breakthrough observations of chromospheric vector magnetic field measurements at the true lower boundary of the heliospheric system. ChroMag will provide measurements that will enable scientists to study and better understand the energetics of the solar atmosphere, how prominences are formed, how energy is stored in the magnetic field structure of the atmosphere and how it is released during space weather events like flares and coronal mass ejections. An essential part of the ChroMag program is a commitment to develop and provide community access to the `inversion' tools necessary to interpret the measurements and derive the magneto-hydrodynamic parameters of the plasma. Measurements of an instrument like ChroMag provide critical physical context for the Solar Dynamics Observatory (SDO) and Interface Region Imaging Spectrograph (IRIS) as well as ground-based observatories such as the future Advanced Technology Solar Telescope (ATST). A prototype is currently under construction at the High Altitude Observatory of the National Center for Atmospheric Research in Boulder, CO, USA. The heart of the ChroMag instrument is an electro-optically tunable wide-fielded narrow-band birefringent six-stage Lyot filter with a built-in polarimeter. We will present a progress update on the ChroMag design, and present results from the prototype instrument.

  3. Determining Prominent Subdomains in Medicine

    PubMed Central

    Bernhardt, Powell J.; Humphrey, Susanne M.; Rindflesch, Thomas C.

    2005-01-01

    We discuss an automated method for identifying prominent subdomains in medicine. The motivation is to enhance the results of natural language processing by focusing on sublanguages associated with medical specialties concerned with prevalent disorders. At the core of our approach is a statistical system for topical categorization of medical text. A method based on epidemiological evidence is compared to another that considers frequency of occurrence of Medline citations. We suggest the isolation of UMLS terminology peculiar to individual medical specialties as a way of enhancing natural language processing systems in the biomedical domain. PMID:16778999

  4. Cross-system effects of dysphagia treatment on dysphonia: a case report

    PubMed Central

    LaGorio, Lisa A; Carnaby-Mann, Giselle D; Crary, Michael A

    2008-01-01

    Traditionally, treatment of dysphagia and dysphonia has followed a specificity approach whereby treatment plans have focused on each dysfunction individually. Recently however, a therapeutic cross-system effect has been proposed between these two dysfunctions. At least one study has demonstrated swallowing improvement in subjects who completed a dysphonia treatment program. However, we are unaware of any evidence demonstrating the converse effect. In this paper, we present a case-report of a 74 year old male who demonstrated improvement in selected vocal parameters after completion of a dysphagia therapy program. Dysphagia therapy resulted in improved laryngeal function in this subject. Results implicate improved vocal fold tension with increased glottal closure. Further investigation into the potential for this cross-system effect is warranted. PMID:18667069

  5. Observations of loops and prominences

    NASA Technical Reports Server (NTRS)

    Strong, Keith T.

    1994-01-01

    We review recent observations by the Yohkoh-SXT (Soft X-ray Telescope) in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (greater than or equal to 32 s full-disk and greater than or equal to 2 s partial-frame images), high spatial resolution (greater than or equal to 2.5 arcsec pixels), high sensitivity (EM less than or equal to 10(exp 42) cm(exp -3)), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 105 km. The cross-section of most loops seems to be constant. Loops displaying significant Gamma's are the exception, not the rule, implying the presence of widespread currents in the corona. All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly

  6. Laryngeal involvement causing dysphonia in a 29 year old nursing mother with lepromatous leprosy

    PubMed Central

    Fwoloshi, Sombo; Machona, Sharon Musonda; Mudenda, Victor; Ngalamika, Owen

    2015-01-01

    Leprosy is a granulomatous disease that mainly affects the skin and peripheral nerves. It is caused by infection with mycobacterium leprae or mycobacterium lepromatosus. In most instances, diagnosis of leprosy can easily be made based on the clinical signs and symptoms. However, when patients present with atypical features, clinical diagnosis can be a challenge. We report a case of a nursing mother with lepromatous leprosy who presented with dysphonia and skin lesions initially thought to be a deep cutaneous mycosis. PMID:26327983

  7. Prominent Doublet Ridges on Europa

    NASA Technical Reports Server (NTRS)

    1997-01-01

    This image of Jupiter's satellite Europa was obtained from a range of 7364 miles (11851 km) by the Galileo spacecraft during its fourth orbit around Jupiter and its first close pass of Europa. The image spans 30 miles by 57 miles (48 km x 91 km) and shows features as small as 800 feet (240 meters) across, a resolution more than 150 times better than the best Voyager coverage of this area. The sun illuminates the scene from the right. The large circular feature in the upper left of the image could be the scar of a large meteorite impact. Clusters of small craters seen in the right of the image may mark sites where debris thrown from this impact fell back to the surface. Prominent doublet ridges over a mile (1.6 km) wide cross the plains in the right part of the image; younger ridges overlap older ones, allowing the sequence of formation to be determined. Gaps in ridges indicate areas where emplacement of new surface material has obliterated pre-existing terrain.

    The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC.

    This image and other images and data received from Galileo are posted on the Galileo mission home page on the World Wide Web at http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo

  8. Solar Prominence Fine Structure and Dynamics

    NASA Astrophysics Data System (ADS)

    Berger, Thomas

    2014-01-01

    We review recent observational and theoretical results on the fine structure and dynamics of solar prominences, beginning with an overview of prominence classifications, the proposal of possible new ``funnel prominence'' classification, and a discussion of the recent ``solar tornado'' findings. We then focus on quiescent prominences to review formation, down-flow dynamics, and the ``prominence bubble'' phenomena. We show new observations of the prominence bubble Rayleigh-Taylor instability triggered by a Kelvin-Helmholtz shear flow instability occurring along the bubble boundary. Finally we review recent studies on plasma composition of bubbles, emphasizing that differential emission measure (DEM) analysis offers a more quantitative analysis than photometric comparisons. In conclusion, we discuss the relation of prominences to coronal magnetic flux ropes, proposing that prominences can be understood as partially ionized condensations of plasma forming the return flow of a general magneto-thermal convection in the corona.

  9. Some crucial corona and prominence observations

    NASA Technical Reports Server (NTRS)

    Tandberg-Hanssen, E. A.

    1986-01-01

    A number of theories and hypotheses are currently being developed to explain the often complex behavior of corona and prominence plasmas. In order to test the theories and hypotheses certain crucial observations are necessary. Some of these observations are examined and a few conclusions are drawn. Corona mass balance, corona and prominence classifications, prominence formation and stability, and coronal mass ejection are dicussed.

  10. Re-interpreting Prominences Classified as Tornadoes

    NASA Astrophysics Data System (ADS)

    Martin, Sara F.; Venkataramanasastry, Aparna

    2015-04-01

    Some papers in the recent literature identify tornado prominences with barbs of quiescent prominences while papers in the much older historic literature include a second category of tornado prominence that does not correspond to a barb of a quiescent prominence. The latter are described as prominence mass rotating around a nearly vertical axis prior to its eruption and the rotation was verified by spectral measurements. From H alpha Doppler-shifted mass motions recorded at Helio Research or the Dutch Open Telescope, we illustrate how the apparent tornado-like motions, identified with barbs, are illusions in our mind’s eye resulting from poorly resolved counterstreaming threads of mass in the barbs of quiescent prominences. In contrast, we confirm the second category of rotational motion in prominences shortly before and during eruption. In addition, we identify this second category as part of the late phase of a phenomenon called the roll effect in erupting prominences. In these cases, the eruption begins with the sideways rolling of the top of a prominence. As the eruption proceeds the rolling motion propagates down one leg or both legs of the prominence depending on whether the eruption is asymmetric or symmetric respectively. As an asymmetric eruption continues, the longer lasting leg becomes nearly vertical and its rotational motion also continues. If only this phase of the eruption was observed, as in some historic cases, it was called a tornado prominence. However, when we now observe entire eruptions in time-lapse sequences, the similarity to terrestrial tornadoes is lost. We conclude that neither prominence barbs, that give the illusion of rotation, nor the cases of true rotational motion, in the legs of erupting prominences, are usefully described as tornado prominences when the complete prominence structure or complete erupting event is observed.

  11. Simulations of Buoyant Plumes in Solar Prominences

    NASA Astrophysics Data System (ADS)

    Hurlburt, N.; Berger, T.

    2012-08-01

    Observations of solar prominences reveal a complex, dynamic flow field within them. The flow field within quiescent prominences is characterized by long "threads" and dark "bubbles" that fall and rise (respectively) in a thin sheet. The flow field in active prominences display more helical motions that travel along the axis of the prominence. We explore the possible dynamics of both of these with the aid of 2.5D MHD simulations. Our model, compressible plasma possesses density and temperature gradients and resides in magnetic field configurations that mimc those of a solar prominence. We present results of various configurations and discuss the nonlinear behavior of the resulting dynamics.

  12. Brainstem auditory evoked potentials in a case of 'Manto syndrome', or spasmodic torticollis with thoracic outlet syndrome.

    PubMed

    Disertori, B; Ducati, A; Piazza, M; Pavani, M

    1982-12-01

    A case of spasmodic torticollis with thoracic outlet syndrome observed for over 18 months is presented and discussed. Maximal head rotation (determining backward gaze) was associated with compression of the brachial plexus between the scaleni muscles and motor, sensory and trophic troubles in the hand. This new syndrome is called after the diviner Manto, quoted by Dante Alighieri in his 'Divina Commedia' (Inferno, XX, 52-56). The etiology was ascribed to subacute toxic effects of methylparathion. Brainstem Auditory Evoked Potentials (BAEPs) demonstrated severe brainstem involvement, maximal in the mesencephalic structures. Clinical and neurophysiological data improved on treatment with L-5-hydroxytryptophan. Finally, BAEPs returned to normal. PMID:6984700

  13. Spasmolytic and Anti-Spasmodic Action of Trachyspermum ammi Essence on Rat's Ileum Contraction

    PubMed Central

    Hejazian, Seyed Hassan; Bagheri, Seyyed Majid; Safari, Fatemeh

    2014-01-01

    Background: Trachyspermum ammi is a plant of umbelliferae family and has been traditionally used in the treatment of many gastrointestinal disorders such as indigestion, colic, and diarrhea. Our previous study demonstrated that aqueous extract of Trachyspermum ammi reduced the contractile activity of rat's ileum. Aims: This study was designed to examine the effect of Trachyspermum ammi essence on acetylcholine-induced contraction in isolated rat's ileum. Materials and Methods: In this experimental procedure, the tissue samples were suspended from the transducer lever and mounted on the organ bath containing Tyrode's solution. Isotonic responses were recorded by using an isotonic transducer and the amplitude of contractions. This process was induced by cumulative logarithmic concentrations of acetylcholine before and after exposing tissue by saline and different concentrations of essence. Results: The chemical constituents of the essence from distillate extract of Trachyspermum ammi seeds were studied by gas chromatography mass spectrometry (GC-MS) and the chemical analysis showed many components in which thymol was the main constituent. Our findings showed that the essence derived from the extract in all concentrations used in this study (0.002, 0.005, and 0.01% V/V) significantly reduced acetylcholine-induced contractions (47.34, 60.46, and 86%, respectively, P < 0.05). The same concentrations of the essence also exhibit a significant anti-spasmodic action on acetylcholine-induced contractions (0.1,88.3, and 90.7%, respectively, P < 0.05). Conclusion: Since thymol was the major constituent of our samples of Trachyspermum ammi, the relaxant effect observed in this study is probably due to this agent which can exert an anti-cholinergic property. PMID:25599053

  14. Apparent Solar Tornado-Like Prominences

    NASA Astrophysics Data System (ADS)

    Panasenco, Olga; Martin, Sara F.; Velli, Marco

    2014-02-01

    Recent high-resolution observations from the Solar Dynamics Observatory (SDO) have reawakened interest in the old and fascinating phenomenon of solar tornado-like prominences. This class of prominences was first introduced by Pettit ( Astrophys. J. 76, 9, 1932), who studied them over many years. Observations of tornado prominences similar to the ones seen by SDO had already been documented by Secchi ( Le Soleil, 1877). High-resolution and high-cadence multiwavelength data obtained by SDO reveal that the tornado-like appearance of these prominences is mainly an illusion due to projection effects. We discuss two different cases where prominences on the limb might appear to have a tornado-like behavior. One case of apparent vortical motions in prominence spines and barbs arises from the (mostly) 2D counterstreaming plasma motion along the prominence spine and barbs together with oscillations along individual threads. The other case of apparent rotational motion is observed in a prominence cavity and results from the 3D plasma motion along the writhed magnetic fields inside and along the prominence cavity as seen projected on the limb. Thus, the "tornado" impression results either from counterstreaming and oscillations or from the projection on the plane of the sky of plasma motion along magnetic-field lines, rather than from a true vortical motion around an (apparent) vertical or horizontal axis. We discuss the link between tornado-like prominences, filament barbs, and photospheric vortices at their base.

  15. Loudness predicts prominence: Fundamental frequency lends little

    NASA Astrophysics Data System (ADS)

    Kochanski, G.; Grabe, E.; Coleman, J.; Rosner, B.

    2005-08-01

    We explored a database covering seven dialects of British and Irish English and three different styles of speech to find acoustic correlates of prominence. We built classifiers, trained the classifiers on human prominence/nonprominence judgments, and then evaluated how well they behaved. The classifiers operate on 452 ms windows centered on syllables, using different acoustic measures. By comparing the performance of classifiers based on different measures, we can learn how prominence is expressed in speech. Contrary to textbooks and common assumption, fundamental frequency (f0) played a minor role in distinguishing prominent syllables from the rest of the utterance. Instead, speakers primarily marked prominence with patterns of loudness and duration. Two other acoustic measures that we examined also played a minor role, comparable to f0. All dialects and speaking styles studied here share a common definition of prominence. The result is robust to differences in labeling practice and the dialect of the labeler.

  16. Prominence mass supply and the cavity

    SciTech Connect

    Schmit, Donald J.; Innes, D.; Gibson, S.; Luna, M.; Karpen, J.

    2013-12-20

    A prevalent but untested paradigm is often used to describe the prominence-cavity system: the cavity is under-dense because it is evacuated by supplying mass to the condensed prominence. The thermal non-equilibrium (TNE) model of prominence formation offers a theoretical framework to predict the thermodynamic evolution of the prominence and the surrounding corona. We examine the evidence for a prominence-cavity connection by comparing the TNE model with diagnostics of dynamic extreme ultraviolet (EUV) emission surrounding the prominence, specifically prominence horns. Horns are correlated extensions of prominence plasma and coronal plasma which appear to connect the prominence and cavity. The TNE model predicts that large-scale brightenings will occur in the Solar Dynamics Observatory Atmospheric Imaging Assembly 171 Å bandpass near the prominence that are associated with the cooling phase of condensation formation. In our simulations, variations in the magnitude of footpoint heating lead to variations in the duration, spatial scale, and temporal offset between emission enhancements in the other EUV bandpasses. While these predictions match well a subset of the horn observations, the range of variations in the observed structures is not captured by the model. We discuss the implications of our one-dimensional loop simulations for the three-dimensional time-averaged equilibrium in the prominence and the cavity. Evidence suggests that horns are likely caused by condensing prominence plasma, but the larger question of whether this process produces a density-depleted cavity requires a more tightly constrained model of heating and better knowledge of the associated magnetic structure.

  17. Formation and Plasma Circulation of Solar Prominences

    NASA Astrophysics Data System (ADS)

    Xia, C.; Keppens, R.

    2016-05-01

    Solar prominences are long-lived cool and dense plasma curtains in the hot and rarefied outer solar atmosphere or corona. The physical mechanism responsible for their formation and especially for their internal plasma circulation has been uncertain for decades. The observed ubiquitous downflows in quiescent prominences are difficult to interpret because plasma with high conductivity seems to move across horizontal magnetic field lines. Here we present three-dimensional numerical simulations of prominence formation and evolution in an elongated magnetic flux rope as a result of in situ plasma condensations fueled by continuous plasma evaporation from the solar chromosphere. The prominence is born and maintained in a fragmented, highly dynamic state with continuous reappearance of multiple blobs and thread structures that move mainly downward, dragging along mass-loaded field lines. The circulation of prominence plasma is characterized by the dynamic balance between the drainage of prominence plasma back to the chromosphere and the formation of prominence plasma via continuous condensation. Plasma evaporates from the chromosphere, condenses into the prominence in the corona, and drains back to the chromosphere, establishing a stable chromosphere–corona plasma cycle. Synthetic images of the modeled prominence with the Solar Dynamics Observatory Atmospheric Imaging Assembly closely resemble actual observations, with many dynamical threads underlying an elliptical coronal cavity.

  18. Tornados and Transverse Oscillations during Prominence Eruption

    NASA Astrophysics Data System (ADS)

    Banerjee, Dipankar; Chandrashekhar, K.; Morton, Richard; Pant, Vaibhav; Datta, Ajanta

    2016-07-01

    We report and analyse different phases of a prominence eruption. The winding-unwinding of two footpoints and a tornado like swirling motion is studied. The prominence eruption is observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). This prominence eruption is associated with a CME at a central principal angle of 340 degree, according to the SOHO/LASCO CME catalogue. We can observe the prominence threads and the time distance maps reveal that the loop threads are entangled. We also study the transverse oscillations in the threads. Swirling motions after the eruptions are also quantified and its possible link with the CME kinematics is also studied

  19. Botulinum toxin injection - larynx

    MedlinePlus

    Injection laryngoplasty; Botox-larynx: spasmodic dysphonia-BTX; Essential voice tremor (EVT)-btx; Glottic insufficiency; Percutaneous electromyography-guided botulinum toxin treatment; Percutaneous indirect laryngoscopy- ...

  20. MAGNETIC TOPOLOGY OF BUBBLES IN QUIESCENT PROMINENCES

    SciTech Connect

    Dudik, J.; Aulanier, G.; Schmieder, B.; Zapior, M.; Heinzel, P.

    2012-12-10

    We study a polar-crown prominence with a bubble and its plume observed in several coronal filters by the SDO/AIA and in H{alpha} by the MSDP spectrograph in Bialkow (Poland) to address the following questions: what is the brightness of prominence bubbles in EUV with respect to the corona outside of the prominence and the prominence coronal cavity? What is the geometry and topology of the magnetic field in the bubble? What is the nature of the vertical threads seen within prominences? We find that the brightness of the bubble and plume is lower than the brightness of the corona outside of the prominence, and is similar to that of the coronal cavity. We constructed linear force-free models of prominences with bubbles, where the flux rope is perturbed by inclusion of parasitic bipoles. The arcade field lines of the bipole create the bubble, which is thus devoid of magnetic dips. Shearing the bipole or adding a second one can lead to cusp-shaped prominences with bubbles similar to the observed ones. The bubbles have complex magnetic topology, with a pair of coronal magnetic null points linked by a separator outlining the boundary between the bubble and the prominence body. We conjecture that plume formation involves magnetic reconnection at the separator. Depending on the viewing angle, the prominence can appear either anvil-shaped with predominantly horizontal structures, or cusp-shaped with predominantly vertical structuring. The latter is an artifact of the alignment of magnetic dips with respect to the prominence axis and the line of sight.

  1. Species and tissue-specificity of prokinetic, laxative and spasmodic effects of Fumaria parviflora

    PubMed Central

    2012-01-01

    Background Fumaria parviflora Linn. (Fumariaceae), is a small branched annual herb found in many parts of the world including Saudi Arabia and Pakistan. This study was designed to provide pharmacological basis for the medicinal use of Fumaria parviflora in gut motility disorders. Methods The in-vivo prokinetic and laxative assays were conducted in mice. Isolated intestinal preparations (ileum and jejunum) from different animal species (mouse, guinea-pig and rabbit) were separately suspended in tissue baths containing Tyrode's solution bubbled with carbogen and maintained at 37°C. The spasmogenic responses were recorded using isotonic transducers coupled with PowerLab data acquisition system. Results The aqueous-methanol extract of Fumaria parviflora (Fp.Cr), which tested positive for the presence of alkaloids, saponins, tannins and anthraquinones showed partially atropine-sensitive prokinetic and laxative activities in the in-vivo in mice at 30 and 100 mg/kg. In the in-vitro studies, Fp.Cr (0.01-1 mg/ml) caused a concentration-dependent atropine-sensitive stimulatory effect both in mouse tissues (jejunum and ileum), and rabbit jejunum but had no effect in rabbit ileum. In guinea-pig tissues (ileum and jejunum), the crude extract showed a concentration-dependent stimulatory effect with higher efficacy in ileum and the effect was partially blocked by atropine, indicating the involvement of more than one types of gut-stimulant components (atropine-sensitive and insensitive). This could be a plausible reason for the greater efficacy of Fp.Cr in gut preparations of guinea-pig than in rabbit or mouse. Conclusions This study shows the prokinetic, laxative and spasmodic effects of the plant extract partially mediated through cholinergic pathways with species and tissue-selectivity, and provides a sound rationale for the medicinal use of Fumaria parviflora in gut motility disorders such as, indigestion and constipation. This study also suggests using different species to

  2. Formation of Prominences and Dynamics Before Eruption

    NASA Astrophysics Data System (ADS)

    Luna, Manuel

    2016-07-01

    Solar prominences have fascinated to astronomers since the first scientific observations of eclipses. Prominences are spectacular manifestations of both quiescent and eruptive solar activity. These are cool and dense structures suspended in the very hot solar corona. The continuous improvements in spatial and temporal resolution from both ground- and space-based instruments have revealed a rich structure and dynamics of prominences. Despite over one century of observations, the magnetic structure of a solar prominence, the origin of its mass, and their dynamics remain vigorously debated issues with profound implications for space weather. In this talk I will address the question of the origin of the cool mass of prominences by reviewing past and recent advances in theoretical modelling.

  3. Ion-Neutral Coupling in Solar Prominence

    NASA Technical Reports Server (NTRS)

    Gilbert, H.; DeVore, C. R.; Karpen, J.; Kucera, T.; Antiochos, S.; Kawashima, R.

    2011-01-01

    Coupling between ions and neutrals in magnetized plasmas is fundamentally important to many aspects of heliophysics, including our ionosphere, the solar chromosphere, the solar wind interaction with planetary atmospheres, and the interface between the heliosphere and the interstellar medium. Ion-neutral coupling also plays a major role in the physics of solar prominences. By combining theory, modeling, and observations we are working toward a better understanding of the structure and dynamics of partially ionized prominence plasma. Two key questions are addressed in the present work: 1) what physical mechanism(s) sets the cross-field scale of prominence threads? 2) Are ion-neutral interactions responsible for the vertical flows and structure in prominences? We present initial results from a study investigating what role ion-neutral interactions play in prominence dynamics and structure. This research was supported by NASA.

  4. Basic properties and models of solar prominences

    NASA Technical Reports Server (NTRS)

    Forbes, T. G.

    1990-01-01

    Prominences are relatively cool (10,000 K) and dense plasma clouds which may persist for 100 days or more in the midst of the much hotter (1 million K) and more tenuous (10 exp 9/cu cm) corona. Many observations imply that the magnetic field in and around prominences is responsible both for isolating prominences from the corona and for supporting them against gravity. It is not at all obvious how the magnetic field can do both these tasks, but the limited theoretical models that are available suggest that a magnetic-flux rope is involved. Using a new analytical model, it is argued that the flux rope could also play a key role in the eruption of a prominence by supplying the magnetic energy necessary to drive the prominence outwards.

  5. Prominences: The Key to Understanding Solar Activity

    NASA Technical Reports Server (NTRS)

    Karpen, Judy T.

    2011-01-01

    Prominences are spectacular manifestations of both quiescent and eruptive solar activity. The largest examples can be seen with the naked eye during eclipses, making prominences among the first solar features to be described and catalogued. Steady improvements in temporal and spatial resolution from both ground- and space-based instruments have led us to recognize how complex and dynamic these majestic structures really are. Their distinguishing characteristics - cool knots and threads suspended in the hot corona, alignment along inversion lines in the photospheric magnetic field within highly sheared filament channels, and a tendency to disappear through eruption - offer vital clues as to their origin and dynamic evolution. Interpreting these clues has proven to be contentious, however, leading to fundamentally different models that address the basic questions: What is the magnetic structure supporting prominences, and how does so much cool, dense plasma appear in the corona? Despite centuries of increasingly detailed observations, the magnetic and plasma structures in prominences are poorly known. Routine measurements of the vector magnetic field in and around prominences have become possible only recently, while long-term monitoring of the underlying filament-channel formation process also remains scarce. The process responsible for prominence mass is equally difficult to establish, although we have long known that the chromosphere is the only plausible source. As I will discuss, however, the motions and locations of prominence material can be used to trace the coronal field, thus defining the magnetic origins of solar eruptions. A combination of observations, theory, and numerical modeling must be used to determine whether any of the competing theories accurately represents the physics of prominences. I will discuss the criteria for a successful prominence model, compare the leading models, and present in detail one promising, comprehensive scenario for

  6. Investigation on Eruptive Prominences Observed by SDO

    NASA Astrophysics Data System (ADS)

    Su, Yingna; McCauley, Patrick; van Ballegooijen, Adriaan; Ji, Haisheng; Reeves, Katharine; DeLuca, Edward

    2015-04-01

    We will present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by SDO/AIA (end-on view) and displays a quasi vertical-thread structure. Bright U-shape (horn-like) structure is observed surrounding the upper portion of the prominence (171 Angstrom) before the eruption and becomes more prominent during the eruption. When viewed on the disk, STEREO-B shows that this long prominence is composed of a series of vertical threads and displays a half loop-like structure during the eruption. We focus on the magnetic support of the prominence by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO. During the eruption, AIA observes dark ribbons seen in absorption at 171 Angstrom in corresponding to the bright ribbons at 304 Angstrom. We construct a series of magnetic field models (including sheared arcade model, twisted flux rope model, and model with HFT), then compare with observations. Various observational characteristics appear to support the twisted flux rope model. Our study suggests that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast rise phase, and evidence of reconnection (post-eruption arcade, new U-shape Structure, rising blobs) appears about one hour later. We will also present a statistical study on the kinematics of limb eruptive prominences observed by SDO/AIA. A brief introduction on an online catalog of prominence eruptions observed by SDO/AIA will also be presented.

  7. Ion-Neutral Coupling in Solar Prominences

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly

    2011-01-01

    Interactions between ions and neutrals in a partially ionized plasma are important throughout heliophysics, including near the solar surface in prominences. Understanding how ion-neutral coupling affects formation, support, structure, and dynamics of prominences will advance our physical understanding of magnetized systems involving a transition from a weakly ionized dense gas to a fully ionized tenuous plasma. We address the fundamental physics of prominence support, which is normally described in terms of a magnetic force on the prominence plasma that balances the solar gravitational force, and the implications for observations. Because the prominence plasma is only partially ionized, it is necessary to consider the support of the both the ionized and neutral components. Support of the neutrals is accomplished through a frictional interaction between the neutral and ionized components of the plasma, and its efficacy depends strongly on the degree of ionization of the plasma. More specifically, the frictional force is proportional to the relative flow of neutral and ion species, and for a sufficiently weakly ionized plasma, this flow must be relatively large to produce a frictional force that balances gravity. A large relative flow, of course, implies significant draining of neutral particles from the prominence. We evaluate the importance of this draining effect for a hydrogen-helium plasma, and consider the observational evidence for cross-field diffusion of neutral prominence material.

  8. Effects of Omeprazole Over Voice Quality in Muscle Tension Dysphonia Patients With Laryngopharyngeal Reflux

    PubMed Central

    Kandogan, Tolga; Aksoy, Gökce; Dalgic, Abdullah

    2012-01-01

    Backround Laryngopharyngeal reflux (LPR) is the backflow of stomach contents above upper esophageal sphincter, into the pharynx, larynx, and upper aerodigestive system. Objectives In this study, effects of omeprazole over voice quality in muscle tension dysphonia with laryngopharyngeal reflux was ınvestigated. Patients and Methods Nine patients, 7 males and 2 females, aged between 27-43 (mean age:31) were included to this study. The diagnosis of muscle tension dysphonia with LPR was established by video laryngoscopy, rigid scope 70º. The laryngeal changes related with LPR were evaluated according to Reflux Finding Score. The patients received omeprazole 20 mg twice a day for a period of 6 months. None of the patients received voice therapy. Vocal hygiene guidelines were also explained to the patients. Objective and subjective voice parameters (Jitter, shimmer, NHR, Voice Handicap Index, and Auditive analysis; Roughness, breathiness, and hoarseness) were evaluated in this study. Results After treatment with omeprazol, all the parameters showed an improvement in voice quality, but only VHI (P = 0) and shimmer (P = 0,018) are statistically significant. Conclusions For FD patients with LPR condition, we highly recommend that LPR treatment should be part of the treatment plan. PMID:23483094

  9. [Computer-assisted phonetography as a diagnostic aid in functional dysphonia].

    PubMed

    Airainer, R; Klingholz, F

    1991-07-01

    A total of 160 voice-trained and untrained subjects with functional dysphonia were given a "clinical rating" according to their clinical findings. This was a certain value on a scale that recorded the degree of functional voice disorder ranging from a marked hypofunction to an extreme hyperfunction. The phonetograms of these patients were approximated by ellipses, whereby the definition and quantitative recording of several phonetogram parameters were rendered possible. By means of a linear combination of phonetogram parameters, a "calculated assessment" was obtained for each patient that was expected to tally with the "clinical rating". This paper demonstrates that a graduation of the dysphonic clinical picture with regard to the presence of hypofunctional or hyperfunctional components is possible via computerised phonetogram evaluation. In this case, the "calculated assessments" for both male and female singers and non-singers must be computed using different linear combinations. The method can be introduced as a supplementary diagnostic procedure in the diagnosis of functional dysphonia. PMID:1910366

  10. Topological Analyses of Symmetric Eruptive Prominences

    NASA Astrophysics Data System (ADS)

    Panasenco, O.; Martin, S. F.

    Erupting prominences (filaments) that we have analyzed from Hα Doppler data at Helio Research and from SOHO/EIT 304 Å, show strong coherency between their chirality, the direction of the vertical and lateral motions of the top of the prominences, and the directions of twisting of their legs. These coherent properties in erupting prominences occur in two patterns of opposite helicity; they constitute a form of dynamic chirality called the ``roll effect." Viewed from the positive network side as they erupt, many symmetrically-erupting dextral prominences develop rolling motion toward the observer along with right-hand helicity in the left leg and left-hand helicity in the right leg. Many symmetricaly-erupting sinistral prominences, also viewed from the positive network field side, have the opposite pattern: rolling motion at the top away from the observer, left-hand helical twist in the left leg, and right-hand twist in the right leg. We have analysed the motions seen in the famous movie of the ``Grand Daddy" erupting prominence and found that it has all the motions that define the roll effect. From our analyses of this and other symmetric erupting prominences, we show that the roll effect is an alternative to the popular hypothetical configuration of an eruptive prominence as a twisted flux rope or flux tube. Instead we find that a simple flat ribbon can be bent such that it reproduces nearly all of the observed forms. The flat ribbon is the most logical beginning topology because observed prominence spines already have this topology prior to eruption and an initial long magnetic ribbon with parallel, non-twisted threads, as a basic form, can be bent into many more and different geometrical forms than a flux rope.

  11. Nonlinear MHD Waves in a Prominence Foot

    NASA Astrophysics Data System (ADS)

    Ofman, L.; Knizhnik, K.; Kucera, T.; Schmieder, B.

    2015-11-01

    We study nonlinear waves in a prominence foot using a 2.5D MHD model motivated by recent high-resolution observations with Hinode/Solar Optical Telescope in Ca ii emission of a prominence on 2012 October 10 showing highly dynamic small-scale motions in the prominence material. Observations of Hα intensities and of Doppler shifts show similar propagating fluctuations. However, the optically thick nature of the emission lines inhibits a unique quantitative interpretation in terms of density. Nevertheless, we find evidence of nonlinear wave activity in the prominence foot by examining the relative magnitude of the fluctuation intensity (δI/I ˜ δn/n). The waves are evident as significant density fluctuations that vary with height and apparently travel upward from the chromosphere into the prominence material with quasi-periodic fluctuations with a typical period in the range of 5-11 minutes and wavelengths <2000 km. Recent Doppler shift observations show the transverse displacement of the propagating waves. The magnetic field was measured with the THEMIS instrument and was found to be 5-14 G. For the typical prominence density the corresponding fast magnetosonic speed is ˜20 km s-1, in qualitative agreement with the propagation speed of the detected waves. The 2.5D MHD numerical model is constrained with the typical parameters of the prominence waves seen in observations. Our numerical results reproduce the nonlinear fast magnetosonic waves and provide strong support for the presence of these waves in the prominence foot. We also explore gravitational MHD oscillations of the heavy prominence foot material supported by dipped magnetic field structure.

  12. Helical flux ropes in solar prominences

    NASA Technical Reports Server (NTRS)

    Martens, P. C. H.; Van Ballegooijen, A. A.

    1990-01-01

    The present numerical method for the computation of force-free, cancelling magnetic structures shows that flux cancellation at the neutral line in a sheared magnetic arcade generates helical field lines that can support a prominence's plasma. With increasing flux cancellation, the axis of the helical fields moves to greater heights; this is suggestive of a prominence eruption. Two alternative scenarios are proposed for the formation of polar crown prominences which yield the correct axial magnetic field sign. Both models are noted to retain the formation of helical flux tubes through flux cancellation as their key feature.

  13. The initial trajectories of eruptive solar prominences

    NASA Astrophysics Data System (ADS)

    Filippov, B. P.

    2016-03-01

    Trajectories of eruptive prominences are compared with the shapes of coronal neutral surfaces calculated in a potential approximation using photospheric measurements. Space-based Solar Dymamics Observatory and STEREO observations carried out at different viewing angles enable a precise determination of a prominence's position at successive times during its eruption. In the initial segments of their trajectories, eruptive prominences move along neutral surfaces ( B r = 0) of the potential coronal magnetic field. This can be used to predict the directions of subsequent coronal mass ejections and to estimate their geoefficiency.

  14. Dysphonia: medical treatment and a medical voice hygiene advice approach. A prospective randomised pilot study.

    PubMed

    Pedersen, M; Beranova, A; Møller, S

    2004-07-01

    For many years all patients with dysphonia referred to in the literature as resulting from non-organic (functional) voice disorders were sent to speech therapy. Medical diagnoses were not taken into account. In our earlier Cochrane review on vocal cord nodules we discovered that evidence-based research in the area of benign voice disorders with dysphonia, and with or without slight benign swellings including nodules on the vocal cords, was lacking at that time. Therefore, a prospective randomised pilot study based on our Cochrane review has been made on dysphonic patients with non-organic (function provoked?) voice disorders as the basis for further evidence-based studies. Medical treatment was based on the scientific approach that once a micro-organic disorder caused by reflux, infection, allergy or environmental irritatants (e.g., dust or noise in the workplace) was discovered by very careful anamnesis and systematic objective routine analyses and was treated effectively, with documentation, the non-organic voice disorder disappeared, as, e.g., in the case of a diagnosis and treatment of helicobakter pylori. The reason is that the mucosal swelling/dysfunction of the vocal cords is secondary. In order to try to understand why the recommendation to all these patients for many years was only voice therapy, which the speech therapists "felt to be effective", updated voice-hygiene advice (for posture, accents of the diaphragm, intonation pattern and resonance) was given by experienced laryngologists, randomised with the updated medical diagnosis/therapy in order to elucidate what effect the training might have. No evidence-based studies in the literature document any effect. The crucial point seemed to be that doctors mostly did not examine any other diagnoses other than the "dysphonia" and did not dig down to any of the medical reasons when the vocal fold diagnosis of "non- organic disorders" was made. This should be changed in the future. This pilot study was based

  15. NASA's SDO Sees Unraveling Solar Prominence

    NASA Video Gallery

    An elongated solar prominence rose up above the sun’s surface and slowly unraveled on Feb. 3, 2016, as seen in this video by NASA’s Solar Dynamics Observatory, or SDO. The sun appears to move in th...

  16. EUV observations of quiescent prominences from Skylab

    NASA Technical Reports Server (NTRS)

    Moe, O. K.; Cook, J. W.; Mango, S. A.

    1979-01-01

    Measurements of line intensities and line widths for three quiescent prominences observed with Naval Research Laboratory slit spectrograph on ATM/Skylab are reported. The wavelengths of the observed lines cover the range 1175 A to 1960 A. The measured intensities have been calibrated to within approximately a factor 2 and are average intensities over a 2 arcsec by 60 arcsec slit. Nonthermal velocities from the measured line widths are derived. The nonthermal velocity is found to increase with temperature in the prominence transition zone. Electron densities and pressures are derived from density sensitive line ratios. Electron pressures for two of the prominences are found to lie in the range 0.04-0.08 dyn/sq cm, while values for the third and most intense and active of the three prominences are in the range 0.07-0.22 dyn/sq cm.

  17. Ring-shaped Prominence Erupts from Sun

    NASA Video Gallery

    A coronal mass ejection (CME) on Jan. 31, 2013 was accompanied by a large prominence eruption best visible in light with a wavelength of 304 angstroms. NASA’s Solar Dynamics Observatory captured ...

  18. Hefty Prominence Eruption Observed by SDO

    NASA Video Gallery

    A mass of solar material gathered itself into a twisting mass, spun around for a bit, then rose up and broke apart over a 10-hour period on Oct. 13, 2015. Prominences are unstable clouds of gas tet...

  19. Formation and eruption of solar prominences

    NASA Technical Reports Server (NTRS)

    Van Ballegooijen, A. A.; Martens, P. C. H.

    1989-01-01

    A model for the magnetic field associated with solar prominences is considered. It is shown that flux cancellation at the neutral line of a sheared magnetic arcade leads to the formation of helical field lines which are capable, in principle, of supporting prominence plasma. A numerical method for the computation of force-free, canceling magnetic structures is presented. Starting from an initial potential field we prescribe the motions of magnetic footpoints at the photosphere, with reconnection occurring only at the neutral line. As more and more flux cancels, magnetic flux is transferred from the arcade field to the helical field. Results for a particular model of the photospheric motions are presented. The magnetic structure is found to be stable: the arcade field keeps the helical field tied down at the photosphere. The axis of the helical field moves to larger and larger height, suggestive of prominence eruption. These results suggest that prominence eruptions may be trigered by flux cancellation.

  20. A distinctive type of ascending prominence - 'Fountain'

    NASA Technical Reports Server (NTRS)

    Tandberg-Hanssen, E.; Hansen, R. T.; Riddle, A. C.

    1975-01-01

    Cinematographic observations of solar prominences made at Mauna Loa, Hawaii, during the past few years suggest that there is a well-defined subclass of ascending prominences characterized by closed-system transference of chromospheric material along an arch or loop (up one leg and down the other). While this occurs, the entire prominence envelope steadily rises upward and expands through the corona. These prominences are denoted as 'fountains'. Several examples are described. Fountains appear to be well contained by coronal magnetic fields. Their total kinetic energy is of the order of 10 to the 30th power erg, but dissipation is typically quite slow (over time periods of 100 min or so), so that the correlative disturbances (radio bursts, coronal transients, chromospheric brightenings) are generally not spectacular or nonexistent.

  1. A DROPLET MODEL OF QUIESCENT PROMINENCE DOWNFLOWS

    SciTech Connect

    Haerendel, G.; Berger, T.

    2011-04-20

    Observations of quiescent prominences with the Solar Optical Telescope on the Hinode satellite have revealed the ubiquitous existence of downflows forming coherent thin and highly structured vertically oriented threads with velocities between 10 and 20 km s{sup -1}. Their widths range between 300 and 500 km. They are often initiated at the top of the visible prominence, but sometimes also at intermediate level. We propose that the downflows are made of plasma packets that squeeze themselves through the dominantly horizontal field under the action of gravity. Their origin is assumed to be hot plasma supplied from either inside or the immediate vicinity of the prominence and condensing at its top. Under compression and further cooling, the matter overflows to the flanks of the prominence dragging its magnetic field with it. Under the increasing action of gravity, vertical structures are forming which eventually disconnect from the field of the inflow channel thus forming finite plasma packets. This process is reminiscent of water flowing over a mountain ridge and breaking up into a multitude of droplets. Like water droplets being subject to air drag, the falling plasma droplets experience a drag force by the horizontal prominence field and assume a steady vertical velocity. This happens via the excitation of Alfven waves. Lateral confinement by the prominence field determines their spatial extent. The small scales of the droplets and the directional balance of their internal tangled magnetic fields can explain the absence of appreciable vertical components in magnetic field measurements. On the basis of the observed width and vertical speed of the downflows and by adopting a prominence field of about 8 G, we derive central density and temperature of the droplets, which turn out to be quite consistent with known prominence characteristics. In the formulation of the drag force a dimensionless 'magnetic drag coefficient' has been introduced with a value well below unity.

  2. An arcade-like eruptive prominence

    NASA Astrophysics Data System (ADS)

    Zhong, Shu-Hua; Zhan, La-Sheng

    2004-12-01

    An eruptive prominence happened on the east-northern limb of the Sun on March 7, 1991. It appeared in a relatively quiet region where any activity phenomena such as flare, filament and sunspot etc. was not found. The maximum height reachable of the prominence was 6.97×104km and its maximum length reached as 11.6×104km. The eruptive prominence might belong to the one of the middle-smaller scale according to its size in morphology. The course of the eruption exhibited some properties: ascending rapidly and descending slowly just like the process of the flare eruption. After the eruption, the most material in the prominence basically moved along a parabola under the action of magnetic force lines forming the arcade-like shape and keeping it till to the disappearance of the prominence. Before and after descending, a little matter came from the top part was ejected and divorced from the main body of the prominence and diffused into the interplanetary space.

  3. DIAGNOSING THE PROMINENCE-CAVITY CONNECTION

    SciTech Connect

    Schmit, Donald J.; Gibson, Sarah

    2013-06-10

    Prominences and cavities are ubiquitously observed together, but the physical link between these disparate structures has not been established. We address this issue by using dynamic emission in the extreme ultraviolet to probe the connections of these structures. The SDO/AIA observations show that the cavity exhibits excessive emission variability compared to the surrounding quiet-Sun streamer, particularly in the 171 A bandpass. We find that this dynamic emission takes the form of coherent loop-like brightening structures which emanate from the prominence into the central cavity. The geometry of these structures, dubbed prominence horns, generally mimics the curvature of the cavity boundary. We use a space-time statistical analysis of two cavities in multiple AIA bandpasses to constrain the energetic properties of 45 horns. In general, we find there is a positive correlation between the light curves of the horns in the 171 A and 193 A bandpasses; however, the 193 A emission is a factor of five weaker. There is also a strong correlation between structural changes to the prominence as viewed in the He II 304 A bandpass and the enhanced 171 A emission. In that bandpass, the prominence appears to extend several megameters along the 171 A horn where we observe co-spatial, co-temporal 304 A and 171 A emission dynamics. We present these observations as evidence of the magnetic and energetic connection between the prominence and the cavity. Further modeling work is necessary to explain the physical source and consequences of these events, particularly in the context of the traditional paradigm: the cavity is underdense because it supplies mass to the overdense prominence.

  4. Magnetic Reconnection Models of Prominence Formation

    NASA Astrophysics Data System (ADS)

    Welsch, B. T.; DeVore, C. R.; Antiochos, S. K.

    2005-12-01

    To investigate the hypothesis that prominences form by magnetic reconnection between initially distinct flux systems in the solar corona, we simulate coronal magnetic field evolution when two flux systems are driven together by boundary motions. In particular, we focus on configurations similar to those in the quiescent prominence formation model of Martens & Zwaan. We find that reconnection proceeds very weakly, if at all, in configurations driven with global shear flows (i.e., differential rotation); reconnection proceeds much more efficiently in similar configurations that are driven to collide directly, with converging motions along the neutral line that lead to flux cancellation; reconnected fields from this process can exhibit sheared, dipped field lines along the neutral line, consistent with prominence observations. Our field configurations do not possess the ``breakout'' topology, and eruptions are not observed, even though a substantial amount of flux is canceled in some runs.

  5. Inharmonicity Analysis: A Novel Physical Method for Acoustic Screening of Dysphonia

    NASA Astrophysics Data System (ADS)

    Matteson, Sam; Lu, Fang-Ling

    2008-10-01

    In the United States 6.8% of men, women, and children report current voice problems and approximately 29% will report some problems during their lifetime. Often this dysphonia is due to pathologies of the vocal folds. The authors (a physicist and a speech pathologist) describe an interdisciplinary approach that shows promise of detecting physiological abnormalities of the vocal folds from an analysis of the Fourier spectrum of spoken ``tokens.'' The underlying principle maintains that the normal human vocal fold is a linear oscillator that emits overtones that are very nearly precise integral values of the fundamental. Physiological problems of the vocal folds, however, introduce mechanical non-linearities that manifest themselves as frequency deviations from the ideal harmonic (that is, integral) values. The authors quantify this inharmonicity, describing and illustrating how one can obtain and analyze such data. They outline, as well, a proposed program to assess the clinical sensitivity and significance of the analysis discussed in this work.

  6. De novo FUS P525L mutation in Juvenile amyotrophic lateral sclerosis with dysphonia and diplopia.

    PubMed

    Leblond, Claire S; Webber, Alina; Gan-Or, Ziv; Moore, Fraser; Dagher, Alain; Dion, Patrick A; Rouleau, Guy A

    2016-04-01

    Juvenile amyotrophic lateral sclerosis (jALS) is characterized by progressive upper and lower motor neuron degeneration leading to facial muscle spasticity, spastic dysarthria, and spastic gait with an early onset (before 25 years old). Unlike adult-onset amyotrophic lateral sclerosis (ALS), patients with jALS tend to have slower progression of motor neuron disease and prolonged survival to a normal life expectancy. Mutations in FUS gene have been reported in jALS,(1) including p.P525L mutation that has been consistently associated with early onset and aggressive presentation.(2) Here, we report a patient carrying p.P525L FUS mutation and experiencing an aggressive course of ALS presenting with dysphonia and diplopia. PMID:27123482

  7. Non-organic dysphonia. II. A comparison of subglottal pressures in normal and pathological voices.

    PubMed

    Gramming, P

    1989-01-01

    In previous investigations, typical phonetogram differences have been revealed between healthy and pathological voices: the average maximum and minimum sound pressure levels that a patient suffering from non-organic dysphonia can produce at different fundamental frequencies deviate significantly from the corresponding values for a healthy voice. The subglottal pressure, being the primary tool for regulating the sound pressure level of voice, was estimated from the oral pressure during the voiceless stop/p/in 10 female and 10 male subjects with normal voices and in 10 female and 10 male non-organic dysphonic patients. In loud phonation, the female patients had significantly lower values than the female healthy subjects, while no corresponding significant difference was seen between the male subjects. In soft phonation, the male patients had significantly higher values than the normal healthy subjects, while the females showed no significant difference. PMID:2929314

  8. THE THERMAL INSTABILITY OF SOLAR PROMINENCE THREADS

    SciTech Connect

    Soler, R.; Goossens, M.; Ballester, J. L.

    2011-04-10

    The fine structure of solar prominences and filaments appears as thin and long threads in high-resolution images. In H{alpha} observations of filaments, some threads can be observed for only 5-20 minutes before they seem to fade and eventually disappear, suggesting that these threads may have very short lifetimes. The presence of an instability might be the cause of this quick disappearance. Here, we study the thermal instability of prominence threads as an explanation of their sudden disappearance from H{alpha} observations. We model a prominence thread as a magnetic tube with prominence conditions embedded in a coronal environment. We assume a variation of the physical properties in the transverse direction so that the temperature and density continuously change from internal to external values in an inhomogeneous transitional layer representing the particular prominence-corona transition region (PCTR) of the thread. We use the nonadiabatic and resistive magnetohydrodynamic equations, which include terms due to thermal conduction parallel and perpendicular to the magnetic field, radiative losses, heating, and magnetic diffusion. We combine both analytical and numerical methods to study linear perturbations from the equilibrium state, focusing on unstable thermal solutions. We find that thermal modes are unstable in the PCTR for temperatures higher than 80,000 K, approximately. These modes are related to temperature disturbances that can lead to changes in the equilibrium due to rapid plasma heating or cooling. For typical prominence parameters, the instability timescale is of the order of a few minutes and is independent of the form of the temperature profile within the PCTR of the thread. This result indicates that thermal instability may play an important role for the short lifetimes of threads in the observations.

  9. Automated image based prominent nucleoli detection

    PubMed Central

    Yap, Choon K.; Kalaw, Emarene M.; Singh, Malay; Chong, Kian T.; Giron, Danilo M.; Huang, Chao-Hui; Cheng, Li; Law, Yan N.; Lee, Hwee Kuan

    2015-01-01

    Introduction: Nucleolar changes in cancer cells are one of the cytologic features important to the tumor pathologist in cancer assessments of tissue biopsies. However, inter-observer variability and the manual approach to this work hamper the accuracy of the assessment by pathologists. In this paper, we propose a computational method for prominent nucleoli pattern detection. Materials and Methods: Thirty-five hematoxylin and eosin stained images were acquired from prostate cancer, breast cancer, renal clear cell cancer and renal papillary cell cancer tissues. Prostate cancer images were used for the development of a computer-based automated prominent nucleoli pattern detector built on a cascade farm. An ensemble of approximately 1000 cascades was constructed by permuting different combinations of classifiers such as support vector machines, eXclusive component analysis, boosting, and logistic regression. The output of cascades was then combined using the RankBoost algorithm. The output of our prominent nucleoli pattern detector is a ranked set of detected image patches of patterns of prominent nucleoli. Results: The mean number of detected prominent nucleoli patterns in the top 100 ranked detected objects was 58 in the prostate cancer dataset, 68 in the breast cancer dataset, 86 in the renal clear cell cancer dataset, and 76 in the renal papillary cell cancer dataset. The proposed cascade farm performs twice as good as the use of a single cascade proposed in the seminal paper by Viola and Jones. For comparison, a naive algorithm that randomly chooses a pixel as a nucleoli pattern would detect five correct patterns in the first 100 ranked objects. Conclusions: Detection of sparse nucleoli patterns in a large background of highly variable tissue patterns is a difficult challenge our method has overcome. This study developed an accurate prominent nucleoli pattern detector with the potential to be used in the clinical settings. PMID:26167383

  10. Objective Dysphonia Quantification in Vocal Fold Paralysis: Comparing Nonlinear with Classical Measures

    PubMed Central

    Little, Max A.; Costello, Declan A. E.; Harries, Meredydd L.

    2010-01-01

    Summary Clinical acoustic voice-recording analysis is usually performed using classical perturbation measures, including jitter, shimmer, and noise-to-harmonic ratios (NHRs). However, restrictive mathematical limitations of these measures prevent analysis for severely dysphonic voices. Previous studies of alternative nonlinear random measures addressed wide varieties of vocal pathologies. Here, we analyze a single vocal pathology cohort, testing the performance of these alternative measures alongside classical measures. We present voice analysis pre- and postoperatively in 17 patients with unilateral vocal fold paralysis (UVFP). The patients underwent standard medialization thyroplasty surgery, and the voices were analyzed using jitter, shimmer, NHR, nonlinear recurrence period density entropy (RPDE), detrended fluctuation analysis (DFA), and correlation dimension. In addition, we similarly analyzed 11 healthy controls. Systematizing the preanalysis editing of the recordings, we found that the novel measures were more stable and, hence, reliable than the classical measures on healthy controls. RPDE and jitter are sensitive to improvements pre- to postoperation. Shimmer, NHR, and DFA showed no significant change (P > 0.05). All measures detect statistically significant and clinically important differences between controls and patients, both treated and untreated (P < 0.001, area under curve [AUC] > 0.7). Pre- to postoperation grade, roughness, breathiness, asthenia, and strain (GRBAS) ratings show statistically significant and clinically important improvement in overall dysphonia grade (G) (AUC = 0.946, P < 0.001). Recalculating AUCs from other study data, we compare these results in terms of clinical importance. We conclude that, when preanalysis editing is systematized, nonlinear random measures may be useful for monitoring UVFP-treatment effectiveness, and there may be applications to other forms of dysphonia. PMID:19900790

  11. Measurements of magnetic fields in solar prominences

    NASA Technical Reports Server (NTRS)

    Deglinnocenti, Egidio Landi

    1986-01-01

    Magnetic fields can be measured, in solar prominences, by means of two different basic mechanisms that are responsible for the introduction (or the reduction) of a given amount of polarization in spectral lines: these are the Zeeman effect and the Hanle effect. Through the splitting of the magnetic components of a spectral line, the Zeeman effect is capable of introducing a certain amount of circular polarization across the line profile. The Hanle effect consist of a modification of the linear polarization that is induced in spectral lines by the anisotropic illumination of the prominence plasma by the photospheric radiation field. These two effects are briefly discussed.

  12. Exploring the properties of Solar Prominence Tornados

    NASA Astrophysics Data System (ADS)

    Ahmad, E.; Panesar, N. K.; Sterling, A. C.; Moore, R. L.

    2015-12-01

    Solar prominences consist of relatively cool and dense plasma embedded in the hotter solar corona above the solar limb. They form along magnetic polarity inversion lines, and are magnetically supported against gravity at heights of up to ~100 Mm above the chromosphere. Often, parts of prominences visually resemble Earth-based tornados, with inverted-cone-shaped structures and internal motions suggestive of rotation. These "prominence tornados" clearly possess complex magnetic structure, but it is still not certain whether they actually rotate around a ''rotation'' axis, or instead just appear to do so because of composite internal material motions such as counter-streaming flows or lateral (i.e. transverse to the field) oscillations. Here we study the structure and dynamics of five randomly selected prominences, using extreme ultraviolet (EUV) 171 Å images obtained with high spatial and temporal resolution by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) spacecraft. All of the prominences resided in non-active-region locations, and displayed what appeared to be tornado-like rotational motions. Our set includes examples oriented both broadside and end-on to our line-of-sight. We created time-distance plots of horizontal slices at several different heights of each prominence, to study the horizontal plasma motions. We observed patterns of oscillations at various heights in each prominence, and we measured parameters of these oscillations. We find the oscillation time periods to range over ~50 - 90 min, with average amplitudes of ~6,000 km, and with average velocities of ~7 kms-1. We found similar values for prominences viewed either broadside or end-on; this observed isotropy of the lateral oscillatory motion suggests that the apparent oscillations result from actual rotational plasma motions and/or lateral oscillations of the magnetic field, rather than to counter-streaming flows. This research was supported by the National

  13. Intonational Prominence on Negatives in English.

    ERIC Educational Resources Information Center

    Yaeger-Dror, Malcah L.

    1985-01-01

    Describes a study done to determine which intonational parameters are most important to the meaning being conveyed within different social settings. Defines the factors that appear to influence the use of pitch and/or intensity prominence on negative words. Found that, in many situations, interactional rules take precedence over linguistic rules.…

  14. Dynamic Features in and nearby a Prominence

    NASA Technical Reports Server (NTRS)

    Kucera, T.; Landi, E.

    2006-01-01

    We will discuss the thermal and dynamic properties of dynamic structures in and around a prominence channel observed on the limb on 17 April 2003. Observations were taken with the Solar and Heliospheric Observatory's Solar Ultraviolet Measurements of Emitted Radiation (SOHO/SUMER) in lines formed at temperatures from 80,000 to 1.6 million K. The instrument was pointed to a single location and took a series of 90 s exposures. Two-dimensional context was provided by the Transition Region and Coronal Explorer (TRACE) in the UV and EUV and by the Kanzelhohe Solar Observatory in H-alpha. Two dynamic features were studied in depth: a prominence activation and repeated motions in a loop nearby the prominence. We were able to calculate three-dimensional geometries and trajectories, differential emission measure, and limits on the average density, kinetic and thermal energies. These observations provide important tests for models of dynamics in prominences and cool (approx.10(exp 5) K) loops.

  15. Calibrating the Prominence Magnetometer (ProMag)

    NASA Astrophysics Data System (ADS)

    Fox, Lewis; Casini, R.

    2013-07-01

    The Prominence Magnetometer (ProMag) is a dual-channel, dual-beam, slit-scanning, full Stokes spectro-polarimeter designed by the High Altitude Observatory at the National Center for Atmospheric Research (HAO/NCAR) for the study of the magnetism of solar prominences and filaments. It was deployed in August 2009 at the 40 cm coronagraph of the Evans Solar Facility (ESF) of the National Solar Observatory on Sacramento Peak (NSO/SP). In its standard mode of operation it acquires spectro-polarimetric maps of solar targets simultaneously in the two chromospheric lines of He I at 587.6 nm and 1083.0 nm. Since August 2011 ProMag has operated in “patrol mode” with a dedicated observer. We aim to routinely measure the vector magnetic field in prominences. The electro-optic modulator and polarization analyzer are integrated into a single mechanical unit located at the coude feed of the telescope. This location was necessary for proper co-alignment of the dual beams, but complicates the precise polarimeter calibration necessary to achieve the sensitivity required for prominence measurements (< 10^-3). At this sensitivity, small variations in optical alignment can become significant. We present a calibration method for ProMag, using a polarizer and retarder at coronagraph prime focus. Calibrations are recorded before and after observations. We discuss the success of this method and its limitations.

  16. Vertical Localization of the Malar Prominence

    PubMed Central

    Kaptein, John S.; Markarian, Alexander

    2015-01-01

    Background: During reconstruction or augmentation, it is important to localize the malar complex in a symmetrical and aesthetically pleasing position. Few studies have determined the location of this feature and none related the location to gender, age, or ethnicity. Some of these have attempted to relate the position to the aesthetically pleasing Golden Ratio φ. Methods: We assessed the vertical location of the malar prominence relative to other facial landmarks, determined consistency among individuals, and compared this with values used in artistry. Study population consisted of a convenience sample of 67 patients taken from an otolaryngology practice at a large urban medical center. Coordinates of the malar prominence were referenced to distinct facial landmarks from which the ratio of chin-to-malar prominence to chin-to-eye canthus was determined. Results: Average chin-to-malar prominence distance was 0.793 ± 0.023 (SD) of the chin-to-eye canthus distance. Variability due to the specific image chosen [coefficient of variation (CV) = 1.19%] and combined inter/intrareader variability (CV = 1.71%) validate the methodology. Variability among individuals (CV = 2.84%) indicates population consistency. No difference was found between gender and age groups or between whites and Hispanics. Individuals of other/unknown ethnicities were within the range common to whites and Hispanics. Our population’s value is not different from the value of 0.809 used in artistry, which is based on the Golden Ratio φ. Conclusions: The vertical position of the malar prominence is consistent among individuals, is clinically well-approximated by the value based on the Golden Ratio, and may be useful as a reference for surgical reconstruction or augmentation. PMID:26180712

  17. Damped kink oscillations of flowing prominence threads

    NASA Astrophysics Data System (ADS)

    Soler, R.; Ruderman, M. S.; Goossens, M.

    2012-10-01

    Transverse oscillations of thin threads in solar prominences are frequently reported in high-resolution observations. Two typical features of the observations are that the oscillations are damped in time and that simultaneous mass flows along the threads are detected. Flows cause the dense threads to move along the prominence magnetic structure while the threads are oscillating. The oscillations have been interpreted in terms of standing magnetohydrodynamic (MHD) kink waves of the magnetic flux tubes, which support the threads. The damping is most likely due to resonant absorption caused by plasma inhomogeneity. The technique of seismology uses the observations combined with MHD wave theory to estimate prominence physical parameters. This paper presents a theoretical study of the joint effect of flow and resonant absorption on the amplitude of standing kink waves in prominence threads. We find that flow and resonant absorption can either be competing effects on the amplitude or both can contribute to damp the oscillations depending on the instantaneous position of the thread within the prominence magnetic structure. The amplitude profile deviates from the classic exponential profile of resonantly damped kink waves in static flux tubes. Flow also introduces a progressive shift of the oscillation period compared to the static case, although this effect is in general of minor importance. We test the robustness of seismological estimates by using synthetic data aiming to mimic real observations. The effect of the thread flow can significantly affect the estimation of the transverse inhomogeneity length scale. The presence of random background noise adds uncertainty to this estimation. Caution needs to be paid to the seismological estimates that do not take the influence of flow into account.

  18. Prominence material identified in magnetic cloud

    NASA Astrophysics Data System (ADS)

    Yao, Shuo; Marsch, E.; Tu, C.-Y.

    2010-03-01

    Coronal mass ejections (CMEs) often appear in coronagraph images as three-part structures composed of a leading bright front, a dark cavity and a bright core, which are believed to be associated with the sheath of compressed solar wind, the erupting magnetic flux rope and the cool and dense prominence plasma, respectively. However, a convincing identification of this three-part structure in the in-situ solar wind is extremely rare. Therefore, there still remains an open question as to what kind of signatures these three CME parts will reveal in the in situ data ([5]). Our work presents a clear identification of prominence material from in situ observations of the solar wind magnetic field and plasma parameters. The Helios 2 solar probe detected a magnetic cloud at 0.5 AU on 30 March 1976. In this event, we found a region with lower proton temperature and higher proton number density than outside, which is consistent with key features of a prominence as cold and dense solar material. During the same time we also found the occurrence of what possibly is He+, which is a special ion expected to occur only in prominence ejecta. Furthermore, the above observations were all made at a location related to the turning point of a bipolar structure of the interplanetary magnetic field, which is coincident with the notion that a solar prominence lies under the magnetic field lines of a bipolar region and is oriented along the neutral line. Furthermore, from our analysis of solar wind velocity distribution functions (VDFs) we can confirm by kinetic evidence that the plasma inside this special region is colder and more isotropic than outside. Above all, our observations circumstantially confirm the 3-part CME model as described in references [10] and [7].

  19. Tracking prominent points in image sequences

    NASA Astrophysics Data System (ADS)

    Hahn, Michael

    1994-03-01

    Measuring image motion and inferring scene geometry and camera motion are main aspects of image sequence analysis. The determination of image motion and the structure-from-motion problem are tasks that can be addressed independently or in cooperative processes. In this paper we focus on tracking prominent points. High stability, reliability, and accuracy are criteria for the extraction of prominent points. This implies that tracking should work quite well with those features; unfortunately, the reality looks quite different. In the experimental investigations we processed a long sequence of 128 images. This mono sequence is taken in an outdoor environment at the experimental field of Mercedes Benz in Rastatt. Different tracking schemes are explored and the results with respect to stability and quality are reported.

  20. Models of Filament-Prominence Formation

    NASA Astrophysics Data System (ADS)

    Welsch, Brian T.

    Martens and Zwaan (ApJ v. 558 872) have proposed a prominence/ filament formation model in which differential rotation drives reconnection between two initially unconnected active regions to form helical field lines that support mass and are held down by overlying field. Using an MHD solver with adaptive refinement we simulated this process by imposing a shear flow meant to mimic differential rotation on two bipolar flux distributions meant to mimic distinct active regions. In some runs the flux systems are initially potential while in others they have been twisted by footpoint rotation to inject helicity prior to imposing the shear flow. The resulting structures are studied to understand the role of helicity in the formation of prominence-like structures.

  1. 3D Whole-prominence Fine Structure Modeling. II. Prominence Evolution

    NASA Astrophysics Data System (ADS)

    Gunár, Stanislav; Mackay, Duncan H.

    2015-10-01

    We use the new three-dimensional (3D) whole-prominence fine structure model to study the evolution of prominences and their fine structures in response to changes in the underlying photospheric magnetic flux distribution. The applied model combines a detailed 3D prominence magnetic field configuration with a realistic description of the prominence plasma distributed along multiple fine structures. In addition, we utilize an approximate Hα visualization technique to study the evolution of the visible cool prominence plasma both in emission (prominence) and absorption (filament). We show that the initial magnetic field configuration of the modeled prominence is significantly disturbed by the changing position of a single polarity of a magnetic bipole as the bipole is advected toward the main body of the filament. This leads to the creation of a barb, which becomes the dominant feature visible in the synthetic Hα images of both the prominence and filament views. The evolution of the bipole also creates conditions that lead to the disappearance and reappearance of large portions of the main body. We also show that an arch-like region containing a dark void (a bubble) can be naturally produced in the synthetic prominence Hα images. While not visible in terms of the magnetic field lines, it is due to a lack of Hα emission from low-pressure, low-density plasma located in shallow magnetic dips lying along the lines of sight intersecting the dark void. In addition, a quasi-vertical small-scale feature consisting of short and deep dips, piled one above the other, is produced.

  2. On the thermal durability of solar prominences, or how to evaporate a prominence

    NASA Technical Reports Server (NTRS)

    Malherbe, J. M.; Forbes, T. G.

    1986-01-01

    The thermal disappearance of solar prominences under strong perturbations due to wave heating, Ohmic heating, viscous heating or conduction was investigated. Specifically, how large a thermal perturbation is needed to destroy a stable thermal equilibrium was calculated. It was found that the prominence plasma appears to be thermally very rugged. Its cold equilibrium may most likely be destroyed by either strong magnetic heating or conduction in a range of parameters which is relevant to flares.

  3. A Solar Prominence, Elbow-Prominence, Image From Skylab-3 Mission

    NASA Technical Reports Server (NTRS)

    1973-01-01

    Some of the prominences that float like lazy clouds above the solar surface suddenly erupt and break away from the Sun in cataclysmic action. The trigger of this coronal transient, like many others seen by Skylab's coronagraph, was an eruptive prominence that surged outward from the limb of the Sun, ejecting matter that disturbed the outer corona. This image is of the surge in action in ultraviolet light of ionized helium. Simultaneous observations like this made possible an almost immediate understanding of the new-found cosmic phenomenon. The elbow prominence was accidentally photographed by Astronaut Garriott (Skylab-3) while observing a small flare near the limb of the Sun beneath the mighty arch on August 9, 1973.

  4. Explosive Instability of Prominence Flux Ropes

    SciTech Connect

    Hurricane, O; Fong, R H L; Cowley, S C

    2002-09-04

    The rapid, Alfvenic, time scale of erupting solar-prominences has been an enigma ever since they where first identified. Investigators have proposed a variety of different mechanisms in an effort to account for the abrupt reconfiguration observed. No one mechanism clearly stands out as the single cause of these explosive events. Recent analysis has demonstrated that field lines in the solar atmosphere are metastable to ballooning type instabilities. It has been found previously that in ideal MHD plasmas marginally unstable ballooning modes inevitably become ''explosive'' evolving towards a finite time singularity via a nonlinear 3D instability called ''Nonlinear Magnetohydrodynamic Detonation.'' Thus, this mechanism is a good candidate to explain explosive events observed in the solar atmosphere of our star or in others.

  5. Can prominences form in current sheets

    NASA Technical Reports Server (NTRS)

    Malherbe, J. M.; Forbes, T. G.

    1986-01-01

    Two-dimensional numerical simulations of the formation of cold condensations in a vertical current sheet have been performed using the radiative, resistive MHD equations with line-tied boundary conditions at one end of the sheet. Prominence-like condensations are observed to appear above and below an X-line produced by the onset of the tearing-mode instability. Cooling in the sheet is initiated by Ohmic decay, with the densest condensations occurring in the region downstream of a fast-mode shock. This shock, which is due to the line-tied boundary conditions, terminates one of the two supermagnetosonic reconnection jets that develop when the tearing is fully developed. The condensation properties of shock waves, which may trigger or considerably enhance the conditions for thermal condensation are emphasized.

  6. Observational Constraints on Stellar Flares and Prominences

    NASA Astrophysics Data System (ADS)

    Aarnio, Alicia

    2016-07-01

    Multi-wavelength surveys have catalogued a wealth of stellar flare data for stars representing a broad range of masses and ages. Young solar analogs inform our understanding of the Sun's evolution and the influence of its activity on early solar system formation, while field star observations allow us to place its current activity into context within a statistical ensemble of main-sequence G-type stars. At the same time, stellar observations probe a variety of interior and coronal conditions, providing constraints on models of equilibrium (and loss thereof!) for magnetic structures. In this review, I will focus on our current understanding of stellar flares, prominences, and coronal mass ejections as a function of stellar parameters. As our interpretation of stellar data relies heavily on solar-stellar analogy, I will explore how far into extreme stellar parameter spaces this comparison can be invoked.

  7. Manual Therapy and Exercise to Improve Outcomes in Patients With Muscle Tension Dysphonia: A Case Series

    PubMed Central

    Archer, Kristin R.

    2015-01-01

    Background and Purpose Muscle tension dysphonia (MTD), a common voice disorder that is not commonly referred for physical therapy intervention, is characterized by excessive muscle recruitment, resulting in incorrect vibratory patterns of vocal folds and an alteration in voice production. This case series was conducted to determine whether physical therapy including manual therapy, exercise, and stress management education would be beneficial to this population by reducing excess muscle tension. Case Description Nine patients with MTD completed a minimum of 9 sessions of the intervention. Patient-reported outcomes of pain, function, and quality of life were assessed at baseline and the conclusion of treatment. The outcome measures were the numeric rating scale (NRS), Patient-Specific Functional Scale (PSFS), and Voice Handicap Index (VHI). Cervical and jaw range of motion also were assessed at baseline and postintervention using standard goniometric measurements. Outcomes Eight of the patients had no pain after treatment. All 9 of the patients demonstrated an improvement in PSFS score, with 7 patients exceeding a clinically meaningful improvement at the conclusion of the intervention. Three of the patients also had a clinically meaningful change in VHI scores. All 9 of the patients demonstrated improvement in cervical flexion and lateral flexion and jaw opening, whereas 8 patients improved in cervical extension and rotation postintervention. Discussion The findings suggest that physical therapists can feasibly implement an intervention to improve outcomes in patients with MTD. However, a randomized clinical trial is needed to confirm the results of this case series and the efficacy of the intervention. A clinical implication is the expansion of physical therapy to include referrals from voice centers for the treatment of MTD. PMID:25256740

  8. Reliability of speaking and maximum voice range measures in screening for dysphonia.

    PubMed

    Ma, Estella; Robertson, Jennie; Radford, Claire; Vagne, Sarah; El-Halabi, Ruba; Yiu, Edwin

    2007-07-01

    Speech range profile (SRP) is a graphical display of frequency-intensity occurring interactions during functional speech activity. Few studies have suggested the potential clinical applications of SRP. However, these studies are limited to qualitative case comparisons and vocally healthy participants. The present study aimed to examine the effects of voice disorders on speaking and maximum voice ranges in a group of vocally untrained women. It also aimed to examine whether voice limit measures derived from SRP were as sensitive as those derived from voice range profile (VRP) in distinguishing dysphonic from healthy voices. Ninety dysphonic women with laryngeal pathologies and 35 women with normal voices, who served as controls, participated in this study. Each subject recorded a VRP for her physiological vocal limits. In addition, each subject read aloud the "North Wind and the Sun" passage to record SRP. All the recordings were captured and analyzed by Soundswell's computerized real-time phonetogram Phog 1.0 (Hitech Development AB, Täby, Sweden). The SRPs and the VRPs were compared between the two groups of subjects. Univariate analysis results demonstrated that individual SRP measures were less sensitive than the corresponding VRP measures in discriminating dysphonic from normal voices. However, stepwise logistic regression analyses revealed that the combination of only two SRP measures was almost as effective as a combination of three VRP measures in predicting the presence of dysphonia (overall prediction accuracy: 93.6% for SRP vs 96.0% for VRP). These results suggest that in a busy clinic where quick voice screening results are desirable, SRP can be an acceptable alternate procedure to VRP. PMID:16678387

  9. Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling

    NASA Astrophysics Data System (ADS)

    Gunár, S.; Mackay, D. H.

    2016-07-01

    Aims: We analyze distributions of the magnetic field strength and prominence plasma (temperature, pressure, plasma β, and mass) using the 3D whole-prominence fine structure model. Methods: The model combines a 3D magnetic field configuration of an entire prominence, obtained from non-linear force-free field simulations, with a detailed semi-empirically derived description of the prominence plasma. The plasma is located in magnetic dips in hydrostatic equilibrium and is distributed along multiple fine structures within the 3D magnetic model. Results: We show that in the modeled prominence, the variations of the magnetic field strength and its orientation are insignificant on scales comparable to the smallest dimensions of the observed prominence fine structures. We also show the ability of the 3D whole-prominence fine structure model to reveal the distribution of the prominence plasma with respect to its temperature within the prominence volume. This provides new insights into the composition of the prominence-corona transition region. We further demonstrate that the values of the plasma β are small throughout the majority of the modeled prominences when realistic photospheric magnetic flux distributions and prominence plasma parameters are assumed. While this is generally true, we also find that in the region with the deepest magnetic dips, the plasma β may increase towards unity. Finally, we show that the mass of the modeled prominence plasma is in good agreement with the mass of observed non-eruptive prominences.

  10. A Study of quiescent prominences using SDO and STEREO data

    NASA Astrophysics Data System (ADS)

    Panesar, Navdeep Kaur

    2014-05-01

    In this dissertation, we have studied the structure, dynamics and evolution of two quiescent prominences. Quiescent prominences are large structures and mainly associated with the quiet Sun region. For the analysis, we have used the high spatial and temporal cadence data from the Solar Dynamic Observatory (SDO), and the Solar Terrestrial Relations Observatory (STEREO). We combined the observations from two different directions and studied the prominence in 3D. In the study of polar crown prominence, we mainly investigated the prominence flows on limb and found its association with on-disk brightenings. The merging of diffused active region flux in the already formed chain of prominence caused the several brightenings in the filament channel and also injected the plasma upward with an average velocity of 15 km/s. In another study, we investigated the triggering mechanism of a quiescent tornado-like prominence. Flares from the neighboring active region triggered the tornado-like motions of the top of the prominence. Active region field contracts after the flare which results in the expansion of prominence cavity. The prominence helical magnetic field expands and plasma moves along the field lines which appear as a tornado-like activity. In addition, the thermal structure of the tornado-like prominence and neighbouring active region was investigated by analysing emission in six of the seven EUV channels from the SDO. These observational investigations led to our understanding of structure and dynamics of quiescent prominences, which could be useful for theoretical prominence models.

  11. Stability Study of Coronal Cavities and Prominences

    NASA Astrophysics Data System (ADS)

    de Toma, Giuliana; Gibson, Sarah

    2016-05-01

    Cavity/prominence systems are large-scale coronal structures that can live for many weeks and even months and often end their life in the form of large coronal eruptions. To determine the role of the surrounding ambient coronal field in stabilizing thesesystems against eruption, we examined the extent to which the decline with height of the external coronal magnetic field influences their evolution and likelihood to erupt. We selected coronal cavities observed with SDO/AIA during the rising phase of cycle 24 and divided them in two groups, eruptive and non-eruptive. The height of the cavity, both at the cavity center and top, was directly measured from the SDO/AIA images. The ambient coronal field was derived from a PFSS extrapolation of SDO/HMI magnetograms. We find that the decay index of the potential field above the coronal cavity varies significantly in value for both eruptive and non-eruptive cases but stable cavity systems have, on average, a lower decay index and less complex topology than the eruptive ones.

  12. Quantifying Dysphonia Severity Using a Spectralcepstral-Based Acoustic Index: Comparisons with Auditory-Perceptual Judgements from the CAPE-V

    ERIC Educational Resources Information Center

    Awan, Shaheen N.; Roy, Nelson; JettE, Marie E.; Meltzner, Geoffrey S.; Hillman, Robert E.

    2010-01-01

    This study investigated the relationship between acoustic spectral/cepstral measures and listener severity ratings in normal and disordered voice samples. CAPE-V sentence samples and the vowel /[script]/were elicited from eight normal speakers and 24 patients with varying degrees of dysphonia severity. Samples were analysed for measures of the…

  13. Effect of Laryngopharyngeal Neuromuscular Electrical Stimulation on Dysphonia Accompanied by Dysphagia in Post-stroke and Traumatic Brain Injury Patients: A Pilot Study

    PubMed Central

    2016-01-01

    Objective To investigate the effect of laryngopharyngeal neuromuscular electrical stimulation (NMES) on dysphonia in patients with dysphagia caused by stroke or traumatic brain injury (TBI). Methods Eighteen patients participated in this study. The subjects were divided into NMES (n=12) and conventional swallowing training only (CST, n=6) groups. The NMES group received NMES combined with CST for 2 weeks, followed by CST without NMES for the next 2 weeks. The CST group received only CST for 4 weeks. All of the patients were evaluated before and at 2 and 4 weeks into the study. The outcome measurements included perceptual, acoustic and aerodynamic analyses. The correlation between dysphonia and swallowing function was also investigated. Results There were significant differences in the GRBAS (grade, roughness, breathiness, asthenia and strain scale) total score and sound pressure level (SPL) between the two groups over time. The NMES relative to the CST group showed significant improvements in total GRBAS score and SPL at 2 weeks, though no inter-group differences were evident at 4 weeks. The improvement of the total GRBAS scores at 2 weeks was positively correlated with the improved pharyngeal phase scores on the functional dysphagia scale at 2 weeks. Conclusion The results demonstrate that laryngopharyngeal NMES in post-stroke or TBI patients with dysphonia can have promising effects on phonation. Therefore, laryngopharyngeal NMES may be considered as an additional treatment option for dysphonia accompanied by dysphagia after stroke or TBI. PMID:27606266

  14. Magnetic field and radiative transfer modelling of a quiescent prominence

    NASA Astrophysics Data System (ADS)

    Gunár, S.; Schwartz, P.; Dudík, J.; Schmieder, B.; Heinzel, P.; Jurčák, J.

    2014-07-01

    Aims: The aim of this work is to analyse the multi-instrument observations of the June 22, 2010 prominence to study its structure in detail, including the prominence-corona transition region and the dark bubble located below the prominence body. Methods: We combined results of the 3D magnetic field modelling with 2D prominence fine structure radiative transfer models to fully exploit the available observations. Results: The 3D linear force-free field model with the unsheared bipole reproduces the morphology of the analysed prominence reasonably well, thus providing useful information about its magnetic field configuration and the location of the magnetic dips. The 2D models of the prominence fine structures provide a good representation of the local plasma configuration in the region dominated by the quasi-vertical threads. However, the low observed Lyman-α central intensities and the morphology of the analysed prominence suggest that its upper central part is not directly illuminated from the solar surface. Conclusions: This multi-disciplinary prominence study allows us to argue that a large part of the prominence-corona transition region plasma can be located inside the magnetic dips in small-scale features that surround the cool prominence material located in the dip centre. We also argue that the dark prominence bubbles can be formed because of perturbations of the prominence magnetic field by parasitic bipoles, causing them to be devoid of the magnetic dips. Magnetic dips, however, form thin layers that surround these bubbles, which might explain the occurrence of the cool prominence material in the lines of sight intersecting the prominence bubbles. Movie and Appendix A are available in electronic form at http://www.aanda.org

  15. SIMULATING THE IN SITU CONDENSATION PROCESS OF SOLAR PROMINENCES

    SciTech Connect

    Xia, C.; Keppens, R.; Antolin, P.; Porth, O.

    2014-09-10

    Prominences in the solar corona are a hundredfold cooler and denser than their surroundings, with a total mass of 10{sup 13} up to 10{sup 15} g. Here, we report on the first comprehensive simulations of three-dimensional, thermally and gravitationally stratified magnetic flux ropes where in situ condensation to a prominence occurs due to radiative losses. After a gradual thermodynamic adjustment, we witness a phase where runaway cooling occurs while counter-streaming shearing flows drain off mass along helical field lines. After this drainage, a prominence-like condensation resides in concave upward field regions, and this prominence retains its overall characteristics for more than two hours. While condensing, the prominence establishes a prominence-corona transition region where magnetic field-aligned thermal conduction is operative during the runaway cooling. The prominence structure represents a force-balanced state in a helical flux rope. The simulated condensation demonstrates a right-bearing barb, as a remnant of the drainage. Synthetic images at extreme ultraviolet wavelengths follow the onset of the condensation, and confirm the appearance of horns and a three-part structure for the stable prominence state, as often seen in erupting prominences. This naturally explains recent Solar Dynamics Observatory views with the Atmospheric Imaging Assembly on prominences in coronal cavities demonstrating horns.

  16. Simulating the in Situ Condensation Process of Solar Prominences

    NASA Astrophysics Data System (ADS)

    Xia, C.; Keppens, R.; Antolin, P.; Porth, O.

    2014-09-01

    Prominences in the solar corona are a hundredfold cooler and denser than their surroundings, with a total mass of 1013 up to 1015 g. Here, we report on the first comprehensive simulations of three-dimensional, thermally and gravitationally stratified magnetic flux ropes where in situ condensation to a prominence occurs due to radiative losses. After a gradual thermodynamic adjustment, we witness a phase where runaway cooling occurs while counter-streaming shearing flows drain off mass along helical field lines. After this drainage, a prominence-like condensation resides in concave upward field regions, and this prominence retains its overall characteristics for more than two hours. While condensing, the prominence establishes a prominence-corona transition region where magnetic field-aligned thermal conduction is operative during the runaway cooling. The prominence structure represents a force-balanced state in a helical flux rope. The simulated condensation demonstrates a right-bearing barb, as a remnant of the drainage. Synthetic images at extreme ultraviolet wavelengths follow the onset of the condensation, and confirm the appearance of horns and a three-part structure for the stable prominence state, as often seen in erupting prominences. This naturally explains recent Solar Dynamics Observatory views with the Atmospheric Imaging Assembly on prominences in coronal cavities demonstrating horns.

  17. The executive prominent/memory prominent spectrum in Alzheimer’s disease is highly heritable

    PubMed Central

    Mez, Jesse; Mukherjee, Shubhabrata; Thornton, Timothy; Fardo, David W.; Trittschuh, Emily; Sutti, Sheila; Sherva, Richard; Kauwe, John S.; Naj, Adam C.; Beecham, Gary W.; Gross, Alden; Saykin, Andrew J.; Green, Robert C.; Crane, Paul K.

    2016-01-01

    Late-onset Alzheimer’s disease (LOAD) can present heterogeneously, with several subtypes recognized, including dysexecutive AD. One way to identify people with dysexecutive AD is to consider the difference between memory and executive functioning, which we refer to as the executive prominent/memory prominent spectrum. We aimed to determine if this spectrum was heritable. We used neuropsychological and genetic data from people with mild LOAD (Clinical Dementia Rating 0.5 or 1.0) from the National Alzheimer’s Coordinating Center and the Alzheimer’s Disease Neuroimaging Initiative. We cocalibrated the neuropsychological data to obtain executive functioning and memory scores and used their difference as a continuous phenotype to calculate its heritability overall and by chromosome. Narrow-sense heritability of the difference between memory and executive functioning scores was 0.68 (standard error 0.12). Single nucleotide polymorphisms on chromosomes 1, 2, 4, 11, 12, and 18 explained the largest fraction of phenotypic variance, with signals from each chromosome accounting for 5%–7%. The chromosomal pattern of heritability differed substantially from that of LOAD itself. PMID:27103524

  18. The executive prominent/memory prominent spectrum in Alzheimer's disease is highly heritable.

    PubMed

    Mez, Jesse; Mukherjee, Shubhabrata; Thornton, Timothy; Fardo, David W; Trittschuh, Emily; Sutti, Sheila; Sherva, Richard; Kauwe, John S; Naj, Adam C; Beecham, Gary W; Gross, Alden; Saykin, Andrew J; Green, Robert C; Crane, Paul K

    2016-05-01

    Late-onset Alzheimer's disease (LOAD) can present heterogeneously, with several subtypes recognized, including dysexecutive AD. One way to identify people with dysexecutive AD is to consider the difference between memory and executive functioning, which we refer to as the executive prominent/memory prominent spectrum. We aimed to determine if this spectrum was heritable. We used neuropsychological and genetic data from people with mild LOAD (Clinical Dementia Rating 0.5 or 1.0) from the National Alzheimer's Coordinating Center and the Alzheimer's Disease Neuroimaging Initiative. We cocalibrated the neuropsychological data to obtain executive functioning and memory scores and used their difference as a continuous phenotype to calculate its heritability overall and by chromosome. Narrow-sense heritability of the difference between memory and executive functioning scores was 0.68 (standard error 0.12). Single nucleotide polymorphisms on chromosomes 1, 2, 4, 11, 12, and 18 explained the largest fraction of phenotypic variance, with signals from each chromosome accounting for 5%-7%. The chromosomal pattern of heritability differed substantially from that of LOAD itself. PMID:27103524

  19. Formation of active region and quiescent prominence magnetic field configurations

    NASA Technical Reports Server (NTRS)

    An, C.-H.; Bao, J. J.; Wu, S. T.

    1986-01-01

    To investigate the formation of prominences, researchers studied chromospheric mass injection into an overlying coronal dipole magnetic field using a 2-D ideal magnetohydrodynamic (MHD) numerical model. Researchers propose that active region prominences are formed by chromospheric plasmas injected directly into the overlying coronal magnetic field and that quiescent prominences are formed by plasmas evaporated at the interface between spicules and corona. Hence, for the simulation of an active region prominence magnetic field we inject the mass from one side, but use a symmetric mass injection to form a quiescent prominence field configuration. Researchers try to find optimum conditions for the formation of Kippenhahn-Schuluter(K-S)type field configuration for stable support of the injection plasmas. They find that the formation of K-S type field configuration by mass injection requires a delicate balance between injection velocity, density, and overlying magnetic fields. These results may explain why a prominence does not form on every neutral line.

  20. Neutral Atom Diffusion in a Partially Ionized Prominence Plasma

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly

    2010-01-01

    The support of solar prominences is normally described in terms of a magnetic force on the prominence plasma that balances the solar gravitational force. Because the prominence plasma is only partially ionized. it is necessary to consider in addition the support of the neutral component of the prominence plasma. This support is accomplished through a frictional interaction between the neutral and ionized components of the plasma, and its efficacy depends strongly on the degree of ionization of the plasma. More specifically, the frictional force is proportional to the relative flow of neutral and ion species, and for a sufficiently weakly ionized plasma, this flow must be relatively large to produce a frictional force that balances gravity. A large relative flow, of course, implies significant draining of neutral particles from the prominence. We evaluate the importance of this draining effect for a hydrogen-helium plasma, and consider the observational evidence for cross-field diffusion of neutral prominence material,

  1. Prominence Energetics Measured with SOHO/SUMER and TRACE

    NASA Technical Reports Server (NTRS)

    Kucera, T.; Landi, E.

    2004-01-01

    The mechanisms by which solar prominences are filled with plasma are still undetermined. In this study we perform a quantitative analysis of the thermal properties of moving features in prominences in order to put constraints on models of prominence formation and dynamics. In order to make such measurements of the quickly moving features seen in prominences in the W we use the SOHO/SUMER spectrograph to take a time series of exposures from a single pointing position, providing a measurement of spectral line properties as a function of time and position along the slit. temperatures from 80,000 - 1.6 million K. These measurements are combined with TRACE movies in transition region and coronal temperature bands to obtain more complete information concerning prominence structure and motions. The resulting observations allow us to analyze the thermal and kinetic energy of the moving prominence sources as functions of time.

  2. Coronal transient--eruptive prominence of 1980 August 5

    SciTech Connect

    Fisher, R.; Garcia, C.J.; Seagraves, P.

    1981-06-15

    A coronal transient was observed in association with an eruptive prominence event using the Mauna Loa experiment system. The transient, a rarefaction, formed before the acceleration of the eruptive prominence. Upward velocities of various features, as seen in the plane of the sky, show a marked difference as a function of time between the transient and the eruptive prominence. A region of enhanced electron density formed slowly in front of the rarefaction.

  3. The variations of prominence activities during solar cycle

    NASA Astrophysics Data System (ADS)

    Shimojo, Masumi

    The prominence activities (prominence eruption/disappearance) in the solar atmosphere closely relate with the CMEs that cause great influences on heliosphere and magnetosphere. Gopal-swarmy et al. (2003) reported that 72 The Nobeyama Radioheliograph (NoRH) is observing Sun in microwave (17 GHz) since 1992. At a flare, the main component of the microwave from Sun is emitted from non-thermal electrons that are accelerated by flare. On the other hand, the main component of the microwave is thermal emission when Sun is quiet, and a prominence is clearly observed in microwave because there is the prominence on the limb. We developed the automatic prominence activity detection program based on 17 GHz images observed by NoRH, and investigated the variation of the properties of the prominence activities that oc-curred from 1992 to the end of 2009. We found the following results. 1. The variation in the number of prominence activities is similar to that of sunspots during one solar cycle but there are differences between the peak times of prominence activities and sunspots. 2. The frequency distribution as a function of the magnitude of the prominence activities the size of activated prominences at each phase shows a power-law distribution. The power-law index of the distribution does not change except around the solar minimum. 3. The number of promi-nence activities has a dependence on the latitude On the other hand the average magnitude is independent of the latitude. In the paper, we will also discuss the relationship the other properties of prominence eruptions, solar cycle and the photospheric magnetic field.

  4. Old and New Aspects of Prominence Physics from Coronal Observations

    NASA Astrophysics Data System (ADS)

    Koutchmy, S.; Filippov, B.; Lamy, P.

    2007-05-01

    Classical W-L eclipse observations at typical spatial resolution of 10 arcsec show dark cavities surrounding prominences. Images at higher spatial resolution processed with a spatial filter reveal small dynamical cool clouds moving inside the inner corona around prominences. More recently EIT/SoHO observations taken using the 304 Å channel showed He+ prominences sometimes not seen in cooler lines. TRACE movies of the Fe IX and XI emissions where prominences are seen in absorption also bring appreciable informations on the dynamical surrounding of prominences, without showing obvious correlations between prominence and coronal structures. Accordingly, we re-examine the significance of the cavity and propose a possible interpretation as magnetic interlaced 3-D flux ropes and loops evacuating the corona, in addition to twisted flux ropes where the prominence plasma is condensing. Future space missions like ASPIICS should pay more attention to cavities and emptiness, to coronal dynamics around prominences, in order to resolve the long-standing problem of the origin of prominences and perhaps, perform a new diagnostic of the erupting process responsible for many CMEs.

  5. Internal Dynamics of a Twin-layer Solar Prominence

    NASA Astrophysics Data System (ADS)

    Xia, C.; Keppens, R.

    2016-07-01

    Modern observations revealed rich dynamics within solar prominences. The globally stable quiescent prominences, characterized by the presence of thin vertical threads and falling knobs, are frequently invaded by small rising dark plumes. These dynamic phenomena are related to magnetic Rayleigh–Taylor instability, since prominence matter, 100 times denser than surrounding coronal plasma, is lifted against gravity by weak magnetic field. To get a deeper understanding of the physics behind these phenomena, we use three-dimensional magnetohydrodynamic simulations to investigate the nonlinear magnetoconvective motions in a twin-layer prominence in a macroscopic model from chromospheric layers up to 30 Mm height. The properties of simulated falling “fingers” and uprising bubbles are consistent with those in observed vertical threads and rising plumes in quiescent prominences. Both sheets of the twin-layer prominence show a strongly coherent evolution due to their magnetic connectivity, and demonstrate collective kink deformation. Our model suggests that the vertical threads of the prominence as seen in an edge-on view, and the apparent horizontal threads of the filament when seen top-down are different appearances of the same structures. Synthetic images of the modeled twin-layer prominence reflect the strong degree of mixing established over the entire prominence structure, in agreement with the observations.

  6. Prominence in triconstituent compounds: pitch contours and linguistic theory.

    PubMed

    Kösling, Kristina; Kunter, Gero; Baayen, Harald; Plag, Ingo

    2013-12-01

    According to the widely accepted Lexical Category Prominence Rule (LCPR), prominence assignment to triconstituent compounds depends on the branching direction. Left-branching compounds, that is, compounds with a left-hand complex constituent, are held to have highest prominence on the left-most constituent, whereas right-branching compounds have highest prominence on the second of the three constituents. The LCPR is, however, only poorly empirically supported. The present paper tests a new hypothesis concerning the prominence of triconstituent compounds and suggests a new methodology for the empirical investigation of compound prominence. According to this hypothesis, the prominence pattern of the embedded compound has a decisive influence on the prominence of the whole compound. Using a mixed-effects generalized additive model for the analysis of the pitch movements, it is shown that all triconstituent compounds have an accent on the first constituent irrespective of branching, and that the placement of a second, or even a third, accent is dependent on the prominence pattern of the embedded compound. The LCPR is wrong. PMID:24597276

  7. Nonlinear dynamic-based analysis of severe dysphonia in patients with vocal fold scar and sulcus vocalis

    PubMed Central

    Choi, Seong Hee; Zhang, Yu; Jiang, Jack J.; Bless, Diane M.; Welham, Nathan V.

    2011-01-01

    Objective The primary goal of this study was to evaluate a nonlinear dynamic approach to the acoustic analysis of dysphonia associated with vocal fold scar and sulcus vocalis. Study Design Case-control study. Methods Acoustic voice samples from scar/sulcus patients and age/sex-matched controls were analyzed using correlation dimension (D2) and phase plots, time-domain based perturbation indices (jitter, shimmer, signal-to-noise ratio [SNR]), and an auditory-perceptual rating scheme. Signal typing was performed to identify samples with bifurcations and aperiodicity. Results Type 2 and 3 acoustic signals were highly represented in the scar/sulcus patient group. When data were analyzed irrespective of signal type, all perceptual and acoustic indices successfully distinguished scar/sulcus patients from controls. Removal of type 2 and 3 signals eliminated the previously identified differences between experimental groups for all acoustic indices except D2. The strongest perceptual-acoustic correlation in our dataset was observed for SNR; the weakest correlation was observed for D2. Conclusions These findings suggest that D2 is inferior to time-domain based perturbation measures for the analysis of dysphonia associated with scar/sulcus; however, time-domain based algorithms are inherently susceptible to inflation under highly aperiodic (i.e., type 2 and 3) signal conditions. Auditory-perceptual analysis, unhindered by signal aperiodicity, is therefore a robust strategy for distinguishing scar/sulcus patient voices from normal voices. Future acoustic analysis research in this area should consider alternative (e.g., frequency- and quefrency-domain based) measures alongside additional nonlinear approaches. PMID:22516315

  8. Prominent Feature Analysis: What It Means for the Classroom

    ERIC Educational Resources Information Center

    Swain, Sherry Seale; Graves, Richard L.; Morse, David T.

    2010-01-01

    The purpose of a prominent feature analysis is to describe the stylistic flexibility that a young writer, or a group of young writers, exhibits on a given day, with a given prompt. In prominent feature analysis, there are no guidebooks, no rubrics--just student papers and the expertise of teachers. Teachers come to the papers individually and yet…

  9. 21 CFR 101.15 - Food; prominence of required statements.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 21 Food and Drugs 2 2014-04-01 2014-04-01 false Food; prominence of required statements. 101.15 Section 101.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) FOOD FOR HUMAN CONSUMPTION FOOD LABELING General Provisions § 101.15 Food; prominence of...

  10. 21 CFR 101.15 - Food; prominence of required statements.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 21 Food and Drugs 2 2012-04-01 2012-04-01 false Food; prominence of required statements. 101.15 Section 101.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) FOOD FOR HUMAN CONSUMPTION FOOD LABELING General Provisions § 101.15 Food; prominence of...

  11. 21 CFR 101.15 - Food; prominence of required statements.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 21 Food and Drugs 2 2013-04-01 2013-04-01 false Food; prominence of required statements. 101.15 Section 101.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) FOOD FOR HUMAN CONSUMPTION FOOD LABELING General Provisions § 101.15 Food; prominence of required statements. (a) A word, statement,...

  12. A prominence eruption driven by flux feeding from chromospheric fibrils

    SciTech Connect

    Zhang, Quanhao; Liu, Rui; Wang, Yuming; Shen, Chenglong; Liu, Kai; Liu, Jiajia; Wang, S.

    2014-07-10

    We present multi-wavelength observations of a prominence eruption originating from a quadrupolar field configuration, in which the prominence was embedded in a side arcade. Within the two-day period prior to its eruption on 2012 October 22, the prominence was perturbed three times by chromospheric fibrils underneath, which rose upward, became brightened, and merged into the prominence, resulting in horizontal flows along the prominence axis, suggesting that the fluxes carried by the fibrils were incorporated into the magnetic field of the prominence. These perturbations caused the prominence to oscillate and to rise faster than before. The absence of intense heating within the first two hours after the onset of the prominence eruption, which followed an exponential increase in height, indicates that ideal instability played a crucial role. The eruption involved interactions with the other side arcade, leading up to a twin coronal mass ejection, which was accompanied by transient surface brightenings in the central arcade, followed by transient dimmings and brightenings in the two side arcades. We suggest that flux feeding from chromospheric fibrils might be an important mechanism to trigger coronal eruptions.

  13. On Common Ground: Prominent Women Talk about Work & Family.

    ERIC Educational Resources Information Center

    Zuckerman, Diana, Ed.

    This publication presents interviews with 11 prominent women, representing different backgrounds, philosophies, and life experiences, in which they speak about their own experiences with work and family issues. The introduction, "On Common Ground: Prominent Women Talk about Work & Family" (Diana Zuckerman), provides an overview. The 11 interviews…

  14. [Spasmodic torticollis, substantiating Manto syndrome, of possible toxic aethiology, with alterations of brainstem acoustic evoked potentials (BAEPs). Treatment with L-5-hydroxytryptophan. Follow up of 18 months, during which high degree resolution of symptoms and normalization of BAEPs took place].

    PubMed

    Disertori, B; Ducati, A; Piazza, M

    1982-01-01

    A case of very severe spasmodic torticollis observed for 18 months is presented and discussed. Head was so rotated that permitted only backward seeing and compressed brachial plexus between scaleni muscles with sensory, motor and trophic troubles in the hand. A toxic aethiology from parathion is likely. Brainstem Acoustic Evoked Potentials (BAEPs) showed in the beginning abnormal responses, especially as refers to waves originating in the mesencephalon. Therapy with L-5-hydroxytryptophan subdued neurological symptoms; a parallel normalization of BAEPs recording was observed. The Authors propose to call this syndrome (spasmodic torticollis with thoracic outlet syndrome) after the mythical diviner Manto, which Dante Alighieri refers to in his "Divina Commedia" (Inferno, XX, 55 e segg.). PMID:6985243

  15. Thermal Properties of Prominence Motions as Observed in the UV

    NASA Technical Reports Server (NTRS)

    Kucera, T.; Landi, E.

    2003-01-01

    The mechanisms by which solar prominences are filled with plasma are still undetermined. In this study we perform a quantitative analysis of the thermal properties of moving features in prominences in order to put constraints on models of prominence formation and dynamics. In order to make such measurements of quickly moving features seen in prominences in the UV we use the SOHO instruments SUMER and CDS to take a time series of exposures at a single pointing position, providing a measurement of spectral line properties as a function of time and position along the slit. The resulting observations in spectral lines in a range of 'transition region' temperatures allow us to analyze the thermal properties of the moving prominence sources as a function of time.

  16. Magnetic Field in Atypical Prominence Structures: Bubble, Tornado, and Eruption

    NASA Astrophysics Data System (ADS)

    Levens, P. J.; Schmieder, B.; López Ariste, A.; Labrosse, N.; Dalmasse, K.; Gelly, B.

    2016-08-01

    Spectropolarimetric observations of prominences have been obtained with the THEMIS telescope during four years of coordinated campaigns. Our aim is now to understand the conditions of the cool plasma and magnetism in “atypical” prominences, namely when the measured inclination of the magnetic field departs, to some extent, from the predominantly horizontal field found in “typical” prominences. What is the role of the magnetic field in these prominence types? Are plasma dynamics more important in these cases than the magnetic support? We focus our study on three types of “atypical” prominences (tornadoes, bubbles, and jet-like prominence eruptions) that have all been observed by THEMIS in the He i D3 line, from which the Stokes parameters can be derived. The magnetic field strength, inclination, and azimuth in each pixel are obtained by using the inversion method of principal component analysis on a model of single scattering in the presence of the Hanle effect. The magnetic field in tornadoes is found to be more or less horizontal, whereas for the eruptive prominence it is mostly vertical. We estimate a tendency toward higher values of magnetic field strength inside the bubbles than outside in the surrounding prominence. In all of the models in our database, only one magnetic field orientation is considered for each pixel. While sufficient for most of the main prominence body, this assumption appears to be oversimplified in atypical prominence structures. We should consider these observations as the result of superposition of multiple magnetic fields, possibly even with a turbulent field component.

  17. Back-and-Forth Methodology for Objective Voice Quality Assessment: From/to Expert Knowledge to/from Automatic Classification of Dysphonia

    NASA Astrophysics Data System (ADS)

    Fredouille, Corinne; Pouchoulin, Gilles; Ghio, Alain; Revis, Joana; Bonastre, Jean-François; Giovanni, Antoine

    2009-12-01

    This paper addresses voice disorder assessment. It proposes an original back-and-forth methodology involving an automatic classification system as well as knowledge of the human experts (machine learning experts, phoneticians, and pathologists). The goal of this methodology is to bring a better understanding of acoustic phenomena related to dysphonia. The automatic system was validated on a dysphonic corpus (80 female voices), rated according to the GRBAS perceptual scale by an expert jury. Firstly, focused on the frequency domain, the classification system showed the interest of 0-3000 Hz frequency band for the classification task based on the GRBAS scale. Later, an automatic phonemic analysis underlined the significance of consonants and more surprisingly of unvoiced consonants for the same classification task. Submitted to the human experts, these observations led to a manual analysis of unvoiced plosives, which highlighted a lengthening of VOT according to the dysphonia severity validated by a preliminary statistical analysis.

  18. Topic-Prominence and Subject-Prominence in L2 Acquisition: Evidence of English-to-Chinese Typological Transfer.

    ERIC Educational Resources Information Center

    Jin, Hong Gang

    1994-01-01

    Investigated whether topic-prominence transfer is a universal developmental stage or a transferable typology by analyzing the behavior of 46 native speakers of English learning Chinese, a subject-prominence (SP) language, as a second language. Results found that the learners displayed a process of systematically transferring English SP features to…

  19. Mass composition and dynamics in quiet sun prominences

    NASA Astrophysics Data System (ADS)

    Kilper, Gary K.

    2009-06-01

    Solar prominences are transient phenomena in the solar atmosphere that display highly dynamic activity and can result in dramatic eruptions, ejecting a large amount of material into the heliosphere. The dynamics of the prominence plasma reveal information about its interaction with the magnetic field of the prominence, while the eruptions are associated with coronal mass ejections, which greatly affect space weather near Earth and throughout the solar system. My research on these topics was conducted via observational analyses of the partially-ionized prominence material, its composition, and the dynamics over time in prominences that range in activity from quiescent to highly active. The main results are evidence that (1) in quiescent prominences, neutral He is located more in the lower part of the structure, (2) a higher level of activity in prominences is related to a mixing of the material, and (3) an extended period of high activity and mixing occurs prior to eruptions, possibly due to mass loading. In addition, innovative modifications to analytical techniques led to measurements of the material's mass, composition, and small-scale dynamics.

  20. Synthetic differential emission measure curves of prominence fine structures. II. The SoHO/SUMER prominence of 8 June 2004

    NASA Astrophysics Data System (ADS)

    Gunár, S.; Parenti, S.; Anzer, U.; Heinzel, P.; Vial, J.-C.

    2011-11-01

    Aims: This study is the first attempt to combine the prominence observations in Lyman, UV, and EUV lines with the determination of the prominence differential emission measure derived using two different techniques, one based on the inversion of the observed UV and EUV lines and the other employing 2D non-LTE prominence fine-structure modeling of the Lyman spectra. Methods: We use a trial-and-error method to derive the 2D multi-thread prominence fine-structure model producing synthetic Lyman spectra in good agreement with the observations. We then employ a numerical method to perform the forward determination of the DEM from 2D multi-thread models and compare the synthetic DEM curves with those derived from observations using inversion techniques. Results: A set of available observations of the June 8, 2004 prominence allows us to determine the range of input parameters, which contains models producing synthetic Lyman spectra in good agreement with the observations. We select three models, which represent this parametric-space area well and compute the synthetic DEM curves for multi-thread realizations of these models. The synthetic DEM curves of selected models are in good agreement with the DEM curves derived from the observations. Conclusions: We show that the evaluation of the prominence fine-structure DEM complements the analysis of the prominence hydrogen Lyman spectra and that its combination with the detailed radiative-transfer modeling of prominence fine structures provides a useful tool for investigating the prominence temperature structure from the cool core to the prominence-corona transition region.

  1. Prominence and Control: The Weighted Rich-Club Effect

    NASA Astrophysics Data System (ADS)

    Opsahl, Tore; Colizza, Vittoria; Panzarasa, Pietro; Ramasco, José J.

    2008-10-01

    Complex systems are often characterized by large-scale hierarchical organizations. Whether the prominent elements, at the top of the hierarchy, share and control resources or avoid one another lies at the heart of a system’s global organization and functioning. Inspired by network perspectives, we propose a new general framework for studying the tendency of prominent elements to form clubs with exclusive control over the majority of a system’s resources. We explore associations between prominence and control in the fields of transportation, scientific collaboration, and online communication.

  2. Prominence condensation and magnetic levitation in a coronal loop

    NASA Technical Reports Server (NTRS)

    Van Hoven, G.; Mok, Y.; Drake, J. F.

    1992-01-01

    The results of a model dynamic simulation of the formation and support of a narrow prominence at the apex of a coronal magnetic loop or arcade are described. The condensation process proceeds via an initial radiative cooling and pressure drop, and a secondary siphon flow from the dense chromospheric ends. The antibuoyancy effect as the prominence forms causes a bending of the confining magnetic field, which propagates toward the semirigid ends of the magnetic loop. Thus, a wide magnetic 'hammock' or well (of the normal-polarity Kippenhahn-Schlueter-type) is formed, which supports the prominence at or near the field apex. The simplicity of this 1.5-dimensional model, with its accompanying diagnostics, elucidates the various contributions to the nonlinear dynamics of prominence condensation and levitation.

  3. Mass flows in a prominence spine as observed in EUV

    SciTech Connect

    Kucera, T. A.; Gilbert, H. R.

    2014-07-20

    We analyze a quiescent prominence observed by the Solar Dynamics Observatory's Atmospheric Imaging Assembly (AIA) with a focus on mass and energy flux in the spine, measured using Lyman continuum absorption. This is the first time this type of analysis has been applied with an emphasis on individual features and fluxes in a quiescent prominence. The prominence, observed on 2010 September 28, is detectable in most AIA wavebands in absorption and/or emission. Flows along the spine exhibit horizontal bands 5''-10'' wide and kinetic energy fluxes on the order of a few times 10{sup 5} erg s{sup –1}cm{sup –2}, consistent with quiet sun coronal heating estimates. For a discrete moving feature we estimate a mass of a few times 10{sup 11} g. We discuss the implications of our derived properties for a model of prominence dynamics, the thermal non-equilibrium model.

  4. Prominent dysautonomia in a patient with POEMS syndrome.

    PubMed

    Thakral, Sharda; Issa, Naoum P; Barboi, Alexandru C; Lee, John M

    2016-06-01

    POEMS syndrome is a rare, multisystem disorder characterized by polyneuropathy, organomegaly, endocrinopathy, monoclonal protein, and/or skin changes. Here we present an unusual case of a patient with POEMS syndrome who exhibited a prominent autonomic neuropathy. PMID:27165541

  5. Obscuration of Flare Emission by an Eruptive Prominence

    NASA Technical Reports Server (NTRS)

    Gopalswamy, Nat; Yashiro, Seiji

    2013-01-01

    We report on the eclipsing of microwave flare emission by an eruptive prominence from a neighboring region as observed by the Nobeyama Radioheliograph at 17 GHz. The obscuration of the flare emission appears as a dimming feature in the microwave flare light curve. We use the dimming feature to derive the temperature of the prominence and the distribution of heating along the length of the filament. We find that the prominence is heated to a temperature above the quiet Sun temperature at 17 GHz. The duration of the dimming is the time taken by the eruptive prominence in passing over the flaring region. We also find evidence for the obscuration in EUV images obtained by the Solar and Heliospheric Observatory (SOHO) mission.

  6. Solar Prominence Eruption Marks 1 Million on Helioviewer

    NASA Video Gallery

    This movie of a prominence eruption on April 20, 2013, was the millionth movie made on Helioviewer.org. The wispy eruption seen here eventually blossomed into a much larger cloud of solar material,...

  7. Repetition is easy: Why repeated referents have reduced prominence

    PubMed Central

    Lam, Tuan Q.; Watson, Duane G.

    2011-01-01

    The repetition and predictability of a word in a conversation are two factors that are believed to affect whether or not it is emphasized: predictable, repeated words are less acoustically prominent than unpredictable, new words. However, because predictability and repetition are correlated, it is unclear whether speakers lengthen unpredictable words to facilitate comprehension or whether this lengthening is the result of difficulties in accessing a new (non-repeated) lexical item. In this paper, we investigate the relationship between acoustic prominence, repetition, and predictability in a description task. In Experiment 1, we find that repeated referents are produced with reduced prominence, even when these referents are unexpected. In Experiment 2, we find that predictability and repetition both have independent effects on duration and intensity. However, word duration was primarily determined by repetition, and intensity was primarily determined by predictability. The data are most consistent with an account in which multiple cognitive factors influence the acoustic prominence of a word. PMID:21156876

  8. Observation of Low Level Heating in an Erupting Prominence

    NASA Technical Reports Server (NTRS)

    Kucera, Therese A.

    2007-01-01

    We present multi-wavelength observations of low level heating in an erupting prominence observed in the UV and EUV over a wide range of temperatures and wavelengths by SOHO's SUMER instrument, TRACE and also in H-alpha by the Yunnan Astronomical Observatory. The eruption occurred on 2004 April 30. The heating is relatively mild, leading only to the ionization of neutral hydrogen and probably helium. It is also localized, occurring along the bottom edge of the erupting prominence and in a kink-like feature in the prominence. The heating is revealed as a decrease in the Lyman absorption. This decrease results in an apparent increase in emission in all the lines observed by SUMER, especially those formed at temperatures -1 0A5. However, this is due to the disappearance of cooler absorbing material in the prominence rather than an increase in these higher temperature species.

  9. Observation of Low Level Heating in an Erupting Prominence

    NASA Technical Reports Server (NTRS)

    Kucera, Theresa; Landi, E.

    2007-01-01

    We present multi-wavelength observations of low level heating in an erupting prominence observed in the UV and EUV over a wide range of temperatures and wavelengths by SOHO's SUMER instrument, TRACE and also in H-alpha by the Yunnan Astronomical Observatory. The eruption occurred on 2004 April 30. The heating is relatively mild, leading only to the ionization of neutral hydrogen and probably helium. It is also localized, occurring along the bottom edge of the erupting prominence and in a kink-like feature in the prominence. The heating is revealed as a decrease in the Lyman absorption. This decrease results in an apparent increase in emission in all the lines observed by SUMER, especially those formed at temperatures approx. 10(exp 5). However, this is due to the disappearance of cooler absorbing material in the prominence rather than an increase in these higher temperature species.

  10. Hinode and IRIS Observations of a Prominence-Cavity System

    NASA Astrophysics Data System (ADS)

    Jibben, Patricia R.; Reeves, Kathy; Su, Yingna

    2016-05-01

    Long-lived solar prominences often have a coronal cavity enclosing the prominence. Within the cavity, hot X-ray emission can persist above the prominence and in the central regions of the cavity. We present the results of an Interface Region Imaging Spectrograph (IRIS) and Hinode coordinated Observation Program (IHOP 264) study of a prominence-cavity system. The X-ray Telescope (XRT) observes an inflow of bright X-ray emission that strikes and envelops the prominence-cavity system causing an eruption of chromospheric plasma near the base of the prominence. During and after the eruption, an increase in X-ray emission forms within the cavity and above the prominence. IRIS and the EUV Imaging Spectrometer (EIS) observe strong blue shifts in both chromosphere and coronal lines during the eruption. The Solar Optical Telescope (SOT) Ca II H-line data show bright emission along the eruption path with complex turbulent plasma motions. The IRIS Si IV 1394 Angstrom spectra along the on-disk portion of the prominence show a region of decreased emission near the base of the prominence, suggesting a magnetic field bald-patch topology along the Polarity Inversion Line (PIL). Combined, these observations imply a cylindrical flux rope best represents the prominence-cavity system. A model of the magnetic structure of the prominence-cavity system comprised of a weakly twisted flux rope can explain the observed loops in the X-ray and EUV data. Observations from the Coronal Multichannel Polarimeter (CoMP) are compared to predicted models and are inconclusive. We find that more sensitive measurements of the magnetic field strength along the line-of-sight are needed to verify this configuration.Patricia Jibben and Kathy Reeves are supported by under contract 80111112705 from Lockheed-Martin to SAO, contract NNM07AB07C from NASA to SAO, grant number NNX12AI30G from NASA to SAO, and contract Z15-12504 from HAO to SAO under a grant from AFOSR. Yingna Su is supported by the Youth Fund of

  11. An Acoustic Measure for Word Prominence in Spontaneous Speech

    PubMed Central

    Wang, Dagen; Narayanan, Shrikanth

    2010-01-01

    An algorithm for automatic speech prominence detection is reported in this paper. We describe a comparative analysis on various acoustic features for word prominence detection and report results using a spoken dialog corpus with manually assigned prominence labels. The focus is on features such as spectral intensity and speech rate that are directly extracted from speech based on a correlation-based approach without requiring explicit linguistic or phonetic knowledge. Additionally, various pitch-based measures are studied with respect to their discriminating ability for prominence detection. A parametric scheme for modeling pitch plateau is proposed and this feature alone is found to outperform the traditional local pitch statistics. Two sets of experiments are used to explore the usefulness of the acoustic score generated using these features. The first set focuses on a more traditional way of word prominence detection based on a manually-tagged corpus. A 76.8% classification accuracy was achieved on a corpus of role-playing spoken dialogs. Due to difficulties in manually tagging speech prominence into discrete levels (categories), the second set of experiments focuses on evaluating the score indirectly. Specifically, through experiments on the Switchboard corpus, it is shown that the proposed acoustic score can discriminate between content word and function words in a statistically significant way. The relation between speech prominence and content/function words is also explored. Since prominent words tend to be predominantly content words, and since content words can be automatically marked from text-derived part of speech (POS) information, it is shown that the proposed acoustic score can be indirectly cross-validated through POS information. PMID:20454538

  12. A STATISTICAL STUDY OF TRANSVERSE OSCILLATIONS IN A QUIESCENT PROMINENCE

    SciTech Connect

    Hillier, A.; Morton, R. J.; Erdélyi, R.

    2013-12-20

    The launch of the Hinode satellite has allowed for seeing-free observations at high-resolution and high-cadence making it well suited to study the dynamics of quiescent prominences. In recent years it has become clear that quiescent prominences support small-amplitude transverse oscillations, however, sample sizes are usually too small for general conclusions to be drawn. We remedy this by providing a statistical study of transverse oscillations in vertical prominence threads. Over a 4 hr period of observations it was possible to measure the properties of 3436 waves, finding periods from 50 to 6000 s with typical velocity amplitudes ranging between 0.2 and 23 km s{sup –1}. The large number of observed waves allows the determination of the frequency dependence of the wave properties and derivation of the velocity power spectrum for the transverse waves. For frequencies less than 7 mHz, the frequency dependence of the velocity power is consistent with the velocity power spectra generated from observations of the horizontal motions of magnetic elements in the photosphere, suggesting that the prominence transverse waves are driven by photospheric motions. However, at higher frequencies the two distributions significantly diverge, with relatively more power found at higher frequencies in the prominence oscillations. These results highlight that waves over a large frequency range are ubiquitous in prominences, and that a significant amount of the wave energy is found at higher frequency.

  13. Cross-linguistic evidence for gender as a prominence feature.

    PubMed

    Esaulova, Yulia; von Stockhausen, Lisa

    2015-01-01

    This paper discusses recent findings in the online sentence processing research that suggest to consider gender information a prominence feature. Prominence features are hierarchically ordered information types that interact with formal features of arguments (e.g., grammatical functions, thematic roles) and thus determine the readers' ability to efficiently interpret linguistic ambiguities. While previous research addressed a number of prominence features (e.g., animacy, definiteness, person), there is now first empirical evidence indicating that gender information also influences the assignment of thematic roles across languages. Grammatically masculine role nouns are processed faster as agents than patients compared to feminine ones. Stereotypically male role nouns (e.g., electrician) are integrated with an agent role easier than neutral ones (e.g., musician), which in turn are integrated easier than female ones (e.g., beautician). Conceptualizing gender as a prominence feature will not only expand our knowledge about information types relevant for online comprehension but also uncover subtle gender biases present in language. The present work explores the possibility for a theoretical integration of social psychological and psycholinguistic research focusing on gender with research on prominence. Potential advantages an interdisciplinary approach to the study of gender as a prominence feature, open questions and future directions are discussed. PMID:26441732

  14. Cross-linguistic evidence for gender as a prominence feature

    PubMed Central

    Esaulova, Yulia; von Stockhausen, Lisa

    2015-01-01

    This paper discusses recent findings in the online sentence processing research that suggest to consider gender information a prominence feature. Prominence features are hierarchically ordered information types that interact with formal features of arguments (e.g., grammatical functions, thematic roles) and thus determine the readers’ ability to efficiently interpret linguistic ambiguities. While previous research addressed a number of prominence features (e.g., animacy, definiteness, person), there is now first empirical evidence indicating that gender information also influences the assignment of thematic roles across languages. Grammatically masculine role nouns are processed faster as agents than patients compared to feminine ones. Stereotypically male role nouns (e.g., electrician) are integrated with an agent role easier than neutral ones (e.g., musician), which in turn are integrated easier than female ones (e.g., beautician). Conceptualizing gender as a prominence feature will not only expand our knowledge about information types relevant for online comprehension but also uncover subtle gender biases present in language. The present work explores the possibility for a theoretical integration of social psychological and psycholinguistic research focusing on gender with research on prominence. Potential advantages an interdisciplinary approach to the study of gender as a prominence feature, open questions and future directions are discussed. PMID:26441732

  15. On the Asymmetric Longitudinal Oscillations of a Pikelner's Model Prominence

    NASA Astrophysics Data System (ADS)

    Kraśkiewicz, J.; Murawski, K.; Solov'ev, A.; Srivastava, A. K.

    2016-02-01

    We present analytical and numerical models of a normal-polarity quiescent prominence that are based on the model of Pikelner (Solar Phys. 17, 44, 1971). We derive the general analytical expressions for the two-dimensional (2D) equilibrium plasma quantities such as the mass density and gas pressure, and we specify magnetic-field components for the prominence, which corresponds to a dense and cold plasma residing in the dip of curved magnetic-field lines. Adapting of these expressions, we numerically solve the 2D, nonlinear, ideal MHD equations for the Pikelner model of a prominence that is initially perturbed by reducing the gas pressure at the dip of magnetic-field lines. Our findings reveal that as a result of pressure perturbations, the prominence plasma starts evolving in time. This leads to antisymmetric magnetoacoustic-gravity oscillations and to the mass-density growth at the magnetic dip, and the magnetic-field lines subside there. This growth depends on the depth of the magnetic dip. For a shallower dip, less plasma is condensed, and vice versa. We conjecture that the observed long-period magnetoacoustic-gravity oscillations in various prominence systems are in general the consequence of the internal-pressure perturbations of the plasma residing in equilibrium at the prominence dip.

  16. Spectral Analysis of Velocities in Quiescent Prominences Observed with Hinode

    NASA Astrophysics Data System (ADS)

    McKenzie, David; Freed, Michael

    2015-04-01

    High-resolution observations of solar prominences, especially with the Solar Optical Telescope (SOT) on Hinode, reveal the presence of upward and downward flows consistent with convection, at length scales that were not accessible with previous telescopes. Since prominences are magnetic structures, the strength and arrangement of their magnetic fields are crucial for determining whether a given prominence will erupt into a coronal mass ejection. Convective flows can twist and tangle those magnetic fields. However, the magnetic fields within the prominences are extremely difficult to measure; therefore measurements of the dynamics of the magnetized plasma in prominences, and the balance between magnetic and gas-pressure forces, are valuable for understanding how these apparently stable structures can evolve to become suddenly eruptive. We will show our findings from analysis of the dynamics in a few solar prominences using local correlation tracking, and make estimates of the kinetic energy, diffusivity, and vorticity.This work is supported by NASA under contract NNM07AB07C with the Smithsonian Astrophysical Observatory.

  17. Botulinum toxin injection - larynx

    MedlinePlus

    Injection laryngoplasty; Botox-larynx: spasmodic dysphonia-BTX; Essential voice tremor (EVT)-btx; Glottic insufficiency; Percutaneous electromyography-guided botulinum toxin treatment; Percutaneous indirect laryngoscopy-guided botulinum toxin Treatment; ...

  18. Use of Botulinum Neurotoxin for the Treatment of Movement Disorders

    MedlinePlus

    ... spasmodic dysphonia, or ABSD). Does BoNT control motor tics? Tics associated with Tourette syndrome are relatively brief, intermittent movements (also known as motor tics) or sounds (also known as vocal or phonic ...

  19. Two Categories of Apparent Tornado-like Prominences

    NASA Astrophysics Data System (ADS)

    Martin, Sara F.; Venkataramanasastry, Aparna

    2014-06-01

    Two categories of solar prominences have been described in the literature as having a pattern of mass motions and/or a shape similar to terrestrial tornados. We first identify the two categories associated with prominences in the historic literature and then show that counterparts do exist for both in recent literature but one has not been called a tornado prominence. One category described as being similar to tornados is associated with the barbs of quiescent filaments but barbs appear to have rotational motion only under special conditions. H alpha Doppler observations from Helio Research confirm that this category is an illusion in our mind’s eye resulting from counterstreaming in the large barbs of quiescent filaments. The second category is a special case of rotational motion occurring during the early stages of some erupting prominences, in recent years called the roll effect in erupting prominences. In these cases, the eruption begins with the sideways rolling of the top of a prominence. As the eruption proceeds the rolling motion propagates down one leg or both legs of an erupting prominence depending on whether the eruption is asymmetric or symmetric respectively. As an asymmetric eruption proceeds, the longer lasting leg becomes nearly vertical and has true rotational motion. If only this phase of the eruption was observed, as in the historic cases, it was called a tornado prominence and spectra recorded in these cases provide proof of the rotational motion. When one observes an entire eruption which exhibits the rolling motion, as accomplished at Helio Research, the similarity to a tornado is lost because the event as a whole has quite a different nature and the analogy to a terrestrial tornado not longer appears suitable or helpful in understanding the observed and deduced physical processes. Our conclusion is that there are no solar prominences with motions that are usefully described as tornado or tornado-like events aside from the fun of observing

  20. SEISMOLOGY OF STANDING KINK OSCILLATIONS OF SOLAR PROMINENCE FINE STRUCTURES

    SciTech Connect

    Soler, R.; Arregui, I.; Oliver, R.; Ballester, J. L.

    2010-10-20

    We investigate standing kink magnetohydrodynamic (MHD) oscillations in a prominence fine structure modeled as a straight and cylindrical magnetic tube only partially filled with the prominence material and with its ends fixed at two rigid walls representing the solar photosphere. The prominence plasma is partially ionized and a transverse inhomogeneous transitional layer is included between the prominence thread and the coronal medium. Thus, ion-neutral collisions and resonant absorption are the damping mechanisms considered. Approximate analytical expressions of the period, the damping time, and their ratio are derived for the fundamental mode in the thin tube and thin boundary approximations. We find that the dominant damping mechanism is resonant absorption, which provides damping ratios in agreement with the observations, whereas ion-neutral collisions are irrelevant for damping. The values of the damping ratio are independent of both the prominence thread length and its position within the magnetic tube, and coincide with the values for a tube fully filled with the prominence plasma. The implications of our results in the context of the MHD seismology technique are discussed, pointing out that the reported short-period (2-10 minutes) and short-wavelength (700-8000 km) thread oscillations may not be consistent with a standing mode interpretation and could be related to propagating waves. Finally, we show that the inversion of some prominence physical parameters, e.g., Alfven speed, magnetic field strength, transverse inhomogeneity length scale, etc., is possible using observationally determined values of the period and damping time of the oscillations along with the analytical approximations of these quantities.

  1. Spectrophotometric determination of some anti-tussive and anti-spasmodic drugs through ion-pair complex formation with thiocyanate and cobalt(II) or molybdenum(V)

    NASA Astrophysics Data System (ADS)

    El-Shiekh, Ragaa; Zahran, Faten; El-Fetouh Gouda, Ayman Abou

    2007-04-01

    Two rapid, simple and sensitive extractive specrophotometric methods has been developed for the determination of anti-tussive drugs, e.g., dextromethorphan hydrobromide (DEX) and pipazethate hydrochloride (PiCl) and anti-spasmodic drugs, e.g., drotaverine hydrochloride (DvCl) and trimebutine maleate (TM) in bulk and in their pharmaceutical formulations. The proposed methods depend upon the reaction of cobalt(II)-thiocyanate (method A) and molybdenum(V)-thiocyanate ions (method B) with the cited drugs to form stable ion-pair complexes which extractable with an n-butnol-dichloromethane solvent mixture (3.5:6.5) and methylene chloride for methods A and B, respectively. The blue and orange red color complexes are determined either colorimetrically at λmax 625 nm (using method A) and 467 or 470 nm for (DEX and PiCl) or (DvCl and TM), respectively (using method B). The concentration range is 20-400 and 2.5-50 μg mL -1 for methods A and B, respectively. The proposed method was successfully applied for the determination of the studied drugs in pure and in pharmaceutical formulations applying the standard additions technique and the results obtained in good agreement well with those obtained by the official method.

  2. Spectrophotometric determination of some anti-tussive and anti-spasmodic drugs through ion-pair complex formation with thiocyanate and cobalt(II) or molybdenum(V).

    PubMed

    El-Shiekh, Ragaa; Zahran, Faten; El-Fetouh Gouda, Ayman Abou

    2007-04-01

    Two rapid, simple and sensitive extractive specrophotometric methods has been developed for the determination of anti-tussive drugs, e.g., dextromethorphan hydrobromide (DEX) and pipazethate hydrochloride (PiCl) and anti-spasmodic drugs, e.g., drotaverine hydrochloride (DvCl) and trimebutine maleate (TM) in bulk and in their pharmaceutical formulations. The proposed methods depend upon the reaction of cobalt(II)-thiocyanate (method A) and molybdenum(V)-thiocyanate ions (method B) with the cited drugs to form stable ion-pair complexes which extractable with an n-butnol-dichloromethane solvent mixture (3.5:6.5) and methylene chloride for methods A and B, respectively. The blue and orange red color complexes are determined either colorimetrically at lambdamax 625 nm (using method A) and 467 or 470 nm for (DEX and PiCl) or (DvCl and TM), respectively (using method B). The concentration range is 20-400 and 2.5-50 microg mL-1 for methods A and B, respectively. The proposed method was successfully applied for the determination of the studied drugs in pure and in pharmaceutical formulations applying the standard additions technique and the results obtained in good agreement well with those obtained by the official method. PMID:17142094

  3. SDO/AIA observations of a partially erupting prominence

    SciTech Connect

    Tripathi, Durgesh; Reeves, Katharine K.; Gibson, Sarah E.; Srivastava, Abhishek; Joshi, Navin C.

    2013-12-01

    We report an observation of a partially erupting prominence and its associated dynamical plasma processes based on observations recorded by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. The prominence first went through a slow rise (SR) phase followed by a fast rise (FR) phase. The SR phase began after a couple of small brightenings were seen toward the footpoints. When the prominence had transitioned from SR to FR, it had already become kinked. The prominence shows strong brightening at the central kink location during the start of FR. We interpret this as an internal magnetic reconnection occurring at a vertical current sheet forming between the two legs of the erupting prominence (flux rope). The brightening at the central kink location is seen in all EUV channels of AIA. The contributions of differential emission at higher temperatures are larger compared to that for typical coronal temperatures supporting a reconnection scenario at the central kink location. The plasma above the brightening location is ejected as a hot plasmoid-like structure embedded in a coronal mass ejection, and those below the brightening move down in the form of blobs moving toward the Sun's surface. The unique time resolution of the AIA has allowed these eruptive aspects, including SR-to-FR, kinking, central current sheet formation, plasmoid-like eruption, and filament 'splitting', to be observed in a single event, providing strong and comprehensive evidence in favor of the model of partially erupting flux ropes.

  4. Can bubbles in quiescent prominences be purely magnetic phenomena?

    NASA Astrophysics Data System (ADS)

    Dudik, Jaroslav; Schmieder, Brigitte; Aulanier, Guillaume; Zapior, Maciej; Heinzel, Petr

    2012-07-01

    We present a model of the magnetic field constituting quiescent prominences. The model assumes a linear force-free field with a weakly twisted flux-tube in an OX/OF topology perturbed by presence of parasitic polarities within the filament channel. The parasitic polarities locally create the cusp-shaped prominences with bubbles exactly as those observed by the SDO/AIA and Bialkow Observatory. We find that the observations are best reproduced if the parasitic bipoles are sheared with respect to the main inversion line. We show that the bubbles are in fact constituted by the arcade-like field lines, as opposed to that of the prominence, which is created by magnetic dips. A pair of null points is always associated with the parasitic bipole. These null points are connected by a separator passing through the prominence bubble. We show how the presence of an additional parasitic bipole moves the separator to the boundary between the bubble and the rest of the prominence, producing a topology favorable for reconnection and possibly for the formation of plumes.

  5. On the Magnetism and Dynamics of Prominence Legs Hosting Tornadoes

    NASA Astrophysics Data System (ADS)

    Martínez González, M. J.; Asensio Ramos, A.; Arregui, I.; Collados, M.; Beck, C.; de la Cruz Rodríguez, J.

    2016-07-01

    Solar tornadoes are dark vertical filamentary structures observed in the extreme ultraviolet associated with prominence legs and filament barbs. Their true nature and relationship to prominences requires an understanding of their magnetic structure and dynamic properties. Recently, a controversy has arisen: is the magnetic field organized forming vertical, helical structures or is it dominantly horizontal? And concerning their dynamics, are tornadoes really rotating or is it just a visual illusion? Here we analyze four consecutive spectro-polarimetric scans of a prominence hosting tornadoes on its legs, which helps us shed some light on their magnetic and dynamical properties. We show that the magnetic field is very smooth in all the prominence, which is probably an intrinsic property of the coronal field. The prominence legs have vertical helical fields that show slow temporal variation that is probably related to the motion of the fibrils. Concerning the dynamics, we argue that (1) if rotation exists, it is intermittent, lasting no more than one hour, and (2) the observed velocity pattern is also consistent with an oscillatory velocity pattern (waves).

  6. Magnetic Field and Plasma Diagnostics from Coordinated Prominence Observations

    NASA Astrophysics Data System (ADS)

    Schmieder, B.; Levens, P.; Dalmasse, K.; Mein, N.; Mein, P.; Lopez-Ariste, A.; Labrosse, N.; Heinzel, P.

    2016-04-01

    We study the magnetic field in prominences from a statistical point of view, by using THEMIS in the MTR mode, performing spectropolarimetry of the He I D3 line. Combining these measurements with spectroscopic data from IRIS, Hinode/EIS as well as ground-based telescopes, such as the Meudon Solar Tower, we infer the temperature, density, and flow velocities of the plasma. There are a number of open questions that we aim to answer: - What is the general direction of the magnetic field in prominences? Is the model using a single orientation of magnetic field always valid for atypical prominences? %- Does this depend on the location of the filament on the disk (visible in Hα, in He II 304 Å) over an inversion line between weak or strong network ? - Are prominences in a weak environment field dominated by gas pressure? - Measuring the Doppler shifts in Mg II lines (with IRIS) and in Hα can tell us if there are substantial velocities to maintain vertical rotating structures, as has been suggested for tornado-like prominences. We present here some results obtained with different ground-based and space-based instruments in this framework.

  7. Interpretation of the prominence differential emissions measure for 3 geometries

    NASA Technical Reports Server (NTRS)

    Schmahl, E. J.; Orrall, F. Q.

    1986-01-01

    Researchers have used prominence extreme ultraviolet line intensities observed from Skylab to derive the differential emission measure Q(T) in the prominence-corona (PC) interface from 3 x 10,000 to 3 times 1 million K, including the effects of Lyman Continuum absorption. Using lines both shortward and longward of the Lyman limit, researchers have estimated the importance of absorption as function of temperature. The magnitude of the absorption, as well as its rate of increase as a function of temperature, place limits on the thread scales and the character of the interfilar medium. Researchers have calculated models based on three assumed geometries: (1) threads with hot sheaths and cool cores; (2) isothermal threads; and (3) threads with longitudinal temperature gradients along the magnetic field. Comparison of the absorption computed from these models with the observed absorption in prominences shows that none of the geometries is totally satisfactory.

  8. THE FORMATION AND ERUPTION OF SOLAR QUIESCENT PROMINENCES

    SciTech Connect

    Zhang, Y. Z.

    2013-11-01

    Following the two-stage catastrophic flux rope model presented by Zhang et al., we investigate how magnetic flux emergence affects the formation and evolution of solar quiescent prominences. The magnetic properties of the flux rope are described with its toroidal magnetic flux per radian Φ{sub p} and poloidal flux Φ{sub ψ}, and Φ{sub p} is defined as the emerging strength (ES) of the magnetic flux. After the first catastrophe, the quiescent prominences are supported by the vertical current sheet and located in cavities below the curved transverse current sheet in the inner corona, for which both ES and Φ{sub ψ} are in the certain ranges. We calculate the strength range as 0.25 < ES < 0.50 for the quadrupolar field, and obtain the equation Φ{sub p}Φ{sub ψ} = const., that is, the relationship between Φ{sub p} and Φ{sub ψ} of the emerging flux for which the quiescent prominences are formed in the inner corona. After the second catastrophe, the quiescent prominences would either fall down onto the solar surface or erupt as an important part of coronal mass ejections. During the eruption of the quiescent prominences, most of the magnetic energy in the flux rope is lost, and less than half of the energy loss of the rope is released in the form of Alfvèn waves. We argue that there would be two important conditions required for the formation and eruption of solar quiescent prominences, a complicated source region and emerging toroidal magnetic flux that exceeds a critical strength.

  9. Morphology and evolution of a h-alpha eruptive prominence

    NASA Astrophysics Data System (ADS)

    Okten, A.; Dermendjiev, V. N.; Petrov, N. I.; Ozisik, T.; Esenoglu, H. H.

    An eruptive prominence has been observed in H-alpha on 18 June 1989 at western solar limb (N10 degree;W90degree) in time interval 08:39-09:22 UT. The eruption started as expansion of the upper part of a filament channel crossing the equator. Several arches of erupting prominence material have been registered in more than 31 frames. All the frames have been processed and analyzed by means of microdensitometer and image processing technique for study the morphology of the eruptive event.

  10. Treatment of Prominent Ears and Otoplasty: A Contemporary Review.

    PubMed

    Pawar, Sachin S; Koch, Cody A; Murakami, Craig

    2015-01-01

    Prominent ears affect approximately 5% of the population and can have a significant psychological impact on patients. A wide variety of otoplasty techniques have been described, all sharing the goal of re-creating the normal appearance of the ear and achieving symmetry between the 2 sides. Recent trends in otoplasty techniques have consistently moved toward less invasive options, ranging from nonsurgical newborn ear molding to cartilage-sparing surgical techniques and even incisionless, office-based procedures. Herein, we review anatomy of the external ear, patient evaluation, the evolution of nonsurgical and surgical otoplasty techniques, otoplasty outcomes, and future trends for treatment of prominent ears. PMID:26158729

  11. Diagnosing the Prominence-Cavity Connection in the Solar Corona

    NASA Astrophysics Data System (ADS)

    Schmit, D. J.

    The energetic equilibrium of the corona is described by a balance of heating, thermal conduction, and radiative cooling. Prominences can be described by the thermal instability of coronal energy balance which leads to the formation of cool condensations. Observationally, the prominence is surrounded by a density depleted elliptical structure known as a cavity. In this dissertation, we use extreme ultraviolet remote sensing observations of the prominence-cavity system to diagnose the static and dynamic properties of these structures. The observations are compared with numerical models for the time-dependent coronal condensation process and the time-independent corona-prominence magnetic field. To diagnose the density of the cavity, we construct a three-dimensional structural model of the corona. This structural model allows us to synthesize extreme ultraviolet emission in the corona in a way that incorporates the projection effects which arise from the optically thin plasma. This forward model technique is used to constrain a radial density profile simultaneously in the cavity and the streamer. We use a χ2 minimization to find the density model which best matches a density sensitive line ratio (observed with Hinode/Extreme ultraviolet Imaging Spectrometer) and the white light scattered intensity (observed with Mauna Loa Solar Observatory MK4 coronagraph). We use extreme ultraviolet spectra and spectral images to diagnose the dynamics of the prominence and the surrounding corona. Based on the doppler shift of extreme ultraviolet coronal emission lines, we find that there are large regions of flowing plasma which appear to occur within cavities. These line of sight flows have speeds of 10 km/s-1 and projected spatial scales of 100 Mm. Using the Solar Dynamics Observatory Atmospheric Imaging Assembly (SDO/AIA) dataset, we observe dynamic emission from the prominence-cavity system. The SDO/AIA dataset observes multiple spectral bandpasses with different temperature

  12. A-B Distinction in a Sample of Prominent Psychotherapists

    ERIC Educational Resources Information Center

    Geller, Jesse D.; Berzins, Juris I.

    1976-01-01

    A sample of prominent psychotherapists were asked to fill out the A-B therapist "type" scale and comment on their possible differential effectiveness in treating schizoid/schizophrenic versus neurotic patients. The data suggest that B therapists desire and seek more complex and exciting sensory-cognitive inputs during therapy hours than A…

  13. 10. CANAL CUT THROUGH SHALE BEDROCK ON PROMINENT POINT, LOOKING ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    10. CANAL CUT THROUGH SHALE BEDROCK ON PROMINENT POINT, LOOKING NORTH-NORTHEAST. NOTE CONCRETE ABUTMENTS PROBABLY INSTALLED IN 1935 TO PREVENT WATER FROM ESCAPING THROUGH A CANAL BANK BREACH. - Snake River Ditch, Headgate on north bank of Snake River, Dillon, Summit County, CO

  14. Further Validation of the Coach Identity Prominence Scale

    ERIC Educational Resources Information Center

    Pope, J. Paige; Hall, Craig R.

    2014-01-01

    This study was designed to examine select psychometric properties of the Coach Identity Prominence Scale (CIPS), including the reliability, factorial validity, convergent validity, discriminant validity, and predictive validity. Coaches (N = 338) who averaged 37 (SD = 12.27) years of age, had a mean of 13 (SD = 9.90) years of coaching experience,…

  15. Controlling the Dynamics of Laboratory Simulations of Solar Prominence Eruptions

    NASA Astrophysics Data System (ADS)

    Bellan, P. M.; Hansen, J. F.

    2000-05-01

    Solar prominence eruptions have been simulated in the laboratory using a magnetized plasma gun. Still photographs obtained from two high-speed cameras in a stereographic configuration have been combined to make three-dimensional movies of the evolution of the plasma. The plasmas resemble actual solar prominences, and evolve in a reproducible sequence through three stages. First, initial breakdown forms a main current channel consisting of several filaments. Second, the filaments twist around each other. Third, the entire plasma takes on a helical structure and expands outward. The three-dimensional structure of the plasma has a chirality consistent with the sign of the injected helicity. Plasma behavior has been investigated using various boundary conditions. Most recently, coils generating a vacuum magnetic field straddling the plasma loop have been constructed. Experiments in this configuration show that the vacuum magnetic field delays the eruption of the prominence, as well as limiting the lateral bulging of the plasma loop. The arched flux tube has a minor radius of 5-15 mm and spans 12 cm between footpoints. The major radius is initially 6 cm and then increases to several times this value as the simulated prominence erupts. Typical maximum plasma currents are 60 kA and typical magnetic fields are 1-5 kG. The duration of the experiment is about 7 microseconds. The experiment takes place in a 1.4 m diameter, 2 m long vacuum chamber and uses hydrogen gas.

  16. Polarimetric measurements in prominences and "tornadoe" observed by THEMIS

    NASA Astrophysics Data System (ADS)

    Schmieder, Brigitte; López Ariste, Arturo; Levens, Peter; Labrosse, Nicolas; Dalmasse, Kévin

    2015-10-01

    Since 2013, coordinated campaigns with the THEMIS spectropolarimeter in Tenerife and other instruments (space based: Hinode/SOT, IRIS or ground based: Sac Peak, Meudon) are organized to observe prominences. THEMIS records spectropolarimetry at the He I D3 and we use the PCA inversion technique to derive their field strength, inclination and azimuth.

  17. The Prominence of Referring Expressions: Message and Lexical Level Effects

    ERIC Educational Resources Information Center

    Lam, Tuan Q.

    2012-01-01

    In conversation, speakers produce some words with greater intensity, longer duration, and higher fundamental frequency (F0) than other words. By making different words in a sentence more prominent than other words, a speaker can change the meaning implied by a sentence. This thesis explores the relationship between processing in the language…

  18. The Most Prominent Roles of an ESP Teacher

    ERIC Educational Resources Information Center

    Ghafournia, Narjes; Sabet, Shokoofeh Ahmadian

    2014-01-01

    One prominent feature of many ESP (English for Specific Purposes) courses, which make them rather different from EGP (English for General Purposes) courses, is the presence of adult learners, who are primary workers and secondary learners. As ESP is a highly learner-cantered approach, paying close attention to the multidimensional needs of…

  19. BENZODIAZEPINES FOR PROMINENT AUDITORY HALLUCINATIONS: A REPORT AND HYPOTHESIS

    PubMed Central

    Andrade, Chittaranjan

    1995-01-01

    A case is reported of diazepam - induced amelioration of prominent auditory hallucinations experienced by a female paranoid schizophrenic. With the assumption that subvocal speech may be primary to such hallucinations, it is proposed that diazepam may have acted by exerting a relaxant effect on speech musculature. This is a hypothesis testable in future research. PMID:21743715

  20. Thermal Properties of Moving UV Features in Prominences

    NASA Technical Reports Server (NTRS)

    Kucera, Therese A.

    2003-01-01

    Multi-thermal features with speeds of 5-70 kilometers per second perpendicular to the line of sight are common in the prominences which showed traceable motions. These speeds are noticeably higher than the typical speeds of 5-20 kilometers per second observed in H-alpha data from "quiet" prominences and are more typical of "activated" prominences in which H-alpha blob speeds of up to 40 kilometers per second have been reported. In order to make a more quantitative determination of the thermal properties of the moving features seen in the UV, we use the SOHO instruments SUMER and CDS to take a time series of exposures from a single pointing position, providing a measurement of spectral line properties as a function of time and position along the slit. The resulting observations in lines spectral lines in a range of "transition region" temperatures allow us to analyze the thermal properties of the moving prominence sources as a function of time.

  1. UV Observations of Prominence Activation and Cool Loop Dynamics

    NASA Technical Reports Server (NTRS)

    Kucera, Therese A.; Landi, Enrico

    2006-01-01

    In this paper we investigate the thermal and dynamic properties of dynamic structures in and around a prominence channel observed on the limb on 17 April 2003. Observations were taken with the Solar and Heliospheric Observatory's Solar Ultraviolet Measurements of Emitted Radiation (SOHO/SUMER) in lines formed at temperatures from 80,000 to 1.6 MK. The instrument was pointed to a single location and took a series of 90 s exposures. Two-dimensional context was provided by the Transition Region and Coronal Explorer (TRACE) in the UV and EUV and the Kanzelhohe Solar Observatory in H-alpha. Two dynamic features were studied in depth: an activated prominence and repeated motions in a loop near the prominence. We calculated three-dimensional geometries and trajectories, differential emission measure, and limits on the mass, pressure, average density, and kinetic and thermal energies. These observations provide important tests for models of dynamics in prominences and cool (approx. 10(exp 5) K)loops, which will ultimately lead to a better understanding the mechanism(s) leading to energy and mass flow in these solar features.

  2. Patterns of Flows in an Intermediate Prominence Observed by Hinode

    NASA Astrophysics Data System (ADS)

    Ahn, Kwangsu; Chae, Jongchul; Cao, Wenda; Goode, Philip R.

    2010-09-01

    The investigation of plasma flows in filaments/prominences gives us clues to understanding their magnetic structures. We studied the patterns of flows in an intermediate prominence observed by Hinode/SOT. By examining a time series of Hα images and Ca II H images, we have found horizontal flows in the spine and vertical flows in the barb. Both of these flows have a characteristic speed of 10-20 km s-1. The horizontal flows displayed counterstreaming. Our detailed investigation revealed that most of the moving fragments in fact reversed direction at the end point of the spine near a footpoint close to the associated active region. These returning flows may be one possible explanation of the well-known counterstreaming flows in prominences. In contrast, we have found vertical flows—downward and upward—in the barb. Most of the horizontal flows in the spine seem to switch into vertical flows when they approach the barb, and vice versa. We propose that the net force resulting from a small deviation from magnetohydrostatic equilibrium, where magnetic fields are predominantly horizontal, may drive these patterns of flow. In the prominence studied here, the supposed magnetohydrostatic configuration is characterized by magnetic field lines sagging with angles of 13° and 39° in the spine and the barb, respectively.

  3. The Effects of Partial Ionization on Prominence Mass Formation

    NASA Astrophysics Data System (ADS)

    Karpen, J. T.; Olson, K.; DeVore, C. R.; Martinez Gomez, D.; Sokolov, I.

    2015-12-01

    The origin of the prominence mass has been an open question since this cool plasma suspended in the hot corona was first discovered. We have known for a long time that the mass must come from the chromosphere, but it is unclear whether this mass is lifted bodily through magnetic levitation, injected by reconnection-driven upflows, or driven from the chromosphere by evaporation and then condensed. One evaporation-condensation scenario, the thermal nonequilibrium (TNE) model, is the most fully developed, quantitative model for the prominence plasma to date. In the TNE scenario, localized heating concentrated at the coronal loop footpoints produces chromospheric evaporation, filling the flux tube with hot, dense plasma that subsequently collapses radiatively to form cool condensations. Thus far this model has been successful in explaining the key properties of the long, persistent threads and small, highly dynamic, transient blobs in prominences, the damping of large-amplitude field-aligned prominence oscillations, the appearance of horn-shaped features above the cool prominence in EUV images of coronal cavities, and coronal rain in the ambient corona. To date, all studies of TNE have assumed that the plasma is fully ionized, which is appropriate for the hot coronal gas but unrealistic for the cool plasma below ~30,000 K. The energetics, dynamics, and evolutionary time scales of the TNE process are expected to be altered when the effects of ionization and recombination are considered. We have modified ARGOS, our 1D hydrodynamic code with adaptive mesh refinement, to include an equation of state that accounts for the effects of partial ionization of the plasma over a wide range of temperatures and densities. We will discuss the results of these simulations and their comparison with our previous studies of TNE in typical filament-supporting flux tubes. This work was partially supported by NASA's LWS Strategic Capability program.

  4. Prominence oscillations: Effect of a time-dependent background temperature

    NASA Astrophysics Data System (ADS)

    Ballester, J. L.; Carbonell, M.; Soler, R.; Terradas, J.

    2016-06-01

    Context. Small amplitude oscillations in prominences have been known about for a long time, and from a theoretical point of view, these oscillations have been interpreted in terms of standing or propagating linear magnetohydrodynamic (MHD) waves. In general, these oscillations were studied by producing small perturbations in a background equilibrium with stationary physical properties. Aims: Taking into account that prominences are dynamic plasma structures, the assumption of a stationary equilibrium is not realistic. Therefore, our main aim is to study the effects produced by a non-stationary background on slow MHD waves, which could be responsible for prominence oscillations. Methods: Assuming that the radiation term is proportional to temperature and constant external heating, we have derived an expression for the temporal variation of the background temperature, which depends on the imbalance between heating and cooling processes. Furthermore, radiative losses, together with parallel thermal conduction, have also been included as damping mechanisms for the waves. Results: As temperature increases with time, the period of slow waves decreases and the amplitude of the velocity perturbations is damped. The inclusion of radiative losses enhances the damping. As temperature decreases with time, the period of slow waves increases and the amplitude of velocity perturbations grows while, as expected, the inclusion of radiative losses contributes to the damping of oscillations. Conclusions: There is observational evidence that, in different locations of the same prominence, oscillations are damped or amplified with time. This temporal damping or amplification can be obtained by a proper combination of a variable background temperature, together with radiative damping. Furthermore, decayless oscillations can also be obtained with an appropriate choice of the characteristic radiation time.

  5. 3D Reconstruction of a Rotating Erupting Prominence

    NASA Technical Reports Server (NTRS)

    Thompson, W. T.; Kliem, B.; Torok, T.

    2011-01-01

    A bright prominence associated with a coronal mass ejection (CME) was seen erupting from the Sun on 9 April 2008. This prominence was tracked by both the Solar Terrestrial Relations Observatory (STEREO) EUVI and COR1 telescopes, and was seen to rotate about the line of sight as it erupted; therefore, the event has been nicknamed the "Cartwheel CME." The threads of the prominence in the core of the CME quite clearly indicate the structure of a weakly to moderately twisted flux rope throughout the field of view, up to heliocentric heights of 4 solar radii. Although the STEREO separation was 48 deg, it was possible to match some sharp features in the later part of the eruption as seen in the 304 Angstrom line in EUVI and in the H alpha-sensitive bandpass of COR1 by both STEREO Ahead and Behind. These features could then be traced out in three dimensional space, and reprojected into a view in which the eruption is directed towards the observer. The reconstructed view shows that the alignment of the prominence to the vertical axis rotates as it rises up to a leading-edge height of approximately equals 2.5 solar radii, and then remains approximately constant. The alignment at 2.5 solar radii differs by about 115 deg. from the original filament orientation inferred from H alpha and EUV data, and the height profile of the rotation, obtained here for the first time, shows that two thirds of the total rotation is reached within approximately equals 0.5 solar radii above the photosphere. These features are well reproduced by numerical simulations of an unstable moderately twisted flux rope embedded in external flux with a relatively strong shear field component.

  6. Structure of Prominence Legs: Plasma and Magnetic Field

    NASA Astrophysics Data System (ADS)

    Levens, P. J.; Schmieder, B.; Labrosse, N.; López Ariste, A.

    2016-02-01

    We investigate the properties of a “solar tornado” observed on 2014 July 15, and aim to link the behavior of the plasma to the internal magnetic field structure of the associated prominence. We made multi-wavelength observations with high spatial resolution and high cadence using SDO/AIA, the Interface Region Imaging Spectrograph (IRIS) spectrograph, and the Hinode/Solar Optical Telescope (SOT) instrument. Along with spectropolarimetry provided by the Télescope Héliographique pour l’Etude du Magnétisme et des Instabilités Solaires telescope we have coverage of both optically thick emission lines and magnetic field information. AIA reveals that the two legs of the prominence are strongly absorbing structures which look like they are rotating, or oscillating in the plane of the sky. The two prominence legs, which are both very bright in Ca ii (SOT), are not visible in the IRIS Mg ii slit-jaw images. This is explained by the large optical thickness of the structures in Mg ii, which leads to reversed profiles, and hence to lower integrated intensities at these locations than in the surroundings. Using lines formed at temperatures lower than 1 MK, we measure relatively low Doppler shifts on the order of ±10 km s‑1 in the tornado-like structure. Between the two legs we see loops in Mg ii, with material flowing from one leg to the other, as well as counterstreaming. It is difficult to interpret our data as showing two rotating, vertical structures that are unrelated to the loops. This kind of “tornado” scenario does not fit with our observations. The magnetic field in the two legs of the prominence is found to be preferentially horizontal.

  7. 22. GENERAL VIEW OF MILL FROM SOUTHEAST. PROMINENT ARE THE ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    22. GENERAL VIEW OF MILL FROM SOUTHEAST. PROMINENT ARE THE 100-TON STEEL CRUSHED UNOXIDIZED ORE BIN, CENTER LEFT; STEPHENS-ADAMSON 15 TON/HR INCLINED BUCKET ELEVATOR IN FRONT OF THE STEEL ORE BIN; AND THE BAKER COOLER, LOWER RIGHT. THESE MACHINES AND OTHERS IN THE AREA WERE PART OF THE UNOXIDIZED ORE CIRCUIT. THE ROASTER IS OUT OF THE PICTURE TO THE RIGHT (EAST). - Bald Mountain Gold Mill, Nevada Gulch at head of False Bottom Creek, Lead, Lawrence County, SD

  8. 3D Reconstruction of a Rotating Erupting Prominence

    NASA Technical Reports Server (NTRS)

    Thompson, W. T.; Kliem, B.; Toeroek, T.

    2011-01-01

    A bright prominence associated with a coronal mass ejection (CME) was seen erupting from the Sun on 9 April 2008. This prominence was tracked by both the Solar Terrestrial Relations Observatory (STEREO) EUVI and COR1 telescopes, and was seen to rotate about the line of sight a it erupted; therefore, the event has been nicknamed the "Cartwheel CME." The threads of the prominence in the core of the CME quite clearly indicate the structure of a weakly to moderately twisted flux rope throughout the field of view, up to heliocentric heights of 4 solar radii. Although the STEREO separation was 48 deg, it was possible to match some sharp features in the later part of the eruption as seen in the 304 A line in EUVI and in the H-alpha-sensitive bandpass of COR I by both STEREO Ahead and Behind. These features could then be traced out in three-dimensional space, and reprojected into a view in which the eruption is directed toward the observer. The reconstructed view shows that the alignment of the prominence to the vertical axis rotates as it rises up to a leading-edge height of approximately equal to 2.5 solar radii, and then remains approximately constant. The alignment at 2.5 solar radii differs by about 115 deg from the original filament orientation inferred from H-alpha and EUV data, and the height profile of the rotation, obtained here for the first time, shows that two thirds of the total rotation are reached within approximately equal to 0.5 solar radii above the photosphere. These features are well reproduced by numerical simulations of an unstable moderately twisted flux rope embedded in external flux with a relatively strong shear field component.

  9. Structure of Prominence Legs: Plasma and Magnetic Field

    NASA Astrophysics Data System (ADS)

    Levens, P. J.; Schmieder, B.; Labrosse, N.; López Ariste, A.

    2016-02-01

    We investigate the properties of a “solar tornado” observed on 2014 July 15, and aim to link the behavior of the plasma to the internal magnetic field structure of the associated prominence. We made multi-wavelength observations with high spatial resolution and high cadence using SDO/AIA, the Interface Region Imaging Spectrograph (IRIS) spectrograph, and the Hinode/Solar Optical Telescope (SOT) instrument. Along with spectropolarimetry provided by the Télescope Héliographique pour l’Etude du Magnétisme et des Instabilités Solaires telescope we have coverage of both optically thick emission lines and magnetic field information. AIA reveals that the two legs of the prominence are strongly absorbing structures which look like they are rotating, or oscillating in the plane of the sky. The two prominence legs, which are both very bright in Ca ii (SOT), are not visible in the IRIS Mg ii slit-jaw images. This is explained by the large optical thickness of the structures in Mg ii, which leads to reversed profiles, and hence to lower integrated intensities at these locations than in the surroundings. Using lines formed at temperatures lower than 1 MK, we measure relatively low Doppler shifts on the order of ±10 km s-1 in the tornado-like structure. Between the two legs we see loops in Mg ii, with material flowing from one leg to the other, as well as counterstreaming. It is difficult to interpret our data as showing two rotating, vertical structures that are unrelated to the loops. This kind of “tornado” scenario does not fit with our observations. The magnetic field in the two legs of the prominence is found to be preferentially horizontal.

  10. Predicting Node Degree Centrality with the Node Prominence Profile

    NASA Astrophysics Data System (ADS)

    Yang, Yang; Dong, Yuxiao; Chawla, Nitesh V.

    2014-11-01

    Centrality of a node measures its relative importance within a network. There are a number of applications of centrality, including inferring the influence or success of an individual in a social network, and the resulting social network dynamics. While we can compute the centrality of any node in a given network snapshot, a number of applications are also interested in knowing the potential importance of an individual in the future. However, current centrality is not necessarily an effective predictor of future centrality. While there are different measures of centrality, we focus on degree centrality in this paper. We develop a method that reconciles preferential attachment and triadic closure to capture a node's prominence profile. We show that the proposed node prominence profile method is an effective predictor of degree centrality. Notably, our analysis reveals that individuals in the early stage of evolution display a distinctive and robust signature in degree centrality trend, adequately predicted by their prominence profile. We evaluate our work across four real-world social networks. Our findings have important implications for the applications that require prediction of a node's future degree centrality, as well as the study of social network dynamics.

  11. Twisting, Rolling Motions, and Helicity in Prominence Eruptions

    NASA Astrophysics Data System (ADS)

    McKillop, Sean; Miralles, Mari Paz; Murphy, Nicholas A.; McCauley, Patrick; Su, Yingna

    2015-04-01

    Panasenco et al. [1] report observations of several CMEs that display a rolling motion about the axis of the erupting prominence. Murphy et al. [2] present simulations of line-tied asymmetric magnetic reconnection that make a falsifiable prediction regarding the handedness of rolling motions of flux ropes during solar eruptions. Mass motions in prominence eruptions tend to be complicated and characterizing these motions is a challenge. We use the AIA filament eruption catalog [3] as a source for finding events. If rolling motions are detected then we will investigate the handedness prediction. We use magnetograms from HMI to determine the strength and asymmetric properties of the photospheric magnetic field in the regions of interest and will use AIA observations to determine the handedness of the rolling motions. We then compare the photospheric magnetic information with the handedness to determine if there is a relationship between the two. We also determine the chirality of the prominences to see if there is any interesting relationship to the twist, rolling motion and/or handedness of the roll.[1] O. Panasenco, S. Martin, A. D. Joshi, & N. Srivastava, J. Atmos. Sol.-Terr. Phys., 73, 1129 (2011)[2] N. A. Murphy, M. P. Miralles, C. L. Pope, J. C. Raymond, H. D. Winter, K. K. Reeves, D. B. Seaton, A. A. van Ballegooijen, & J. Lin, ApJ, 751, 56 (2012)[3] http://aia.cfa.harvard.edu/filament/

  12. The Hα and Hβ emissions in solar prominence structures.

    NASA Astrophysics Data System (ADS)

    Stellmacher, G.; Wiehr, E.

    1994-10-01

    High precision photometry of the Halpha_ and Hbeta_ emissions is performed from spectra of four spatially high resolved quiescent prominences. The data are compared with recent observations and calculations. It is found that for faint emissions the observed Balmer decrement D=E_tot_(Halpha_)/E_tot_(Hbeta_) significantly exceeds the limiting value D=10.0 calculated for slab models. In contrast to former observations, the spatially and spectrally high resolved emission profiles do not require a hot and a cool component for an optimal fit. The deduced source functions do not yield a common value for different prominences, but show an individual mean for each prominence with a tendency for an increase with the optical thickness of Halpha_. Optically thick Halpha_ emissions with central absorptions are spatially related with narrow Hbeta_ emissions and hence with small kinetic temperatures. The narrow Hbeta_ emissions exist over a large range of optical thickness and show equal macroscopic shifts for individual emission features favouring a picture of closely tied bundles of threads.

  13. Predicting Node Degree Centrality with the Node Prominence Profile

    PubMed Central

    Yang, Yang; Dong, Yuxiao; Chawla, Nitesh V.

    2014-01-01

    Centrality of a node measures its relative importance within a network. There are a number of applications of centrality, including inferring the influence or success of an individual in a social network, and the resulting social network dynamics. While we can compute the centrality of any node in a given network snapshot, a number of applications are also interested in knowing the potential importance of an individual in the future. However, current centrality is not necessarily an effective predictor of future centrality. While there are different measures of centrality, we focus on degree centrality in this paper. We develop a method that reconciles preferential attachment and triadic closure to capture a node's prominence profile. We show that the proposed node prominence profile method is an effective predictor of degree centrality. Notably, our analysis reveals that individuals in the early stage of evolution display a distinctive and robust signature in degree centrality trend, adequately predicted by their prominence profile. We evaluate our work across four real-world social networks. Our findings have important implications for the applications that require prediction of a node's future degree centrality, as well as the study of social network dynamics. PMID:25429797

  14. Formation and Evolution of a Multi-Threaded Prominence

    NASA Technical Reports Server (NTRS)

    Luna, M.; Karpen, J. T.; DeVore, C. R.

    2012-01-01

    We investigate the process of formation and subsequent evolution of prominence plasma in a filament channel and its overlying arcade. We construct a three-dimensional time-dependent model of a filament-channel prominence suitable to be compared with observations. We combine this magnetic field structure with one-dimensional independent simulations of many flux tubes. The magnetic structure is a three-dimensional sheared double arcade, and the thermal non-equilibrium process governs the plasma evolution. We have found that the condensations in the corona can be divided into two populations: threads and blobs. Threads are massive condensations that linger in the field line dips. Blobs are ubiquitous small condensations that are produced throughout the filament and overlying arcade magnetic structure, and rapidly fall to the chromosphere. The total prominence mass is in agreement with observations. The threads are the principal contributors to the total mass, whereas the blob contribution is small. The motion of the threads is basically horizontal, while blobs move in all directions along the field. The peak velocities for both populations are comparable, but there is a weak tendency for the velocity to increase with the inclination, and the blobs with motion near vertical have the largest values of the velocity. We have generated synthetic images of the whole structure in an H proxy and in two EUV channels of the AIA instrument aboard SDO. These images show the plasma at cool, warm and hot temperatures. The theoretical differential emission measure of our system agrees very well with observations in the temperature range log T = 4.6-5.7. We conclude that the sheared-arcade magnetic structure and plasma dynamics fit well the abundant observational evidence.

  15. ARE GIANT TORNADOES THE LEGS OF SOLAR PROMINENCES?

    SciTech Connect

    Wedemeyer, Sven; Scullion, Eamon; Rouppe van der Voort, Luc; Bosnjak, Antonija; Antolin, Patrick

    2013-09-10

    Observations in the 171 A channel of the Atmospheric Imaging Assembly of the space-borne Solar Dynamics Observatory show tornado-like features in the atmosphere of the Sun. These giant tornadoes appear as dark, elongated, and apparently rotating structures in front of a brighter background. This phenomenon is thought to be produced by rotating magnetic field structures that extend throughout the atmosphere. We characterize giant tornadoes through a statistical analysis of properties such as spatial distribution, lifetimes, and sizes. A total number of 201 giant tornadoes are detected in a period of 25 days, suggesting that, on average, about 30 events are present across the whole Sun at a time close to solar maximum. Most tornadoes appear in groups and seem to form the legs of prominences, thus serving as plasma sources/sinks. Additional H{alpha} observations with the Swedish 1 m Solar Telescope imply that giant tornadoes rotate as a structure, although they clearly exhibit a thread-like structure. We observe tornado groups that grow prior to the eruption of the connected prominence. The rotation of the tornadoes may progressively twist the magnetic structure of the prominence until it becomes unstable and erupts. Finally, we investigate the potential relation of giant tornadoes to other phenomena, which may also be produced by rotating magnetic field structures. A comparison to cyclones, magnetic tornadoes, and spicules implies that such events are more abundant and short-lived the smaller they are. This comparison might help to construct a power law for the effective atmospheric heating contribution as a function of spatial scale.

  16. Are Giant Tornadoes the Legs of Solar Prominences?

    NASA Astrophysics Data System (ADS)

    Wedemeyer, Sven; Scullion, Eamon; Rouppe van der Voort, Luc; Bosnjak, Antonija; Antolin, Patrick

    2013-09-01

    Observations in the 171 Å channel of the Atmospheric Imaging Assembly of the space-borne Solar Dynamics Observatory show tornado-like features in the atmosphere of the Sun. These giant tornadoes appear as dark, elongated, and apparently rotating structures in front of a brighter background. This phenomenon is thought to be produced by rotating magnetic field structures that extend throughout the atmosphere. We characterize giant tornadoes through a statistical analysis of properties such as spatial distribution, lifetimes, and sizes. A total number of 201 giant tornadoes are detected in a period of 25 days, suggesting that, on average, about 30 events are present across the whole Sun at a time close to solar maximum. Most tornadoes appear in groups and seem to form the legs of prominences, thus serving as plasma sources/sinks. Additional Hα observations with the Swedish 1 m Solar Telescope imply that giant tornadoes rotate as a structure, although they clearly exhibit a thread-like structure. We observe tornado groups that grow prior to the eruption of the connected prominence. The rotation of the tornadoes may progressively twist the magnetic structure of the prominence until it becomes unstable and erupts. Finally, we investigate the potential relation of giant tornadoes to other phenomena, which may also be produced by rotating magnetic field structures. A comparison to cyclones, magnetic tornadoes, and spicules implies that such events are more abundant and short-lived the smaller they are. This comparison might help to construct a power law for the effective atmospheric heating contribution as a function of spatial scale.

  17. Prominent follicular mucinosis with diffuse scalp alopecia resembling alopecia areata.

    PubMed

    Missall, Tricia A; Hurley, M Yadira; Burkemper, Nicole M

    2013-10-01

    A 56-year-old Caucasian female presented with a 2-month history of alopecia. On examination, she had diffuse hair loss of her scalp with some discrete patches of nonscarring alopecia. Histopathology revealed an inflammatory nonscarring alopecia with prominent follicular mucinosis and findings suggestive of alopecia areata. The patient's alopecia completely resolved with oral prednisone. The histopathologic findings and clinical presentation are most consistent with a diagnosis of alopecia areata with follicular mucinosis, although the differential diagnosis is broad. As follicular mucinosis may be associated with both benign and malignant conditions, it is important to be cautious regarding the clinical diagnosis when this reaction pattern is observed histopathologically. PMID:23962142

  18. Model comparison for the density structure along solar prominence threads

    NASA Astrophysics Data System (ADS)

    Arregui, I.; Soler, R.

    2015-06-01

    Context. Quiescent solar prominence fine structures are typically modelled as density enhancements, called threads, which occupy a fraction of a longer magnetic flux tube. This is justified from the spatial distribution of the imaged plasma emission or absorption of prominences at small spatial scales. The profile of the mass density along the magnetic field is unknown, however, and several arbitrary alternatives are employed in prominence wave studies. The identification and measurement of period ratios from multiple harmonics in standing transverse thread oscillations offer a remote diagnostics method to probe the density variation of these structures. Aims: We present a comparison of theoretical models for the field-aligned density along prominence fine structures. They aim to imitate density distributions in which the plasma is more or less concentrated around the centre of the magnetic flux tube. We consider Lorentzian, Gaussian, and parabolic profiles. We compare theoretical predictions based on these profiles for the period ratio between the fundamental transverse kink mode and the first overtone to obtain estimates for the density ratios between the central part of the tube and its foot-points and to assess which one would better explain observed period ratio data. Methods: Bayesian parameter inference and model comparison techniques were developed and applied. To infer the parameters, we computed the posterior distribution for the density gradient parameter that depends on the observable period ratio. The model comparison involved computing the marginal likelihood as a function of the period ratio to obtain the plausibility of each density model as a function of the observable. We also computed the Bayes factors to quantify the relative evidence for each model, given a period ratio observation. Results: A Lorentzian density profile, with plasma density concentrated around the centre of the tube, seems to offer the most plausible inversion result. A

  19. Prominent Eustachian Valve in Newborns: A Report of Four Cases

    PubMed Central

    Gad, Ashraf; Mannan, Javed; Chhabra, Manoj; Zhang, Xi Xiao Yang; Narula, Pramod; Hoang, Danthanh

    2015-01-01

    The Eustachian valve (EV) is an embryological remnant of the inferior vena cava that during fetal life helps divert oxygenated blood from the IVC toward the foramen ovale to escape the pulmonary circulation. This remnant usually regresses after birth and is considered a benign finding in the majority of cases. However, EV can lead to complications in the neonatal period or later in life. In this short case series, we present four newborn infants with prominent EV who were symptomatic after birth and required admission to the neonatal intensive care unit. PMID:26929867

  20. Prominent β-relaxations in yttrium based metallic glasses

    SciTech Connect

    Luo, P.; Lu, Z.; Zhu, Z. G.; Li, Y. Z.; Bai, H. Y.; Wang, W. H.

    2015-01-19

    Most metallic glasses (MGs) exhibit weak slow β-relaxation. We report the prominent β-relaxation in YNiAl metallic glass with a wide composition range. Compared with other MGs, the MGs show a pronounced β-relaxation peak and high β-relaxation peak temperature, and the β-relaxation behavior varies significantly with the changes of the constituent elements, which is attributed to the fluctuations of chemical interactions between the components. We demonstrate the correlation between the β-relaxation and the activation of flow units for mechanical behaviors of the MG and show that the MG is model system for studying some controversial issues in glasses.

  1. Anti-spasmodic assessment of hydroalcoholic extract and essential oil of aerial part of Pycnocycla caespitosa Boiss. & Hausskn on rat ileum contractions.

    PubMed

    Sadraei, Hassan; Asghari, Gholamreza; Alipour, Mahdi

    2016-01-01

    Pycnocycla caespitosa is an essential oil-containing plant naturally growing in southwest of Iran. The extract of this plant has been used as remedy in traditional medicine. Another species of Pycnocyla (P. spinosa) possessed antispasmodic activity. The pharmacological objective of this study was to look for relaxant effect of hydroalcoholic extract and essential oil of P. caespitosa on rat isolated ileum contractions for comparison with loperamide. The essential oil and the hydroalcoholic extract were prepared by hydrodistillation and percolation techniques, respectively. For antispasmodic studies a section of rat ileum was suspended in an organ bath containing Tyrode's solution. The tissue was stimulated with electrical field stimulation (EFS), KCl (80 mM) and acetylcholine (ACh 0.5 μM). The tissue was kept under 1 g tension at 37°C and continuously gassed with O2. The essential oil content in the aerial parts of P. caespitosa was found to be 0.16 % ml/g. The essential oil was analyzed by gas chromatography and gas chromatography-mass spectrometry. Seventy constituents, representing 97 % of the oil were identified. The major components of the oil were carvacrol (7.1%), β-eudesmol (6.4 %), ρ-cymene (5.7%), caryophyllene oxide (3.6%), α-pinine (1.4%) and α-phelandrene (1.1%). The hydroalcoholic extract of P. caespitosa inhibited the response to KCl (IC50 = 48 ± 3 μg/ml), ACh (IC50 = 61 ± 14.7 μg/ml) and EFS (IC50 = 77 ± 17 μg/ml) in a concentration-dependent manner. The essential oil of P. caespitosa also inhibited rat ileum contractions. The IC50 values for KCl, ACh and EFS were 9.2 ± 1.2 μg/ml, 7.6 ± 0.8 μg/ml and 6.4 ± 0.8 μg/ml, respectively. The inhibitory effect of both the essential oil and the extract were reversible. This research confirms the anti-spasmodic activity of both the essential oil and the extract of P. caespitosa on smooth muscle contraction of ileum. PMID:27051430

  2. Anti-spasmodic assessment of hydroalcoholic extract and essential oil of aerial part of Pycnocycla caespitosa Boiss. & Hausskn on rat ileum contractions

    PubMed Central

    Sadraei, Hassan; Asghari, Gholamreza; Alipour, Mahdi

    2016-01-01

    Pycnocycla caespitosa is an essential oil-containing plant naturally growing in southwest of Iran. The extract of this plant has been used as remedy in traditional medicine. Another species of Pycnocyla (P. spinosa) possessed antispasmodic activity. The pharmacological objective of this study was to look for relaxant effect of hydroalcoholic extract and essential oil of P. caespitosa on rat isolated ileum contractions for comparison with loperamide. The essential oil and the hydroalcoholic extract were prepared by hydrodistillation and percolation techniques, respectively. For antispasmodic studies a section of rat ileum was suspended in an organ bath containing Tyrode's solution. The tissue was stimulated with electrical field stimulation (EFS), KCl (80 mM) and acetylcholine (ACh 0.5 μM). The tissue was kept under 1 g tension at 37°C and continuously gassed with O2. The essential oil content in the aerial parts of P. caespitosa was found to be 0.16 % ml/g. The essential oil was analyzed by gas chromatography and gas chromatography–mass spectrometry. Seventy constituents, representing 97 % of the oil were identified. The major components of the oil were carvacrol (7.1%), β-eudesmol (6.4 %), ρ-cymene (5.7%), caryophyllene oxide (3.6%), α-pinine (1.4%) and α-phelandrene (1.1%). The hydroalcoholic extract of P. caespitosa inhibited the response to KCl (IC50 = 48 ± 3 μg/ml), ACh (IC50 = 61 ± 14.7 μg/ml) and EFS (IC50 = 77 ± 17 μg/ml) in a concentration-dependent manner. The essential oil of P. caespitosa also inhibited rat ileum contractions. The IC50 values for KCl, ACh and EFS were 9.2 ± 1.2 μg/ml, 7.6 ± 0.8 μg/ml and 6.4 ± 0.8 μg/ml, respectively. The inhibitory effect of both the essential oil and the extract were reversible. This research confirms the anti-spasmodic activity of both the essential oil and the extract of P. caespitosa on smooth muscle contraction of ileum. PMID:27051430

  3. Hinode SOT Observations of Solar Quiescent Prominence Dynamics

    NASA Astrophysics Data System (ADS)

    Berger, Thomas E.; Shine, Richard A.; Slater, Gregory L.; Tarbell, Theodore D.; Title, Alan M.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Suematsu, Yoshinori; Tsuneta, Saku; Lites, Bruce W.; Shimizu, Toshifumi

    2008-03-01

    We report findings from multihour 0.2'' resolution movies of solar quiescent prominences (QPs) observed with the Solar Optical Telescope (SOT) on the Hinode satellite. The observations verify previous findings of filamentary downflows and vortices in QPs. SOT observations also verify large-scale transverse oscillations in QPs, with periods of 20-40 minutes and amplitudes of 2-5 Mm. The upward propagation speed of several waves is found to be ~10 km s-1, comparable to the sound speed of a 10,000 K plasma, implying that the waves are magnetoacoustic in origin. Most significantly, Hinode SOT observations reveal that dark, episodic upflows are common in QPs. The upflows are 170-700 km in width, exhibit turbulent flow, and rise with approximately constant speeds of ~20 km s-1 from the base of the prominence to heights of ~10-20 Mm. The upflows are visible in both the Ca II H-line and Hα bandpasses of SOT. The new flows are seen in about half of the QPs observed by SOT to date. The dark upflows resemble buoyant starting plumes in both their velocity profile and flow structure. We discuss thermal and magnetic mechanisms as possible causes of the plumes.

  4. Rolling Motions During Solar Prominence Eruptions in Asymmetric Magnetic Environments

    NASA Astrophysics Data System (ADS)

    McKillop, Sean; Miralles, Mari Paz; Murphy, Nicholas Arnold; McCauley, Patrick

    2014-06-01

    Panasenco et al. [1] report observations of several CMEs that display a rolling motion about the axis of the erupting prominence. Murphy et al. [2] present simulations of line-tied asymmetric magnetic reconnection that make a falsifiable prediction regarding the handedness of rolling motions of flux ropes during solar eruptions. We will present initial results of our work to investigate this prediction. To determine the strength and any asymmetric properties of the magnetic field in the regions of interest in the photosphere, we use magnetograms from HMI. We use AIA observations to determine if there is any rolling motion and, if so, what handedness the rolling motions have. We then compare the photospheric magnetic information with the handedness information to determine if there is any relationship between the two. Finally, we will discuss prospects for diagnosing rolling motions of erupting prominence using off-limb IRIS observations.[1] O. Panasenco, S. Martin, A. D. Joshi, & N. Srivastava, J. Atmos. Sol.-Terr. Phys., 73, 1129 (2011)[2] N. A. Murphy, M. P. Miralles, C. L. Pope, J. C. Raymond, H. D. Winter, K. K. Reeves, D. B. Seaton, A. A. van Ballegooijen, & J. Lin, ApJ, 751, 56 (2012)

  5. TOTAL SOLAR ECLIPSE OBSERVATIONS OF HOT PROMINENCE SHROUDS

    SciTech Connect

    Habbal, S. Rifai; Morgan, H.; Scholl, I.; Druckmueller, M.; Rusin, V.; Daw, A.; Johnson, J.; Arndt, M.

    2010-08-20

    Using observations of the corona taken during the total solar eclipses of 2006 March 29 and 2008 August 1 in broadband white light and in narrow bandpass filters centered at Fe X 637.4 nm, Fe XI 789.2 nm, Fe XIII 1074.7 nm, and Fe XIV 530.3 nm, we show that prominences observed off the solar limb are enshrouded in hot plasmas within twisted magnetic structures. These shrouds, which are commonly referred to as cavities in the literature, are clearly distinct from the overlying arch-like structures that form the base of streamers. The existence of these hot shrouds had been predicted by model studies dating back to the early 1970s, with more recent studies implying their association with twisted magnetic flux ropes. The eclipse observations presented here, which cover a temperature range of 0.9 to 2 x10{sup 6} K, are the first to resolve the long-standing ambiguity associated with the temperature and magnetic structure of prominence cavities.

  6. Modelling of solar magnetic field and prominence structures

    NASA Technical Reports Server (NTRS)

    Wu, Shi Tsan

    1988-01-01

    Using plasma theory, the interaction is studied between high frequency and magnetohydrodynamic (MHD) waves from which a set of coupling equations resulted. On the basis of this formalism, the modulation instabilities of an electromagnetic soliton in a current sheet are examined, and it is shown that there is a resistive instability at the onset of the magnetic field reconnection. This mechanism could be used to explain the onset of solar flares and prominences. To improve the resolution of vector magnetic fields at the sun's surface, state-of-the-art optics is examined to improve the design and fabrication of a new spaceborne solar vector magnetograph as part of the SAMEX (Solar Active Measurements Experiment) program.

  7. Old World frog and bird vocalizations contain prominent ultrasonic harmonics

    NASA Astrophysics Data System (ADS)

    Narins, Peter M.; Feng, Albert S.; Lin, Wenyu; Schnitzler, Hans-Ulrich; Denzinger, Annette; Suthers, Roderick A.; Xu, Chunhe

    2004-02-01

    Several groups of mammals such as bats, dolphins and whales are known to produce ultrasonic signals which are used for navigation and hunting by means of echolocation, as well as for communication. In contrast, frogs and birds produce sounds during night- and day-time hours that are audible to humans; their sounds are so pervasive that together with those of insects, they are considered the primary sounds of nature. Here we show that an Old World frog (Amolops tormotus) and an oscine songbird (Abroscopus albogularis) living near noisy streams reliably produce acoustic signals that contain prominent ultrasonic harmonics. Our findings provide the first evidence that anurans and passerines are capable of generating tonal ultrasonic call components and should stimulate the quest for additional ultrasonic species.

  8. Solar corona/prominence seen through the White Light Coronograph

    NASA Technical Reports Server (NTRS)

    1974-01-01

    The solar corona and a solar prominence as seen through the White Light Coronograph, Skylab Experiment S052, on January 17, 1974. This view was reproduced from a television transmission made by a TV camera aboard the Skylab space station in Earth orbit. The bright spot is a burn in the vidicon. The solar corona is the halo around the Sun which is normally visible only at the time of solar eclipse by the Moon. The Skylab coronography uses an externally-mounted disk system which occults the brilliant solar surface while allowing the fainter radiation of the corona to enter an annulus and be photographed. A mirror system allows either TV viewing of the corona or photographic recording of the image.

  9. The role of Magnetic Reconnection in flares and prominence eruptions

    NASA Technical Reports Server (NTRS)

    Forbes, T. G.

    1990-01-01

    Magnetic Reconnection is often invoked as the primary mechanism for driving a flare or a prominence eruption. This paper argues that a catastrophic loss of mechanical equilibrium, rather than reconnection, is probably the primary mechanism for driving these phenomena. However, reconnection is still essential in order for any significant amount of energy to be released. To illustrate this idea, some recent results are presented from an MHD simulation based on a catastrophe mechanism first proposed by Van Tend and Kuperus. In order for this mechanism to be effective, a substantial amount of reconnection must occur within a few Alfven-scale times. Such rapid reconnection is plausible since the loss of mechanical equilibrium can generate flows which drive the reconnection at a rapid rate.

  10. The production effect in memory: a prominent mnemonic in children.

    PubMed

    Icht, Michal; Mama, Yaniv

    2015-09-01

    The 'Production Effect' (PE) refers to a memory advantage for items studied aloud over items studied silently. Thus, vocalizing may serve as a mnemonic that can be used to assist learners in improving their memory for new concepts. Although many other types of mnemonic have been suggested in the literature, the PE seems especially appropriate for young children, as it does not involve literacy skills. The present study is a first investigation of the PE in children. In two experiments we tested five-year-olds in a PE paradigm using pictures of objects as stimuli. In Experiment 1, pictures of familiar objects were presented to be remembered, and in Experiment 2 we used pictures of unfamiliar objects (evaluating new vocabulary acquisition). In both experiments we showed a memory advantage for vocally produced words ('look and say') over other types of learning ('look', 'look and listen'), suggesting the PE as a prominent memory and learning tool. PMID:25404488

  11. Granuloma annulare with prominent lymphoid infiltrates ("pseudolymphomatous" granuloma annulare).

    PubMed

    Cota, Carlo; Ferrara, Gerardo; Cerroni, Lorenzo

    2012-05-01

    Granuloma annulare (GA) is characterized histopathologically by 3 patterns: necrobiotic granuloma, interstitial incomplete form and, rarely, sarcoidal or tuberculoid granuloma. The amount of lymphoid infiltrate in GA is usually limited. We describe 10 cases of GA with prominent "pseudolymphomatous" lymphoid infiltrates mimicking cutaneous lymphoid hyperplasia. Patients were 6 males and 4 females (mean age 49.9 years, median age 47 years, age range 25-70). Lesions were localized to a limited area of the body (n = 6), or involved the entire trunk (n = 3), or were generalized (n = 1). The correct clinical diagnosis of GA was provided only in 30% of the cases. In all cases, histopathologic features were characterized by dense, nodular, superficial, and deep infiltrates of lymphocytes. Immunohistology revealed predominance of T lymphocytes in 7 of 7 tested cases. This "pseudolymphomatous" variant of GA represents a pitfall in the histopathologic diagnosis of the disease and may be misinterpreted as other types of cutaneous lymphoproliferative disorders. PMID:22207445

  12. Source of a Prominent Poleward Surge During Solar Cycle 24

    NASA Astrophysics Data System (ADS)

    Yeates, A. R.; Baker, D.; van Driel-Gesztelyi, L.

    2015-11-01

    As an observational case study, we consider the origin of a prominent poleward surge of leading polarity, visible in the magnetic butterfly diagram during Solar Cycle 24. A new technique is developed for assimilating individual regions of strong magnetic flux into a surface-flux transport model. By isolating the contribution of each of these regions, the model shows the surge to originate primarily in a single high-latitude activity group consisting of a bipolar active region present in Carrington Rotations 2104 - 05 (November 2010 - January 2011) and a multipolar active region in Rotations 2107 - 08 (February - April 2011). This group had a strong axial dipole moment opposed to Joy's law. On the other hand, the modelling suggests that the transient influence of this group on the butterfly diagram will not be matched by a large long-term contribution to the polar field because it is located at high latitude. This is in accordance with previous flux-transport models.

  13. A Driven Mechanism of CMEs and Prominence Eruptions

    NASA Astrophysics Data System (ADS)

    Chen, J.; Krall, J.

    1997-05-01

    It has long been thought that solar magnetic structures such as arcades and flux ropes can erupt if the photospheric footpoints of the magnetic field lines are slowly sheared. The possible mechanisms of eruption include catastrophic loss of equilibrium and some large-scale instabilities such as the MHD kink instability. In this ``storage-release'' scenario, the shearing motion increases the twist in the coronal field, which is equivalent to a quasi-static increase in the energy associated with the horizontal component of the field of an arcade or the poloidal field of a flux rope. Alternatively, it has been shown recently [1] that an equilibrium flux rope under coronal conditions and comparable in size to quiescent prominences can erupt if the poloidal flux is increased on the timescale of eruption. The resulting dynamical properties are consistent with those of CMEs/eruptive prominences, and the computed model structure in the heliosphere closely resembles observed interplanetary magnetic clouds. We explore potentially observable signatures of this alternative scenario in which the initial structure (e.g., a flux rope) is driven by newly emergent magnetic flux. We increase the poloidal flux both quasi-statically and on the timescale of eruption. We compare the different dynamical behaviors in terms of physical observables such as the acceleration/speed of eruption, variation in the magnetic field of the flux rope, and the resulting structures at 1 AU, which can be observed by in situ measurements. The initial equilibrium flux rope and the ``erupting'' flux rope are both found to be stable to the kink mode. The physical processes in the driven versus storage-release scenarios are discussed, and possible observational discriminators are suggested. 1. Chen, J., JGR, vol. 101, 27499, 1996

  14. Three-Dimensional Morphology of a Coronal Prominence Cavity

    NASA Technical Reports Server (NTRS)

    Gibson, S. E.; Kucera, T. A.; Rastawicki, D.; Dove, J.; deToma, G.; Hao, J.; Hill, S.; Hudson, H. S.; Marque, C.; McIntosh, P. S.; Rachmeler, L.; Reeves, K. K.; Schmieder, B.; Schmit, D. J.; Seaton, D. B.; Sterling, A. C.; Tripathi, D.; Williams, D. R.; Zhang, M.

    2010-01-01

    We present a three-dimensional density model of coronal prominence cavities, and a morphological fit that has been tightly constrained by a uniquely well-observed cavity. Observations were obtained as part of an International Heliophysical Year campaign by instruments from a variety of space- and ground-based observatories, spanning wavelengths from radio to soft-X-ray to integrated white light. From these data it is clear that the prominence cavity is the limb manifestation of a longitudinally-extended polar-crown filament channel, and that the cavity is a region of low density relative to the surrounding corona. As a first step towards quantifying density and temperature from campaign spectroscopic data, we establish the three-dimensional morphology of the cavity. This is critical for taking line-of-sight projection effects into account, since cavities are not localized in the plane of the sky and the corona is optically thin. We have augmented a global coronal streamer model to include a tunnel-like cavity with elliptical cross-section and a Gaussian variation of height along the tunnel length. We have developed a semi-automated routine that fits ellipses to cross-sections of the cavity as it rotates past the solar limb, and have applied it to Extreme Ultraviolet Imager (EUVI) observations from the two Solar Terrestrial Relations Observatory (STEREO) spacecraft. This defines the morphological parameters of our model, from which we reproduce forward-modeled cavity observables. We find that cavity morphology and orientation, in combination with the viewpoints of the observing spacecraft, explains the observed variation in cavity visibility for the east vs. west limbs

  15. Magnetic topology and prominence patterns on AB Doradus

    NASA Astrophysics Data System (ADS)

    Donati, J.-F.; Collier Cameron, A.; Hussain, G. A. J.; Semel, M.

    1999-01-01

    We report new Zeeman--Doppler imaging observations of the rapidly rotating young K0 dwarf AB Doradus, obtained with the Anglo-Australian Telescope in 1996 December. From such observations, simultaneous brightness and magnetic images of the stellar photosphere of AB Dor were reconstructed at three different epochs. The magnetic topology of AB Dor is found to be very complex, with at least 12 different radial field regions of opposite polarities located all around the star. Significant azimuthal field fluxes are also detected in the form of one negative polarity region close to the equator, a series of positive polarity patches at intermediate latitudes and an almost complete ring of negative polarity encircling the rotational pole at high latitudes. In particular, the azimuthal polarities we reconstruct are in very good agreement with those obtained by Donati & Cameron, confirming that this field component is directly related to the dynamo-generated large-scale toroidal magnetic structure. The triple polarity latitudinal pattern observed for this structure in the upper hemisphere of AB Dor indicates that the degree of the underlying large-scale poloidal structure in an axisymmetric spherical harmonics expansion is equal to or greater than five. It also strengthens the idea that the dynamo processes operating in AB Dor feature a non-solar component distributed throughout the convective zone. From the subtle distortion of successive brightness images, we can also confirm the surface differential rotation first measured on this star by Donati & Cameron in both sense and magnitude, with a pole rotating more slowly than the equator by about one part in 220. Finally, the rotation periods we measure for four prominences (from the recurrence rate of their spectral signatures in Balmer lines) confirm the presumption that such clouds are anchored at intermediate to high latitudes. The intrinsic variability of these prominences is not associated with any abrupt changes in the

  16. Averages of sound pressure levels and mean fundamental frequencies of speech in relation to phonetograms: comparison of nonorganic dysphonia patients before and after therapy.

    PubMed

    Akerlund, L

    1993-01-01

    The interdependence of changes in mean fundamental frequency and mean phonatory sound level, before and after voice treatment, was studied in 22 female and 11 male patients suffering from nonorganic dysphonia. All patients read continuous texts at three different vocal loudness levels, and also while being exposed to a filtered noise. After the reading sessions, phonetograms were recorded. The female patients achieved a higher mean sound level during the speech test after therapy. By contrast, the male patients increased their mean fundamental frequencies less during noise exposure after therapy, while the female patients retained essentially the same mean fundamental frequencies afterwards. The female patients produced a significantly higher upper phonetogram contour after therapy, whereas the male patients lowered their lower phonetogram contour. PMID:8442416

  17. Spasmodic Torticollis: Signs and Symptoms

    MedlinePlus

    ... pulling” from among these four categories. Latest News & Events NSTA Hosts Two Successful Fundraisers! NSTA Summerfest Fundraiser – ... Selective Denervation Surgery Physical Therapy Latest News and Events NSTA Hosts Two Successful Fundraisers! NSTA Summerfest Fundraiser – ...

  18. A closer view of prominent rocks - 3D

    NASA Technical Reports Server (NTRS)

    1997-01-01

    Many prominent rocks near the Sagan Memorial Station are featured in this image, taken in stereo by the Imager for Mars Pathfinder (IMP) on Sol 3. 3D glasses are necessary to identify surface detail. Shark, Half-Dome, Pumpkin, Flat Top and Frog are at center. Little Flat Top is at right. The horizon in the distance is one to two kilometers away.

    Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is an operating division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator.

    Click below to see the left and right views individually. [figure removed for brevity, see original site] Left [figure removed for brevity, see original site] Right

  19. Eliciting the most prominent perceived differences between microphones.

    PubMed

    Pearce, Andy; Brookes, Tim; Dewhirst, Martin; Mason, Russell

    2016-05-01

    The attributes contributing to the differences perceived between microphones (when auditioning recordings made with those microphones) are not clear from previous research. Consideration of technical specifications and expert opinions indicated that recording five programme items with eight studio and two microelectromechanical system microphones could allow determination of the attributes related to the most prominent inter-microphone differences. Pairwise listening comparisons between the resulting 50 recordings, followed by multi-dimensional scaling analysis, revealed up to 5 salient dimensions per programme item; 17 corresponding pairs of recordings were selected exemplifying the differences across those dimensions. Direct elicitation and panel discussions on the 17 pairs identified a hierarchy of 40 perceptual attributes. An attribute contribution experiment on the 31 lowest-level attributes in the hierarchy allowed them to be ordered by degree of contribution and showed brightness, harshness, and clarity to always contribute highly to perceived inter-microphone differences. This work enables the future development of objective models to predict these important attributes. PMID:27250188

  20. Howard Russell Butler's Oil Paintings of Solar Eclipses and Prominences

    NASA Astrophysics Data System (ADS)

    Pasachoff, Jay M.; Olson, Roberta J. M.

    2014-06-01

    Howard Russell Butler (1856-1934) was invited to join the US Naval Observatory expedition to the total solar eclipse of 1918 because of his ability to paint astronomical phenomena based on quickly-made notes about spatial and color details. His giant triptych of the total eclipses of 1918, 1923, and 1925 was proposed for a never-built astronomical center at the American Museum of Natural History and wound up at their Hayden Planetarium when it was constructed in the mid-1930s. Half-size versions are installed at the Fels Planetarium at the Franklin Institute in Philadelphia and at the Firestone Library of Princeton University, whose newly conserved canvases were recently hung; the Buffalo Museum of Science has another half-size version in storage. We discuss not only the eclipse triptychs but also the series of large oil paintings he made of solar prominences (in storage at the American Museum of Natural History) and of his 1932-eclipse and other relevant works.JMP was supported for this work in part by Division III Discretionary Funds and the Brandi Fund of Williams College. His current eclipse research is supported by grants AGS-1047726 from the Solar Research Program of the Atmospheric and Geospace Sciences Division of NSF and 9327-13 from the Committee for Research and Exploration of the National Geographic Society.

  1. PROMINENCE PLASMA DIAGNOSTICS THROUGH EXTREME-ULTRAVIOLET ABSORPTION

    SciTech Connect

    Landi, E.; Reale, F.

    2013-07-20

    In this paper, we introduce a new diagnostic technique that uses EUV and UV absorption to determine the electron temperature and column emission measure, as well as the He/H relative abundance of the absorbing plasma. If a realistic assumption on the geometry of the latter can be made and a spectral code such as CHIANTI is used, then this technique can also yield the absorbing plasma hydrogen and electron density. This technique capitalizes on the absorption properties of hydrogen and helium at different wavelength ranges and temperature regimes. Several cases where this technique can be successfully applied are described. This technique works best when the absorbing plasma is hotter than 15,000 K. We demonstrate this technique on AIA observations of plasma absorption during a coronal mass ejection eruption. This technique can be easily applied to existing observations of prominences and cold plasmas in the Sun from almost all space missions devoted to the study of the solar atmosphere, which we list.

  2. Prominent reflexive eye-movement orienting associated with deafness.

    PubMed

    Bottari, Davide; Valsecchi, Matteo; Pavani, Francesco

    2012-01-01

    Profound deafness affects orienting of visual attention. Until now, research focused exclusively on covert attentional orienting, neglecting whether overt oculomotor behavior may also change in deaf people. Here we used the pro- and anti-saccade task to examine the relative contribution of reflexive and voluntary eye-movement control in profoundly deaf and hearing individuals. We observed a behavioral facilitation in reflexive compared to voluntary eye movements, indexed by faster saccade latencies and smaller error rates in pro- than anti-saccade trials, which was substantially larger in deaf than hearing participants. This provides the first evidence of plastic changes related to deafness in overt oculomotor behavior, and constitutes an ecologically relevant parallel to the modulations attributed to deafness in covert attention orienting. Our findings also have implications for designers of real and virtual environments for deaf people and reveal that experiments on deaf visual abilities must not ignore the prominent reflexive eye-movement orienting in this sensory-deprived population. PMID:24168645

  3. Radiologic comparison of erosive polyarthritis with prominent interphalangeal involvement

    SciTech Connect

    Gold, R.H.; Bassett, L.W.; Theros, E.G.

    1982-05-01

    Psoriatic arthritis, Reiter's disease, and multicentric reticulohistiocytosis may manifest prominent interphalangeal joint and cutaneous involvement. All three disorders may also affect the sacroiliac joints and spine. Despite these similarities, there are basic radiologic differences enabling distinction between the three disorders. Erosive osteoarthritis must also be considered in the differential diagnosis of interphalangeal erosive arthritis. Psoriatic erosions are characteristically ill defined, often bilaterally asymmetrical, usually unaccompanied by significant osteoporosis, and frequently associated with florid proliferation of subperiosteal new bone. An unilateral polyarticular pattern, which often occurs in a single ray, is the most prevalent of several patterns of involvement. Reiter's disease exhibits many clinical and radiologic similarities to psoriatic arthritis, but in the former there tends to be selective involvement of the joints of the lower limbs and particularly the feet, with relative sparing of the hands and wrists, while in the latter the joints of the upper and lower limbs tend to be involved to an equal extent. Multicentric reticulohistiocytosis (MR). Lesions predominate in skin and synovium and result in sharply circumscribed, rapidly progressive, strikingly bilaterally symmetrical erosions spreading from joint margins to articular surfaces. Most or all of the diarthrodial joints may be affected, but interphalangeal joint predominance and early and severe atlanto-axial involvement are characteristic. Erosive osteoarthritis is characterized by interphalangeal subchondral erosions, accompanying periosteal new bone that is more subtle than that of psoriatic arthritis, and interphalangeal bony ankylosis that occurs with the same frequency as that of psoriatic arthritis.

  4. The coordination of boundary tones and its interaction with prominence.

    PubMed

    Katsika, Argyro; Krivokapić, Jelena; Mooshammer, Christine; Tiede, Mark; Goldstein, Louis

    2014-05-01

    This study investigates the coordination of boundary tones as a function of stress and pitch accent. Boundary tone coordination has not been experimentally investigated previously, and the effect of prominence on this coordination, and whether it is lexical (stress-driven) or phrasal (pitch accent-driven) in nature is unclear. We assess these issues using a variety of syntactic constructions to elicit different boundary tones in an Electromagnetic Articulography (EMA) study of Greek. The results indicate that the onset of boundary tones co-occurs with the articulatory target of the final vowel. This timing is further modified by stress, but not by pitch accent: boundary tones are initiated earlier in words with non-final stress than in words with final stress regardless of accentual status. Visual data inspection reveals that phrase-final words are followed by acoustic pauses during which specific articulatory postures occur. Additional analyses show that these postures reach their achievement point at a stable temporal distance from boundary tone onsets regardless of stress position. Based on these results and parallel findings on boundary lengthening reported elsewhere, a novel approach to prosody is proposed within the context of Articulatory Phonology: rather than seeing prosodic (lexical and phrasal) events as independent entities, a set of coordination relations between them is suggested. The implications of this account for prosodic architecture are discussed. PMID:25300341

  5. 76 FR 59704 - Agency Information Collection Activities; Proposed Collection; Comment Request; Prominent and...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-09-27

    ... Collection; Comment Request; Prominent and Conspicuous Mark of Manufacturers on Single-Use Devices AGENCY... of information technology. Prominent and Conspicuous Mark of Manufacturers on Single-Use Devices...

  6. Catalogue of equivalent widths and line intensities for prominences observed during 1964-1965

    NASA Technical Reports Server (NTRS)

    Rakhubovskiy, A. S.

    1973-01-01

    The method of observation and processing of the prominence spectra are described briefly. The equivalent widths, central intensities, half-widths and Doppler halfwidths are presented of the emission lines of the prominences.

  7. Radio observations of the setting of a quiescent prominence behind the solar limb and the interpretation of results on the eclipse of a prominence on July 31, 1981

    SciTech Connect

    Apushkinskii, G.P.; Topchilo, N.A.

    1985-07-01

    Radio observations of the setting of a quiescent prominence behind the solar limb at 0.8 cm permit a determination of its structure. The chromosphere below the prominence does not emit in the radio range: The radio radius equals the optical radius. The results of the eclipse of July 31, 1981, can be interpreted similarly.

  8. Damping of prominence longitudinal oscillations due to mass accretion

    NASA Astrophysics Data System (ADS)

    Ruderman, Michael S.; Luna, Manuel

    2016-06-01

    We study the damping of longitudinal oscillations of a prominence thread caused by the mass accretion. We suggested a simple model describing this phenomenon. In this model we considered a thin curved magnetic tube filled with the plasma. The prominence thread is in the central part of the tube and it consists of dense cold plasma. The parts of the tube at the two sides of the thread are filled with hot rarefied plasma. We assume that there are flows of rarefied plasma toward the thread caused by the plasma evaporation at the magnetic tube footpoints. Our main assumption is that the hot plasma is instantaneously accommodated by the thread when it arrives at the thread, and its temperature and density become equal to those of the thread. Then we derive the system of ordinary differential equations describing the thread dynamics. We solve this system of ordinary differential equations in two particular cases. In the first case we assume that the magnetic tube is composed of an arc of a circle with two straight lines attached to its ends such that the whole curve is smooth. A very important property of this model is that the equations describing the thread oscillations are linear for any oscillation amplitude. We obtain the analytical solution of the governing equations. Then we obtain the analytical expressions for the oscillation damping time and periods. We find that the damping time is inversely proportional to the accretion rate. The oscillation periods increase with time. We conclude that the oscillations can damp in a few periods if the inclination angle is sufficiently small, not larger that 10°, and the flow speed is sufficiently large, not less that 30 km s-1. In the second model we consider the tube with the shape of an arc of a circle. The thread oscillates with the pendulum frequency dependent exclusively on the radius of curvature of the arc. The damping depends on the mass accretion rate and the initial mass of the threads, that is the mass of the

  9. Demonstration of prominent actin filaments in the root columella

    NASA Technical Reports Server (NTRS)

    Collings, D. A.; Zsuppan, G.; Allen, N. S.; Blancaflor, E. B.; Brown, C. S. (Principal Investigator)

    2001-01-01

    The distribution of actin filaments within the gravity-sensing columella cells of plant roots remains poorly understood, with studies over numerous years providing inconsistent descriptions of actin organization in these cells. This uncertainty in actin organization, and thus in actin's role in graviperception and gravisignaling, has led us to investigate actin arrangements in the columella cells of Zea mays L., Medicago truncatula Gaertn., Linum usitatissiilium L. and Nicotianla benthamiana Domin. Actin organization was examined using a combination of optimized immunofluorescence techniques, and an improved fluorochrome-conjugated phalloidin labeling method reliant on 3-maleimidobenzoyl-N-hydroxy-succinimide ester (MBS) cross-linking combined with glycerol permeabilization. Confocal microscopy of root sections labeled with anti-actin antibodies revealed patterns suggestive of actin throughout the columella region. These patterns included short and fragmented actin bundles, fluorescent rings around amyloplasts and intense fluorescence originating from the nucleus. Additionally, confocal microscopy of MBS-stabilized and Alexa Fluor-phalloidin-labeled root sections revealed a previously undetected state of actin organization in the columella. Discrete actin structures surrounded the amyloplasts and prominent actin cables radiated from the nuclear surface toward the cell periphery. Furthermore, the cortex of the columella cells contained fine actin bundles (or single filaments) that had a predominant transverse orientation. We also used confocal microscopy of plant roots expressing endoplasmic reticulum (ER)-targeted green fluorescent protein to demonstrate rapid ER movements within the columella cells, suggesting that the imaged actin network is functional. The successful identification of discrete actin structures in the root columella cells forms the perception and signaling.

  10. MORPHOLOGY AND DYNAMICS OF SOLAR PROMINENCES FROM 3D MHD SIMULATIONS

    SciTech Connect

    Terradas, J.; Soler, R.; Oliver, R.; Ballester, J. L.; Luna, M.

    2015-01-20

    In this paper we present a numerical study of the time evolution of solar prominences embedded in sheared magnetic arcades. The prominence is represented by a density enhancement in a background-stratified atmosphere and is connected to the photosphere through the magnetic field. By solving the ideal magnetohydrodynamic equations in three dimensions, we study the dynamics for a range of parameters representative of real prominences. Depending on the parameters considered, we find prominences that are suspended above the photosphere, i.e., detached prominences, but also configurations resembling curtain or hedgerow prominences whose material continuously connects to the photosphere. The plasma-β is an important parameter that determines the shape of the structure. In many cases magnetic Rayleigh-Taylor instabilities and oscillatory phenomena develop. Fingers and plumes are generated, affecting the whole prominence body and producing vertical structures in an essentially horizontal magnetic field. However, magnetic shear is able to reduce or even to suppress this instability.

  11. Weighted current sheets supported in normal and inverse configurations - A model for prominence observations

    NASA Technical Reports Server (NTRS)

    Demoulin, P.; Forbes, T. G.

    1992-01-01

    A technique which incorporates both photospheric and prominence magnetic field observations is used to analyze the magnetic support of solar prominences in two dimensions. The prominence is modeled by a mass-loaded current sheet which is supported against gravity by magnetic fields from a bipolar source in the photosphere and a massless line current in the corona. It is found that prominence support can be achieved in three different kinds of configurations: an arcade topology with a normal polarity; a helical topology with a normal polarity; and a helical topology with an inverse polarity. In all cases the important parameter is the variation of the horizontal component of the prominence field with height. Adding a line current external to the prominence eliminates the nonsupport problem which plagues virtually all previous prominence models with inverse polarity.

  12. Magnetic field evolution during prominence eruptions and two-ribbon flares

    NASA Technical Reports Server (NTRS)

    Priest, E. R.; Forbes, T. G.

    1990-01-01

    Simple models for the MHD eruption of a solar prominence are presented in which the prominence is treated as a twisted magnetic flux tube that is being repelled from the solar surface by magnetic pressure forces. Including a background magnetic field allows the prominence to be in equilibrium initially with an inverse polarity and then to erupt due to magnetic nonequilibrium when the background magnetic field is too small or the prominence twist is too great. The electric field at the neutral point below the prominence rapidly increases to a maximum value and then declines. Including the effect of gravity also allows an equilibrium with normal polarity to exist. Finally, an ideal MHD solution is found which incorporates self-consistently a current sheet below the prominence and which implies that a prominence will still erupt and form a current sheet even if no reconnection occurs. When reconnection is allowed it is, therefore, driven by the eruption.

  13. Measurement of Residual Flexibility for Substructures Having Prominent Flexible Interfaces

    NASA Technical Reports Server (NTRS)

    Tinker, Michael L.; Bookout, Paul S.

    1994-01-01

    structure in both test and analysis. Measured and predicted residual functions are compared, and regions of poor data in the measured curves are described. It is found that for accurate residual measurements, frequency response functions having prominent stiffness lines in the acceleration/force format are needed. The lack of such stiffness lines increases measurement errors. Interface drive point frequency respose functions for shuttle orbiter payloads exhibit dominant stiffness lines, making the residual test approach a good candidate for payload modal tests when constrained tests are inappropriate. Difficulties in extracting a residual flexibility value from noisy test data are discussed. It is shown that use of a weighted second order least-squares curve fit of the measured residual function allows identification of residual flexibility that compares very well with predictions for the simple structure. This approach also provides an estimate of second order residual mass effects.

  14. Using Prominence Mass Inferences in Different Coronal Lines to Obtain the He/H Abundance

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly; Kilper, Gary; Alexander, David; Kucera, Therese

    2008-01-01

    In a previous study we developed a new technique for deriving prominence mass by observing how much coronal radiation in the Fe XI1 (lambda 195) spectral line is absorbed by prominence material. In the present work we apply this method, which allows us to consider the effects of both foreground and background radiation in our calculations, to a sample of prominences absorbing in a coronal line that ionizes both H and He (h < 504 Angstroms), and a line that ionizes only H (504 Angstroms < lambda < 911 Angstroms). This approach, first suggested by Kucera et al. (1998), permits the determination of the abundance ratio [He I]/[H I] of neutral helium and hydrogen in the prominence. This ratio should depend on how the prominence is formed, on its current thermodynamic state, and on its dynamical evolution. Thus, it may provide useful insights into the formation and evolution of prominences.

  15. Using Prominence Mass Inferences in Different Coronal Lines to Obtain the He/H Abundance

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly; Kilper, Gary; Alexander, David; Kucera, Therese

    2009-01-01

    In a previous study we developed a new technique for deriving prominence mass by observing how much coronal radiation in the Fe XII (lambda195) spectral Line is absorbed by prominence material. In the present work we apply this method. which allows us to consider the effects of both foreground and background radiation in our calculations, to a sample of prominences absorbing in a coronal line that ionizes both H and He (lambda < 504 Angstroms), and a line that ionizes only H (504 Angstroms < lambda < 911 Angstroms). This approach, first suggested by Mucera et al. (1998). permits the determination of the abundance ratio [He I]/[H I] of neutral helium and hydrogen in the prominence. This ratio should depend on how the prominence is formed, on its current thermodynamic state, and on its dynamical evolution. Thus, it may provide useful insights into the formation and evolution of prominences.

  16. Quiescent Prominence Structure and Dynamics: a new View From the Hinode/SOT

    NASA Astrophysics Data System (ADS)

    Berger, T.; Okamoto, J.; Slater, G.; Magara, T.; Tarbell, T.; Tsuneta, S.; Hurlburt, N.

    2008-05-01

    To date the Hinode/Solar Optical Telescope (SOT) has produced over a dozen sub-arcsecond, multi-hour movies of quiescent solar prominences in both the Ca II 396.8~nm H-line and the H-alpha 656.3~nm line. These datasets have revealed new details of the structure and dynamics of quiescent prominences including a new form of mass transport in the form of buoyant plume upflows from the chromosphere. We review the SOT prominence datasets to show that quiescent prominences appear in two major morphological categories: "vertically" and "horizontally" structured. The vertically structured prominences all show ubiquitous downflows in 400--700~km wide "streams" with velocities of approximately 10~km~s-1. Most of the vertically structured prominences also show episodic upflows in the form of dark turbulent plumes with typical velocities of 20~km~s-1. Large-scale oscillations are frequently seen in vertical prominences with periods on the order of 10 min and upward propagation speeds of approximately 10~km~s-1. In addition, "bubble" events in which large voids 10--30~Mm across inflate and then burst are seen in some of the vertical prominences. In contrast, the horizontally structured quiescent prominences exhibit only limited flows along the horizontal filaments. We speculate on the origin of the distinction between the vertically and horizontally structured prominences, taking into account viewing angle and the underlying photospheric magnetic flux density. We also discuss the nature of the mysterious dark plumes and bubble expansions and their implications for prominence mass balance in light of recent models of prominence magnetic structure that find vertical flows along some field lines.

  17. The role of Alfvén wave heating in solar prominences

    NASA Astrophysics Data System (ADS)

    Soler, Roberto; Terradas, Jaume; Oliver, Ramon; Ballester, Jose Luis

    2016-07-01

    Observations have shown that magnetohydrodynamic waves over a large frequency range are ubiquitous in solar prominences. The waves are probably driven by photospheric motions and may transport energy up to prominences suspended in the corona. Dissipation of wave energy can lead to heating of the cool prominence plasma, thereby contributing to the local energy balance within the prominence. Here we discuss the role of Alfvén wave dissipation as a heating mechanism for the prominence plasma. We consider a slab-like quiescent prominence model with a transverse magnetic field embedded in the solar corona. The prominence medium is modeled as a partially ionized plasma composed of a charged ion-electron single fluid and two separate neutral fluids corresponding to neutral hydrogen and neutral helium. Friction between the three fluids acts as a dissipative mechanism for the waves. The heating caused by Alfvén waves incident on the prominence slab is analytically explored. We find that the dense prominence slab acts as a resonant cavity for the waves. The fraction of incident wave energy that is channeled into the slab strongly depends upon the wave period, P. Using typical prominence conditions, we obtain that wave energy trapping and associated heating are negligible when P ≳ 100 s, so that it is unlikely that those waves have a relevant influence on prominence energetics. When 1 s ≲ P ≲ 100 s the energy absorption into the slab shows several sharp and narrow peaks that can reach up to ~100% when the incident wave frequency matches a cavity resonance of the slab. Wave heating is enhanced at those resonant frequencies. Conversely, when P ≲ 1 s cavity resonances are absent, but the waves are heavily damped by the strong dissipation. We estimate that wave heating may compensate for about 10% of radiative losses of the prominence plasma.

  18. Hinode/SOT Measurements of Flows and Waves in Solar Prominences

    NASA Astrophysics Data System (ADS)

    Berger, Thomas; Okamoto, Takenori; Schmieder, Brigitte

    We review Hinode Solar Optical Telescope (SOT) measurements of flows and waves in quies-cent and active solar prominences. In quiescent prominences, Hinode/SOT observations have revealed a new mode of buoyant transport in the form of dark upflows that originate at the chromospheric base of the prominence. The upflows can take the form of large-scale (10 Mm) "bubbles" that rise through the entire prominence into the overlying coronal cavity, or they can take the form of numerous small-scale (1 Mm) plumes that generate from an apparent Rayleigh-Taylor instability on the boundary between the prominence and the impinging buoy-ant flow system. The episodic flows directly inject mass, magnetic flux, and helicity into the overlying coronal cavity, moving the system towards destabilization and eruption in the form of CMEs. Hinode/SOT quiescent prominence observations have also verified the existence of ubiquitous downflow streams and vortex flows confirming that prominences are far from magne-tostatic conditions. Tracking and doppler measurements of prominence downflows find speeds of 5-15 km s-1 and imply that the trajectories are not strictly vertical. Active region promi-nence studies find counter-streaming flows along horizontal magnetic field lines with velocities of 20-30 km s-1 ; upflows, downflow streams, and rotational flows have not been observed in these systems. Active Region prominence field lines exhibit transverse oscillations indicative of Alfv`n waves with periods of several minutes, amplitudes of 1 Mm, and wavelengths of 250 Mm or more. These properties are consistent with magnetic field strengths of 50 gauss or more at typical prominence density conditions and carry enough energy to heat the surrounding prominence/corona transition region (PCTR).

  19. DETERMINATION OF PROMINENCE PLASMA {beta} FROM THE DYNAMICS OF RISING PLUMES

    SciTech Connect

    Hillier, Andrew; Hillier, Richard; Tripathi, Durgesh

    2012-12-20

    Observations by the Hinode satellite show in great detail the dynamics of rising plumes, dark in chromospheric lines, in quiescent prominences that propagate from large ({approx}10 Mm) bubbles that form at the base of the prominences. These plumes present a very interesting opportunity to study magnetohydrodynamic (MHD) phenomena in quiescent prominences, but obstacles still remain. One of the biggest issues is that of the magnetic field strength, which is not easily measurable in prominences. In this paper we present a method that may be used to determine a prominence's plasma {beta} when rising plumes are observed. Using the classic fluid dynamic solution for flow around a circular cylinder with an MHD correction, the compression of the prominence material can be estimated. This has been successfully confirmed through simulations; application to a prominence gave an estimate of the plasma {beta} as {beta} = 0.47 {+-} 0.079 to 1.13 {+-} 0.080 for the range {gamma} = 1.4-1.7. Using this method it may be possible to estimate the plasma {beta} of observed prominences, therefore helping our understanding of a prominence's dynamics in terms of MHD phenomena.

  20. Nine-month-old infants are sensitive to the temporal alignment of prosodic and gesture prominences.

    PubMed

    Esteve-Gibert, Núria; Prieto, Pilar; Pons, Ferran

    2015-02-01

    This study investigated the sensitivity of 9-month-old infants to the alignment between prosodic and gesture prominences in pointing-speech combinations. Results revealed that the perception of prominence is multimodal and that infants are aware of the timing of gesture-speech combinations well before they can produce them. PMID:25656953

  1. Tic Tac TOE: Effects of Predictability and Importance on Acoustic Prominence in Language Production

    ERIC Educational Resources Information Center

    Watson, Duane G.; Arnold, Jennifer E.; Tanenhaus, Michael K.

    2008-01-01

    Importance and predictability each have been argued to contribute to acoustic prominence. To investigate whether these factors are independent or two aspects of the same phenomenon, naive participants played a verbal variant of Tic Tac Toe. Both importance and predictability contributed independently to the acoustic prominence of a word, but in…

  2. Changes in the Facial Prominence of Women and Men over the Last Decade.

    ERIC Educational Resources Information Center

    Nigro, Georgia N.; And Others

    1988-01-01

    Measured facial prominence of women and men in popular images since the 1970s. Examined 1,200 photographs from "Time" and "Newsweek" (Study 1) and 640 photographs from "Good Housekeeping" and "Ms." (Study 2). Found men had received greater facial prominence than women. Results confirm asymmetry in representation of men's and women's faces and…

  3. Phonetic Realization and Perception of Prominence among Lexical Tones in Mandarin Chinese

    ERIC Educational Resources Information Center

    Bao, Mingzhen

    2008-01-01

    Linguistic prominence is defined as words or syllables perceived auditorily as standing out from their environment. It is explored through changes in pitch, duration and loudness. In this study, phonetic realization and perception of prominence among lexical tones in Mandarin Chinese was investigated in two experiments. Experiment 1 explored…

  4. 21 CFR 501.15 - Animal food; prominence of required statements.

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... 21 Food and Drugs 6 2011-04-01 2011-04-01 false Animal food; prominence of required statements... SERVICES (CONTINUED) ANIMAL DRUGS, FEEDS, AND RELATED PRODUCTS ANIMAL FOOD LABELING General Provisions § 501.15 Animal food; prominence of required statements. (a) A word, statement, or other...

  5. 21 CFR 501.15 - Animal food; prominence of required statements.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... 21 Food and Drugs 6 2010-04-01 2010-04-01 false Animal food; prominence of required statements... SERVICES (CONTINUED) ANIMAL DRUGS, FEEDS, AND RELATED PRODUCTS ANIMAL FOOD LABELING General Provisions § 501.15 Animal food; prominence of required statements. (a) A word, statement, or other...

  6. 77 FR 3779 - Guidance for Industry on Product Name Placement, Size, and Prominence in Advertising and...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-01-25

    ... media, emails, CD-ROMs, and DVDs. In the Federal Register of March 12, 1999 (64 FR 12341), FDA announced... Prominence in Advertising and Promotional Labeling; Availability AGENCY: Food and Drug Administration, HHS... guidance document entitled ``Product Name Placement, Size, and Prominence in Advertising and...

  7. CRITICAL HEIGHT FOR THE DESTABILIZATION OF SOLAR PROMINENCES: STATISTICAL RESULTS FROM STEREO OBSERVATIONS

    SciTech Connect

    Liu Kai; Wang Yuming; Wang Shui; Shen Chenglong

    2012-01-10

    At which height is a prominence inclined to be unstable, or where is the most probable critical height for the prominence destabilization? This question was statistically studied based on 362 solar limb prominences well recognized by Solar Limb Prominence Catcher and Tracker from 2007 April to the end of 2009. We found that there are about 71% disrupted prominences (DPs), among which about 42% of them did not erupt successfully and about 89% of them experienced a sudden destabilization process. After a comprehensive analysis of the DPs, we discovered the following: (1) Most DPs become unstable at a height of 0.06-0.14 R{sub Sun} from the solar surface, and there are two most probable critical heights at which a prominence is very likely to become unstable, the first one is 0.13 R{sub Sun} and the second one is 0.19 R{sub Sun }. (2) An upper limit for the erupting velocity of eruptive prominences (EPs) exists, which decreases following a power law with increasing height and mass; accordingly, the kinetic energy of EPs has an upper limit too, which decreases as the critical height increases. (3) Stable prominences are generally longer and heavier than DPs, and not higher than 0.4 R{sub Sun }. (4) About 62% of the EPs were associated with coronal mass ejections (CMEs); but there is no difference in apparent properties between EPs associated with CMEs and those that are not.

  8. An Analysis of A Tornado-Like Prominence Observed by SDO

    NASA Astrophysics Data System (ADS)

    Wang, W.

    2015-12-01

    We studied a tornado-like prominence near the Northwest limb, observed on 2014 November 1 by the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamic Observatory (SDO). Starting at 02:00 UT, the prominence began to rise slowly. About two hours later, we observed tornado-like horizontal motions as high as 150 Mm above the limb, which were associated with the heating of the dark prominence into brightening material in AIA 17.1 nm. Interactions between the prominence and the overlying coronal loops resulted in the downflows of the prominence material along the loops back to the solar surface, with the landing sites of the downflowing material moving sequentially away from the prominence channel. This could result from magnetic reconnections between the prominence field and the overlying field, which proceeded to higher and higher altitudes when the reconnections encroached into the overlying field. Helical motions at low altitudes are interpreted as flows along the twisted field that supported the prominence against the gravity in its quiescent state. A localized flux emergence within a nearby active region is considered as the trigger the tornado.

  9. On the Structure and Evolution of a Polar Crown Prominence/Filament System

    NASA Astrophysics Data System (ADS)

    Panesar, N. K.; Innes, D. E.; Schmit, D. J.; Tiwari, S. K.

    2014-08-01

    Polar crown prominences, that partially circle the Sun's poles between 60° and 70° latitude, are made of chromospheric plasma. We aim to diagnose the 3D dynamics of a polar crown prominence using high-cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304, 171, and 193 Å and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195 Å. Using time series across specific structures, we compare flows across the disk in 195 Å with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns that are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171 Å two-colour images. We also observe intermittent but repetitious flows with velocity 15 km s-1 in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament-linkage model.

  10. Prominence fine-structure dynamics as inferred from 2D non-LTE models

    NASA Astrophysics Data System (ADS)

    Gunar, Stanislav; Schmieder, Brigitte; Mein, Pierre; Heinzel, Petr

    2012-07-01

    2D multi-thread prominence fine structure models are able to produce synthetic Lyman spectra in very good agreement with spectral observations by SOHO/SUMER including the spectral line asymmetries. The synthetic differential emission measure curves derived from these models are also in a good agreement with observations. Now we show that these models are also able to produce synthetic H-alpha line profiles in very good agreement with observations which allows us to analyze not only the physical parameters of the prominence fine-structure plasma but also some aspects of its dynamical behaviour. We compare the synthetic H-alpha spectra with the observed spectra of the April 26, 2007 prominence using three statistical parameters: the line integrated intensity, the line full-width at the half-maximum (FWHM), and the Doppler velocity derived from shifts of the line profiles. This statistical analysis allows us to conclude that the overall statistical distribution of the LOS velocities in the April 26, 2007 prominence at the time of the observations was below +/-15 km/s and in the prominence core was close to +/-10 km/s. In combination with the analysis of the Lyman spectra we determine several physical parameters of the observed prominence fine structures which show that the April 26, 2007 prominence was relatively less massive. We are also able to put some constrains on the prominence core temperature that might be relatively low, reaching values below 6000 K.

  11. Social Prominence and the Heterogeneity of Rejected Status in Late Elementary School

    ERIC Educational Resources Information Center

    Farmer, Thomas W.; Hall, Cristin M.; Leung, Man-Chi; Estell, David B.; Brooks, Debra

    2011-01-01

    The heterogeneity of peer rejection was examined as a function of social prominence in fifth grade classrooms. From an overall sample of 3,891 (1,931 girls) students, 721 youth (424 boys) were identified with rejected status. Social prominence was determined from the aggregation of peer nominations for "leader", "athletic", "cool", and "popular".…

  12. Physics of Solar Prominences: I—Spectral Diagnostics and Non-LTE Modelling

    NASA Astrophysics Data System (ADS)

    Labrosse, N.; Heinzel, P.; Vial, J.-C.; Kucera, T.; Parenti, S.; Gunár, S.; Schmieder, B.; Kilper, G.

    2010-04-01

    This review paper outlines background information and covers recent advances made via the analysis of spectra and images of prominence plasma and the increased sophistication of non-LTE ( i.e. when there is a departure from Local Thermodynamic Equilibrium) radiative transfer models. We first describe the spectral inversion techniques that have been used to infer the plasma parameters important for the general properties of the prominence plasma in both its cool core and the hotter prominence-corona transition region. We also review studies devoted to the observation of bulk motions of the prominence plasma and to the determination of prominence mass. However, a simple inversion of spectroscopic data usually fails when the lines become optically thick at certain wavelengths. Therefore, complex non-LTE models become necessary. We thus present the basics of non-LTE radiative transfer theory and the associated multi-level radiative transfer problems. The main results of one- and two-dimensional models of the prominences and their fine-structures are presented. We then discuss the energy balance in various prominence models. Finally, we outline the outstanding observational and theoretical questions, and the directions for future progress in our understanding of solar prominences.

  13. Prominence and Cool Loop Energetics Measured in the UV, EUV, and H-alpha

    NASA Technical Reports Server (NTRS)

    Kucera, Therese A.; Landi, E.

    2006-01-01

    We investigate the thermal and dynamic properties of moving features in a prominence jet, a approx. 10(exp 5)K loop near a prominence channel, and an erupting prominence. In order to make measurements of the quickly moving features seen in prominences in the UV we use the SOHO/SUMER spectrograph to take a time series of exposures from a single pointing position, providing a measurement of spectral line properties as a function of time and position along the slit. The lines observed cover a broad range of temperatures from 80,000 - 1.6 million K. These measurements are combined with TRACE movies in transition region and coronal temperature bands and with ground based H-alpha data to obtain more complete information concerning prominence structure and motions. The resulting observations allow us perform DEM analysis and to calculate limits on densities, pressures, and the thermal and kinetic energies of the moving sources.

  14. Prominence Cavity Regions Observed Using SWAP 174 Å Filtergrams and Simultaneous Eclipse Flash Spectra

    NASA Astrophysics Data System (ADS)

    Bazin, C.; Koutchmy, S.; Tavabi, E.

    2013-08-01

    SWAP images from PROBA2 taken at 174 Å in the Fe ix/ x lines are compared with simultaneous slitless flash spectra obtained during the solar total eclipse of 11 July 2010. Myriad faint low-excitation emission lines together with the He i and He ii Paschen α chromospheric lines are recorded on eclipse spectra where regions of limb prominences are obtained with space-borne imagers. We analyzed a deep flash spectrum obtained by summing 80 individual spectra to evaluate the intensity modulations of the continuum. Intensity deficits are observed and measured at the prominences boundaries in both eclipse and SWAP images. The prominence cavities interpreted as a relative depression of plasma density, produced inside the corona surrounding the prominences, and some intense heating occurring in these regions, are discussed. Photometric measurements are shown at different scales and different, spectrally narrow, intervals for both the prominences and the coronal background.

  15. The role of prominence in Spanish sentence comprehension: An ERP study.

    PubMed

    Gattei, Carolina A; Tabullo, Ángel; París, Luis; Wainselboim, Alejandro J

    2015-11-01

    Prominence is the hierarchical relation among arguments that allows us to understand 'Who did what to whom' in a sentence. The present study aimed to provide evidence about the role of prominence information for the incremental interpretation of arguments in Spanish. We investigated the time course of neural correlates associated to the comprehension of sentences that require a reversal of argument prominence hierarchization. We also studied how the amount of available prominence information may affect the incremental build-up of verbal expectations. Results of the ERP data revealed that at the disambiguating verb region, object-initial sentences (only one argument available) elicited a centro-parietal negativity with a peak at 400 ms post-onset. Subject-initial sentences (two arguments available) yielded a broadly distributed positivity at around 650 ms. This dissociation suggests that argument interpretation may depend on their morphosyntactic features, and also on the amount of prominence information available before the verb is encountered. PMID:26291770

  16. Transverse oscillations and stability of prominences in a magnetic field dip

    NASA Astrophysics Data System (ADS)

    Kolotkov, D. Y.; Nisticò, G.; Nakariakov, V. M.

    2016-05-01

    Aims: We developed an analytical model of the global transverse oscillations and mechanical stability of a quiescent prominence in the magnetised environment with a magnetic field dip that accounts for the mirror current effect. Methods: The model is based on the interaction of line currents through the Lorentz force. Within this concept the prominence is treated as a straight current-carrying wire, and the magnetic dip is provided by two photospheric current sources. Results: Properties of both vertical and horizontal oscillations are determined by the value of the prominence current, its density and height above the photosphere, and the parameters of the magnetic dip. The prominence can be stable in both horizontal and vertical directions simultaneously when the prominence current dominates in the system and its height is less than the half-distance between the photospheric sources.

  17. Physics of Solar Prominences: I-Spectral Diagnostics and Non-LTE Modelling

    NASA Technical Reports Server (NTRS)

    Labrosse, N.; Heinzel, P.; Vial, J.-C,; Kucera, T.; Parenti, S.; Gunar, S.; Schmieder, B.; Kilper, G.

    2010-01-01

    This review paper outlines background information and covers recent advances made via the analysis of spectra and images of prominence plasma and the increased sophistication of non-LTE (i.e. when there is a departure from Local Thermodynamic Equilibrium) radiative transfer models. We first describe the spectral inversion techniques that have been used to infer the plasma parameters important for the general properties of the prominence plasma in both its cool core and the hotter prominence-corona transition region. We also review studies devoted to the observation of bulk motions of the prominence plasma and to the determination of prominence mass. However, a simple inversion of spectroscopic data usually fails when the lines become optically thick at certain wavelengths. Therefore, complex

  18. On the Visibility of Solar Prominences in SDO/AIA Channels

    NASA Astrophysics Data System (ADS)

    Heinzel, P.; Schmieder, B.; Parenti, S.; Golub, L.

    2012-05-01

    Prominences in EUV lines are observed as dark structures over the limb due absorption and emission blocking mechanisms. However, at 171 Å is observed emission in prominences with TRACE and SDO/AIA, and it is believed to be due to the prominence-corona transition region (PCTR) emitting in cool lines. To check this, we use the Differential Emission Measure (DEM) recently obtained for quiescent prominences using SOHO/SUMER spectra (Parenti and Vial 2007) and compute the synthetic spectra in selected AIA channels. We then compare 171 Å and 195 Å channels and derive conclusions concerning the PCTR emissivity, as well well as the absorption and blocking. The emission seen in the 171 Å channel can be used to better constrain prominence DEM curves.

  19. Fabrication of micro-prominences on PTFE surface using proton beam writing

    NASA Astrophysics Data System (ADS)

    Kitamura(Ogawa), Akane; Satoh, Takahiro; Koka, Masashi; Kobayashi, Tomohiro; Kamiya, Tomihiro

    2013-07-01

    Polytetrafluoroethylene (PTFE) is a typical fluoropolymer and it has several desirable technological properties such as electrical insulation, solid lubrication etc. However, the conventional microstructuring methods have not been well applied to PTFE due to its chemical inertness. Some effective micromachining using synchrotron radiation or ion beam irradiation has been reported. In this study, we create micro-prominences by raising the original surface using proton beam writing (PBW) without chemical etching. A conical prominence was formed by spiral drawing from the center with a 3 MeV proton beam. The body was porous, and the bulk PTFE below the prominence changed to fragmented structures. With decreasing writing speed, the prominence became taller but the height peaked. The prominence gradually reduced in size after the speed reached the optimum value. We expect that these porous projections with high aspect ratio will be versatile in medical fields and microelectromechanical systems (MEMS) technology.

  20. Magnetic Structure and Dynamics of the Erupting Solar Polar Crown Prominence on 2012 March 12

    NASA Astrophysics Data System (ADS)

    Su, Yingna; van Ballegooijen, Adriaan; McCauley, Patrick; Ji, Haisheng; Reeves, Katharine K.; DeLuca, Edward E.

    2015-07-01

    We present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA; end-on view) and displays a quasi-vertical thread structure. A bright U-shaped or horn-like structure is observed surrounding the upper portion of the prominence at 171 Å before the eruption and becomes more prominent during the eruption. The disk view of {STEREO}\\_B shows that this long prominence is composed of a series of vertical threads and displays a half-loop-like structure during the eruption. We focus on the magnetic support of the prominence vertical threads by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO_B. We also construct a series of magnetic field models (sheared arcade model, twisted flux rope model, and unstable model with hyperbolic flux tube). Various observational characteristics appear to be in favor of the twisted flux rope model. We find that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast-rise phase, and signatures of reconnection (posteruption arcade, new U-shaped structure, rising blobs) appear about one hour later. During the eruption, AIA observes dark ribbons seen in absorption at 171 Å corresponding to the bright ribbons shown at 304 Å, which might be caused by the erupting filament material falling back along the newly reconfigured magnetic fields. Brightenings at the inner edge of the erupting prominence arcade are also observed in all AIA EUV channels, which might be caused by the heating due to energy released from reconnection below the rising prominence.

  1. Dynamics of quiescent prominences; Proceedings of the 117th Colloquium of IAU, Hvar, Yugoslavia, Sept. 25-29, 1989

    NASA Technical Reports Server (NTRS)

    Ruzdjak, Vladimir (Editor); Tandberg-Hanssen, Einar (Editor)

    1990-01-01

    Topics discussed include formation of a filament around a magnetic region, evolution of fine structures in a filament, the spatial distribution of prominence threads, high resolution analysis of quiescent prominences at NSO/Sacramento Peak Observatory, small-scale Doppler velocities in a quiescent prominence, Doppler velocity oscillations in quiescent prominences, oscillatory relaxation of an eruptive prominence, and matter flow velocities in an active region emission loop observed in H-alpha. Attention is also given to an automated procedure for measurement of prominence transverse velocities, the nonlinear evolution of magnetized filaments, thermal equilibrium of coronal loops and prominence formation, thermal instability in planar coronal strucutres, radiative transfer in cylindrical prominence threads, numerical simulation of a catastrophe model for prominence eruptions, and the law of evolution and destruction of solar prominences.

  2. Analysis of EUV, UV, and H-alpha Emission from Two Very Different Prominences

    NASA Technical Reports Server (NTRS)

    Kucera, T.; Landi, E.

    2008-01-01

    We analyze the properties of a pair of prominences observed the UV and EUV in April 2004. One was a generally quiet prominence which exhibited a period of activation. Another was a large "coronal cloud" type prominence. Both were observed by SOHO/SUMER, TRACE, and in H$\\alpha$ by BBSO and MLSO. The quiet prominence was also observed by the SOHO/CDS instrument. TRACE and H$\\alpha$ data provide 2D images on with time cadences on the order of 1 minute. The SUMER data was taken from a single slit location with a 90 second cadence and included a number of lines spanning the temperature range 80,000 to 1.6 million K. This observing program was designed to allow us to study prominence dynamics . CDS raster data was taken with a slower cadence, in lines formed at temperatures from 20,000 - 1 million K. We combine these different data sets to analyze the thermal properties, including differential emission measures (DEMs), of these very different prominences, and compare the results to those of prominences previously analyzed by ourselves and others.

  3. Multiple-Thread Model of a Prominence Observed by SUMER and EIT on SOHO

    NASA Astrophysics Data System (ADS)

    Wiik, J. E.; Dammasch, I. E.; Schmieder, B.; Wilhelm, K.

    1999-07-01

    A quiescent polar crown prominence was observed at Meudon in Hα and Ca ii lines, and by EIT and SUMER on board SOHO in UV lines from 9 to 10 March 1996. SUMER observed the prominence continuously in a scanning mode between 21:40 UT on 9 March, and 18:13 UT on 10 March, in the nitrogen line N v (λ1238) with a 1 arc sec2 resolution. Altogether 190 prominence images (121×108 pixels) were obtained. These are presented in a movie. The prominence is highly dynamic. Large-scale features, such as mixed loop systems and dark cavities are changing on time scales of a few hours. Filamentary structure is evident and is changing within a few frames of the movie. A lifetime of 20 25 min for the fine structure has been found by the autocorrelation method. We have statistically analysed the three moments of the N v line in the prominence: line intensity, Doppler shift and linewidth, in the context of a multiple-thread model. We find that the data are consistent with a model where the prominence is assumed to be an ensemble of small threads. In the brightest parts of the prominence it is possible that there are many unresolved threads (15 20) along the line of sight with diameters smaller than a few hundred kilometers. The filling factor is probably very small and in that case the structures occupy only a fraction of the volume.

  4. Observation of the prominence cavity region using slitless eclipse flash spectra and space borne EUV filtergrams

    NASA Astrophysics Data System (ADS)

    Bazin, Cyrille; Koutchmy, Serge; Lamy, Philippe; Tavabi, Ehsan

    2014-01-01

    We used total solar eclipse free of parasitic light for studying the prominence to corona interface, and the corresponding cavity in the context of the coronal physics. We analysed the visible continuum between the prominences to directly look at the electron density. We demonstrate some enhanced heating in the cavity region. Some similarities with the interface regions are shown: the photosphere to the chromosphere and the prominence to the corona interface. The optically thin neutral Helium at 4713 Å and the singly ionized Helium 4686 Å Paschen α lines are considered. We summed 80 slitless visible eclipse flash spectra that we compare with simultaneously obtained EUV SWAP/Proba2 174 Å images of ESA and AIA/SDO 171Å 193 Å 304 Å and 131 Å filtergrams. Intensity profiles in a radial direction are studied. We deduce the variation of the intensity ratio I(He I 4713) / I(He II 4686). Discussion: the temperature rises at the edge of the prominences. We evaluate for the first time with spectrophotometric accuracy the continuum modulations in prominence spectra. W-L intensity deficits are observed near the prominence boundaries in both eclipse spectra and in EUV images, confirming that the prominence -cavity regions correspond to a relative depression of plasma density of the surrounding corona. Conclusion: we demonstrate some enhanced heating occurring in these regions assuming hydrostatic equilibrium.

  5. Prominence plasma and magnetic field structure - A coordinated observation with IRIS, Hinode and THEMIS

    NASA Astrophysics Data System (ADS)

    Schmieder, Brigitte; Labrosse, Nicolas; Levens, Peter; Lopez Ariste, Arturo

    2016-07-01

    During an international campaign in 2014, utilising both space-based (IRIS and Hinode) and ground-based (THEMIS) instruments, we focused on observing prominences. We compare IRIS observations with those of Hinode (EIS and SOT) in order to build a more complete picture of the prominence structure for a quiescent prominence observed on 15 July 2014, identified to have tornado-like structure. THEMIS provides valuable information on the orientation and strength of the internal magnetic field. Here we find there is almost ubiquitously horizontal field with respect to the local limb, with possibly a turbulent component. The Mg II lines form the majority of our IRIS analysis, with a mixture of reversed and non-reversed profiles present in the prominence spectra. Comparing the differences between the Mg II data from IRIS and the Ca II images from Hinode/SOT provides an intriguing insight into the prominence legs in these channels. We present plasma diagnostics from IRIS, with line of sight velocities of around 10 km/s in either direction along the magnetic loops of material in the front of the prominence, and line widths comparable to those found for prominences by previous authors (e.g. Schmieder et al. 2014). We also take a look into the lines formed at higher, coronal plasma temperatures, as seen by Hinode/EIS, to compare plasma structures at a full range of temperatures.

  6. Unusual Migration of Prominence Activities in the Southern Hemisphere during Cycles 23-24

    NASA Astrophysics Data System (ADS)

    Shimojo, Masumi

    2013-12-01

    The solar activity in Cycles 23-24 shows differences from the previous cycles that were observed with modern instruments, e.g., long cycle duration and a small number of sunspots. To appreciate the anomalies further, we investigated the prominence eruptions and disappearances observed with the Nobeyama Radioheliograph for over 20 years. Consequently, we found that the occurrence of prominence activities in the northern hemisphere is normal because the period of the number variation is 11 years, and the migration of the producing region of the prominence activities traces the migration of 11 years ago. On the other hand, the migration in the southern hemisphere significantly differs from that in the northern hemisphere and the previous cycles. The prominence activities occurred over -50° latitude in spite of the late decay phase of Cycle 23, and the number of prominence activities in the higher latitude region (over -65°) is very small, even near the solar maximum of Cycle 24. The results suggest that the anomalies of the global magnetic field distribution started at the solar maximum of Cycle 23. A comparison of the butterfly diagram of the prominence activities with the magnetic butterfly diagram indicates that the timing of "the rush to the pole" and the polar magnetic field closely relates to unusual migration. Considering that the rush to the pole is made of the sunspots, the hemispheric asymmetry of the sunspots and the strength of the polar magnetic fields are essential for understanding the anomalies of the prominence activities.

  7. Motions in Prominence Barbs as observed by Hinode/SOT and IRIS

    NASA Astrophysics Data System (ADS)

    Kucera, Therese A.; Ofman, Leon; Tarbell, Theodore D.

    2016-05-01

    We discuss observations of prominence barb dynamics as observed by Hinode/SOT and IRIS. Prominence barbs extend outwards to the side of the main prominence spine and downwards towards the chromosphere. Their properties, including the structure of their magnetic field and the nature of the motions observed in them are a subject of current debate. We use a combination of high cadence, high resolution imaging, H-alpha Doppler, and Mg II line profile data to analyze and understand waves and flows in barbs and discuss their ramifications in terms of a model of the barb magnetic field as collection of dipped field lines.

  8. Monster Prominence

    NASA Video Gallery

    When a rather large-sized (M 3.6 class) flare occurred near the edge of the Sun, it blew out a gorgeous, waving mass of erupting plasma that swirled and twisted over a 90-minute period (Feb. 24, 20...

  9. Onset of solar flares as predicted by two-dimensional MHD-models of quiescent prominences

    NASA Technical Reports Server (NTRS)

    Galindotrejo, J.

    1985-01-01

    The close connection between the sudden disapperance (disparition brusque) of the quiescent prominences and the two-ribbon flares are well known. During this dynamic phase the prominence ascends rapidly (typically with a velocity about 100 Km/sec) and disappears. In another later stage is observed material falling back into the chromosphere. The impact of this downfalling matter on the chromosphere produces the H brightening, which shows the symmetric double pattern. The occurence of the disparition brusque is thought to be a consequence of a plasma instability of magnetohydrostatic (MHD) structures. By means of the MHD-energy principle, the stability properties of four prominence models are analyzed. It is shown that all considered models undergo instabilities for parameters outside of the observed range at quiescent prominences. The possibility that such instabilities in the flare parameter range may indicate just the onset of a flare is considered.

  10. Hinode SOT observations of plume upflows and cascading downflows in quiescent solar prominences

    NASA Astrophysics Data System (ADS)

    Berger, T.; Shine, R.; Slater, G.; Tarbell, T.; Title, A.; Lites, B.; Tsuneta, S.; Okamoto, T. J.; Ichimoto, K.; Katsukawa, Y.; Sekii, T.; Suematsu, Y.; Shimizu, T.

    2007-12-01

    We present several Hinode SOT filtergram movies of quiescent solar prominences that show newly discovered "plume-like" upflows and cascading "waterfall-like" downflows that persist for the entire multi-hour duration of the observations. The flow speeds are on the order of 10 km/sec with typical widths of 400-700 km. Preliminary calculations show that if the upflows are buoyancy driven, the associated thermal perturbation is on the order of 10,000 K, sufficient to explain the dark appearance of the upflows in the interference filter passbands. In addition we observe rotational vortices and body oscillations within the prominences. These new observations challenge current magnetostatic models of solar prominences by showing that prominence plasmas are in constant motion, often in directions perpendicular to the magnetic field lines proposed by the models. TRACE, Hinode/EIS, and Hinode/XRT observations are used to investigate the differential topology of the flows across temperature regimes.

  11. Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. I. Turbulent Upflow Plumes

    NASA Astrophysics Data System (ADS)

    Berger, Thomas E.; Slater, Gregory; Hurlburt, Neal; Shine, Richard; Tarbell, Theodore; Title, Alan; Lites, Bruce W.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Magara, Tetsuya; Suematsu, Yoshinori; Shimizu, Toshifumi

    2010-06-01

    Hinode/Solar Optical Telescope (SOT) observations reveal two new dynamic modes in quiescent solar prominences: large-scale (20-50 Mm) "arches" or "bubbles" that "inflate" from below into prominences, and smaller-scale (2-6 Mm) dark turbulent upflows. These novel dynamics are related in that they are always dark in visible-light spectral bands, they rise through the bright prominence emission with approximately constant speeds, and the small-scale upflows are sometimes observed to emanate from the top of the larger bubbles. Here we present detailed kinematic measurements of the small-scale turbulent upflows seen in several prominences in the SOT database. The dark upflows typically initiate vertically from 5 to 10 Mm wide dark cavities between the bottom of the prominence and the top of the chromospheric spicule layer. Small perturbations on the order of 1 Mm or less in size grow on the upper boundaries of cavities to generate plumes up to 4-6 Mm across at their largest widths. All plumes develop highly turbulent profiles, including occasional Kelvin-Helmholtz vortex "roll-up" of the leading edge. The flows typically rise 10-15 Mm before decelerating to equilibrium. We measure the flowfield characteristics with a manual tracing method and with the Nonlinear Affine Velocity Estimator (NAVE) "optical flow" code to derive velocity, acceleration, lifetime, and height data for several representative plumes. Maximum initial speeds are in the range of 20-30 km s-1, which is supersonic for a ~10,000 K plasma. The plumes decelerate in the final few Mm of their trajectories resulting in mean ascent speeds of 13-17 km s-1. Typical lifetimes range from 300 to 1000 s (~5-15 minutes). The area growth rate of the plumes (observed as two-dimensional objects in the plane of the sky) is initially linear and ranges from 20,000 to 30,000 km2 s-1 reaching maximum projected areas from 2 to 15 Mm2. Maximum contrast of the dark flows relative to the bright prominence plasma in SOT images

  12. The ecology of prominences. [classification, morphology and significance to solar physics

    NASA Technical Reports Server (NTRS)

    Zirin, H.

    1979-01-01

    The paper discusses the roles of prominences in the solar scheme. Attention is given to classifications and the ways in which prominences exist: hydrostatic support, ballistic support, and magnetic support. In the case of ballistic support, surges are differentiated from sprays which involve the ejection of material that is already above the solar surface. Discussion also covers filimets and fibrils and the conditions for their appearance. It is proposed that most flares originate in prominence instabilities. In addition supergranulation is covered, noting the network is not seen on the boundary of unipolar regions. It is concluded that prominences play a critical role in flares and field reconnection, and the evolution of solar magnetic fields.

  13. Morphology Of A Hot Prominence Cavity Observed with Hinode/XRT and SDO/AIA

    NASA Technical Reports Server (NTRS)

    Weber, Mark A.; Reeves, K. K.; Gibson, S. E.; Kucera, T. A.

    2012-01-01

    Prominence cavities appear as circularly shaped voids in coronal emission over polarity inversion lines where a prominence channel is straddling the solar limb. The presence of chromospheric material suspended at coronal altitudes is a common but not necessary feature within these cavities. These voids are observed to change shape as a prominence feature rotates around the limb. We use a morphological model projected in cross-sections to fit the cavity emission in Hinode/XRT passbands, and then apply temperature diagnostics to XRT and SDO/AIA data to investigate the thermal structure. We find significant evidence that the prominence cavity is hotter than the corona immediately outside the cavity boundary. This investigation follows upon "Thermal Properties of A Solar Coronal Cavity Observed with the X-ray Telescope on Hinode" by Reeves et al., 2012, ApJ, in press.

  14. QUIESCENT PROMINENCE DYNAMICS OBSERVED WITH THE HINODE SOLAR OPTICAL TELESCOPE. I. TURBULENT UPFLOW PLUMES

    SciTech Connect

    Berger, Thomas E.; Slater, Gregory; Hurlburt, Neal; Shine, Richard; Tarbell, Theodore; Title, Alan; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Magara, Tetsuya; Suematsu, Yoshinori; Shimizu, Toshifumi

    2010-06-20

    Hinode/Solar Optical Telescope (SOT) observations reveal two new dynamic modes in quiescent solar prominences: large-scale (20-50 Mm) 'arches' or 'bubbles' that 'inflate' from below into prominences, and smaller-scale (2-6 Mm) dark turbulent upflows. These novel dynamics are related in that they are always dark in visible-light spectral bands, they rise through the bright prominence emission with approximately constant speeds, and the small-scale upflows are sometimes observed to emanate from the top of the larger bubbles. Here we present detailed kinematic measurements of the small-scale turbulent upflows seen in several prominences in the SOT database. The dark upflows typically initiate vertically from 5 to 10 Mm wide dark cavities between the bottom of the prominence and the top of the chromospheric spicule layer. Small perturbations on the order of 1 Mm or less in size grow on the upper boundaries of cavities to generate plumes up to 4-6 Mm across at their largest widths. All plumes develop highly turbulent profiles, including occasional Kelvin-Helmholtz vortex 'roll-up' of the leading edge. The flows typically rise 10-15 Mm before decelerating to equilibrium. We measure the flowfield characteristics with a manual tracing method and with the Nonlinear Affine Velocity Estimator (NAVE) 'optical flow' code to derive velocity, acceleration, lifetime, and height data for several representative plumes. Maximum initial speeds are in the range of 20-30 km s{sup -1}, which is supersonic for a {approx}10,000 K plasma. The plumes decelerate in the final few Mm of their trajectories resulting in mean ascent speeds of 13-17 km s{sup -1}. Typical lifetimes range from 300 to 1000 s ({approx}5-15 minutes). The area growth rate of the plumes (observed as two-dimensional objects in the plane of the sky) is initially linear and ranges from 20,000 to 30,000 km{sup 2} s{sup -1} reaching maximum projected areas from 2 to 15 Mm{sup 2}. Maximum contrast of the dark flows relative to

  15. The Causal Ordering of Prominence and Salience in Identity Theory: An Empirical Examination

    PubMed Central

    Brenner, Philip S.; Serpe, Richard T.; Stryker, Sheldon

    2016-01-01

    Identity theory invokes two distinct but related concepts, identity salience and prominence, to explain how the organization of identities that make up the self impacts the probability that a given identity is situationally enacted. However, much extant research has failed to clearly distinguish between salience and prominence, and their empirical relationship has not been adequately investigated, impeding a solid understanding of the significance and role of each in a general theory of the self. This study examines their causal ordering using three waves of panel data from 48 universities focusing on respondents’ identities as science students. Analyses strongly support a causal ordering from prominence to salience. We provide theoretical and empirical grounds to justify this ordering while acknowledging potential variation in its strength across identities. Finally, we offer recommendations about the use of prominence and salience when measures of one or both are available or when analyses use cross-sectional data. PMID:27284212

  16. Time-resolved diffused optical characterization of key tissue constituents of human bony prominence locations

    NASA Astrophysics Data System (ADS)

    Konugolu Venkata Sekar, Sanathana; Farina, Andrea; Martinenghi, Edoardo; Dalla Mora, Alberto; Taroni, Paola; Pifferi, Antonio; Negredo, Eugènia; Puig, Jordi; Escrig, Roser; Rosales, Quim; Lindner, Claus; Pagliazzi, Marco; Durduran, Turgut

    2015-07-01

    We report a broadband time-resolved characterization of selected bony prominence locations of the human body. A clinical study was performed at six different bony prominence locations of 53 subjects. A portable broadband time-resolved system equipped with pulse drift and distortion compensation strategy was used for absorption and scattering measurements. Key tissue constituents were quantified as a pilot step towards non-invasive optical assessment of bone pathologies.

  17. Prominence activity related to CME observed by SOHO, Yohkoh and ground-based observatories

    NASA Technical Reports Server (NTRS)

    Schmieder, B.; vanDriel-Gesztelyi, L.; Wiik, J. E.; Kucera, T.; Thompson, B.; DeForest, C.; SaintCyr, C.; Simnett, G. M.

    1997-01-01

    Examples of destabilization of prominences and their associated coronal mass ejections (CMEs) are presented. During the 1996 campaigns of multi-wavelength observations with the Solar and Heliospheric Observatory (SOHO), the Yohkoh satellite's soft X-ray telescope (SXT) and the Meudon (France) H alpha spectroheliograph eruptive solar filaments and prominences associated with the CMEs were observed. Two of the observed events showed that CMEs and 'brusques disparitions' (BDs) seem to be consequences of global magnetic field instability.

  18. Dynamics of a Prominence-horn Structure during Its Evaporation in the Solar Corona

    NASA Astrophysics Data System (ADS)

    Wang, Bing; Chen, Yao; Fu, Jie; Li, Bo; Li, Xing; Liu, Wei

    2016-08-01

    The physical connections among and formation mechanisms of various components of the prominence-horn cavity system remain elusive. Here we present observations of such a system, focusing on a section of the prominence that rises and separates gradually from the main body. This forms a configuration sufficiently simple to yield clues regarding the above issues. It is characterized by embedding horns, oscillations, and a gradual disappearance of the separated material. The prominence-horn structure exhibits a large-amplitude longitudinal oscillation with a period of ∼150 minutes and an amplitude of ∼30 Mm along the trajectory defined by the concave horn structure. The horns also experience a simultaneous transverse oscillation with a much smaller amplitude (∼3 Mm) and a shorter period (∼10–15 minutes), likely representative of a global mode of the large-scale magnetic structure. The gradual disappearance of the structure indicates that the horn, an observational manifestation of the field-aligned transition region separating the cool and dense prominence from the hot and tenuous corona, is formed due to the heating and diluting process of the central prominence mass; most previous studies suggested that it is the opposite process, i.e., the cooling and condensation of coronal plasmas, that formed the horn. This study also demonstrates how the prominence transports magnetic flux to the upper corona, a process essential for the gradual build-up of pre-eruption magnetic energy.

  19. EVIDENCE FOR ROTATIONAL MOTIONS IN THE FEET OF A QUIESCENT SOLAR PROMINENCE

    SciTech Connect

    Orozco Suarez, D.; Asensio Ramos, A.; Trujillo Bueno, J.

    2012-12-20

    We present observational evidence of apparent plasma rotational motions in the feet of a solar prominence. Our study is based on spectroscopic observations taken in the He I 1083.0 nm multiplet with the Tenerife Infrared Polarimeter attached to the German Vacuum Tower Telescope. We recorded a time sequence of spectra with 34 s cadence placing the slit of the spectrograph almost parallel to the solar limb and crossing two feet of an intermediate size, quiescent hedgerow prominence. The data show opposite Doppler shifts, {+-}6 km s{sup -1}, at the edges of the prominence feet. We argue that these shifts may be interpreted as prominence plasma rotating counterclockwise around the vertical axis to the solar surface as viewed from above. The evolution of the prominence seen in EUV images taken with the Solar Dynamics Observatory provided us with clues to interpret the results as swirling motions. Moreover, time-distance images taken far from the central wavelength show plasma structures moving parallel to the solar limb with velocities of about 10-15 km s{sup -1}. Finally, the shapes of the observed intensity profiles suggest the presence of, at least, two components at some locations at the edges of the prominence feet. One of them is typically Doppler shifted (up to {approx}20 km s{sup -1}) with respect to the other, thus suggesting the existence of supersonic counter-streaming flows along the line of sight.

  20. SOLAR LIMB PROMINENCE CATCHER AND TRACKER (SLIPCAT): AN AUTOMATED SYSTEM AND ITS PRELIMINARY STATISTICAL RESULTS

    SciTech Connect

    Wang Yuming; Cao Hao; Chen Junhong; Zhang Tengfei; Yu Sijie; Zheng Huinan; Shen Chenglong; Wang, S.; Zhang Jie

    2010-07-10

    In this paper, we present an automated system, which has the capability to catch and track solar limb prominences based on observations from the extreme-ultraviolet (EUV) 304 A passband. The characteristic parameters and their evolution, including height, position angle, area, length, and brightness, are obtained without manual interventions. By applying the system to the STEREO-B/SECCHI/EUVI 304 A data during 2007 April-2009 October, we obtain a total of 9477 well-tracked prominences and a catalog of these events available online. A detailed analysis of these prominences suggests that the system has a rather good performance. We have obtained several interesting statistical results based on the catalog. Most prominences appear below the latitude of 60{sup 0} and at the height of about 26 Mm above the solar surface. Most of them are quite stable during the period they are tracked. Nevertheless, some prominences have an upward speed of more than 100 km s{sup -1}, and some others show significant downward and/or azimuthal speeds. There are strong correlations among the brightness, area, and height. The expansion of a prominence is probably one major cause of its fading during the rising or erupting process.

  1. Prominence Bubbles and Plumes: Thermo-magnetic Buoyancy in Coronal Cavity Systems

    NASA Astrophysics Data System (ADS)

    Berger, Thomas; Hurlburt, N.

    2009-05-01

    The Hinode/Solar Optical Telescope continues to produce high spatial and temporal resolution images of solar prominences in both the Ca II 396.8 nm H-line and the H-alpha 656.3 nm line. Time series of these images show that many quiescent prominences produce large scale (50 Mm) dark "bubbles" that "inflate" into, and sometimes burst through, the prominence material. In addition, small-scale (2--5 Mm) dark plumes are seen rising into many quiescent prominences. We show typical examples of both phenomena and argue that they originate from the same mechanism: concentrated and heated magnetic flux that rises due to thermal and magnetic buoyancy to equilibrium heights in the prominence/coronal-cavity system. More generally, these bubbles and upflows offer a source of both magnetic flux and mass to the overlying coronal cavity, supporting B.C. Low's theory of CME initiation via steadily increasing magnetic buoyancy breaking through the overlying helmut streamer tension forces. Quiescent prominences are thus seen as the lowermost parts of the larger coronal cavity system, revealing through thermal effects both the cooled downflowing "drainage" from the cavity and the heated upflowing magnetic "plasmoids" supplying the cavity. We compare SOT movies to new 3D compressible MHD simulations that reproduce the dark turbulent plume dynamics to establish the magnetic and thermal character of these buoyancy-driven flows into the corona.

  2. Solar Magnetized Tornadoes: Rotational Motion in a Tornado-like Prominence

    NASA Astrophysics Data System (ADS)

    Su, Yang; Gömöry, Peter; Veronig, Astrid; Temmer, Manuela; Wang, Tongjiang; Vanninathan, Kamalam; Gan, Weiqun; Li, YouPing

    2014-04-01

    Su et al. proposed a new explanation for filament formation and eruption, where filament barbs are rotating magnetic structures driven by underlying vortices on the surface. Such structures have been noticed as tornado-like prominences when they appear above the limb. They may play a key role as the source of plasma and twist in filaments. However, no observations have successfully distinguished rotational motion of the magnetic structures in tornado-like prominences from other motions such as oscillation and counter-streaming plasma flows. Here we report evidence of rotational motions in a tornado-like prominence. The spectroscopic observations in two coronal lines were obtained from a specifically designed Hinode/EIS observing program. The data revealed the existence of both cold and million-degree-hot plasma in the prominence leg, supporting the so-called prominence-corona transition region. The opposite velocities at the two sides of the prominence and their persistent time evolution, together with the periodic motions evident in SDO/AIA dark structures, indicate a rotational motion of both cold and hot plasma with a speed of ~5 km s-1.

  3. Dynamics of a Prominence-horn Structure during Its Evaporation in the Solar Corona

    NASA Astrophysics Data System (ADS)

    Wang, Bing; Chen, Yao; Fu, Jie; Li, Bo; Li, Xing; Liu, Wei

    2016-08-01

    The physical connections among and formation mechanisms of various components of the prominence-horn cavity system remain elusive. Here we present observations of such a system, focusing on a section of the prominence that rises and separates gradually from the main body. This forms a configuration sufficiently simple to yield clues regarding the above issues. It is characterized by embedding horns, oscillations, and a gradual disappearance of the separated material. The prominence-horn structure exhibits a large-amplitude longitudinal oscillation with a period of ˜150 minutes and an amplitude of ˜30 Mm along the trajectory defined by the concave horn structure. The horns also experience a simultaneous transverse oscillation with a much smaller amplitude (˜3 Mm) and a shorter period (˜10–15 minutes), likely representative of a global mode of the large-scale magnetic structure. The gradual disappearance of the structure indicates that the horn, an observational manifestation of the field-aligned transition region separating the cool and dense prominence from the hot and tenuous corona, is formed due to the heating and diluting process of the central prominence mass; most previous studies suggested that it is the opposite process, i.e., the cooling and condensation of coronal plasmas, that formed the horn. This study also demonstrates how the prominence transports magnetic flux to the upper corona, a process essential for the gradual build-up of pre-eruption magnetic energy.

  4. Locality interactions with prominence in determining the scope of phrasal lengthening

    PubMed Central

    Byrd, Dani; Riggs, Daylen

    2009-01-01

    Temporal lengthening of gestures and segments located in a boundary-adjacent syllable has been found in both pre- and postboundary contexts. However, the temporal extent or scope of this lengthening, particularly in the articulatory domain, is not well described. We address the question of scope of prosodic lengthening by considering specifically whether prominence interacts with boundary-related articulatory lengthening in such a way that prominent elements not immediately at a phrase edge are lengthened relative to the same prominent elements phrase-medially (i.e. at a considerable distance from a boundary). Articulatory kinematic data were collected for three subjects to analyze consonant constrictions of prominent syllables located (1) either immediately before or after a boundary and (2) two and three syllables away from that boundary. The results indicate that, as expected, gestures undergo prosodic lengthening when immediately local to the phase boundary. However, some subjects did display prosodic lengthening at a small remove from the boundary for a prominent syllable. This effect was strongest in the postboundary condition. These results suggest that a consideration of prominence may be relevant in understanding the temporal patterning of boundary-related articulatory lengthening. PMID:19888443

  5. SOLAR MAGNETIZED TORNADOES: ROTATIONAL MOTION IN A TORNADO-LIKE PROMINENCE

    SciTech Connect

    Su, Yang; Veronig, Astrid; Temmer, Manuela; Vanninathan, Kamalam; Gömöry, Peter; Wang, Tongjiang; Gan, Weiqun; Li, YouPing

    2014-04-10

    Su et al. proposed a new explanation for filament formation and eruption, where filament barbs are rotating magnetic structures driven by underlying vortices on the surface. Such structures have been noticed as tornado-like prominences when they appear above the limb. They may play a key role as the source of plasma and twist in filaments. However, no observations have successfully distinguished rotational motion of the magnetic structures in tornado-like prominences from other motions such as oscillation and counter-streaming plasma flows. Here we report evidence of rotational motions in a tornado-like prominence. The spectroscopic observations in two coronal lines were obtained from a specifically designed Hinode/EIS observing program. The data revealed the existence of both cold and million-degree-hot plasma in the prominence leg, supporting the so-called prominence-corona transition region. The opposite velocities at the two sides of the prominence and their persistent time evolution, together with the periodic motions evident in SDO/AIA dark structures, indicate a rotational motion of both cold and hot plasma with a speed of ∼5 km s{sup –1}.

  6. Eruptive Prominences and Their Impact on the Earth and Our Life

    NASA Astrophysics Data System (ADS)

    Lugaz, Noé

    Following prominence eruptions (see Chap. 16 : Webb, Solar prominences. New York: Springer, 2014), the associated coronal mass ejections (CMEs) propagate into the solar wind and interplanetary medium. While the complex interactions with the magnetic field and plasma in the corona (see Chaps. 15 and 16 : Gopalswamy, Solar prominences. New York: Springer, 2014; Webb, Solar prominences. New York: Springer, 2014) have been observed for decades, it has only been in the last decade that the interaction of CMEs with the interplanetary medium can be directly imaged. As CMEs and prominences impact Earth, Earth's magnetosphere may be disrupted through reconnection and/or compression, resulting in geomagnetic storms. In the most extreme cases, CMEs and prominences may have a global effect on man-made technologies and human beings, especially if they are in space. The conditions in the near-Earth environment directly affected by the Sun and the solar activity are known as space weather and will be discussed here.

  7. Quiescent and Eruptive Prominences at Solar Minimum: A Statistical Study via an Automated Tracking System

    NASA Astrophysics Data System (ADS)

    Loboda, I. P.; Bogachev, S. A.

    2015-07-01

    We employ an automated detection algorithm to perform a global study of solar prominence characteristics. We process four months of TESIS observations in the He II 304Å line taken close to the solar minimum of 2008-2009 and mainly focus on quiescent and quiescent-eruptive prominences. We detect a total of 389 individual features ranging from 25×25 to 150×500 Mm2 in size and obtain distributions of many of their spatial characteristics, such as latitudinal position, height, size, and shape. To study their dynamics, we classify prominences as either stable or eruptive and calculate their average centroid velocities, which are found to rarely exceed 3 km/s. In addition, we give rough estimates of mass and gravitational energy for every detected prominence and use these values to estimate the total mass and gravitational energy of all simultaneously existing prominences (1012 - 1014 kg and 1029 - 1031 erg). Finally, we investigate the form of the gravitational energy spectrum of prominences and derive it to be a power-law of index -1.1 ± 0.2.

  8. Solar Prominences Embedded in Flux Ropes: Morphological Features and Dynamics from 3D MHD Simulations

    NASA Astrophysics Data System (ADS)

    Terradas, J.; Soler, R.; Luna, M.; Oliver, R.; Ballester, J. L.; Wright, A. N.

    2016-04-01

    The temporal evolution of a solar prominence inserted in a three-dimensional magnetic flux rope is investigated numerically. Using the model of Titov & Démoulin under the regime of weak twist, the cold and dense prominence counteracts gravity by modifying the initially force-free magnetic configuration. In some cases a quasi-stationary situation is achieved after the relaxation phase, characterized by the excitation of standing vertical oscillations. These oscillations show a strong attenuation with time produced by the mechanism of continuum damping due to the inhomogeneous transition between the prominence and solar corona. The characteristic period of the vertical oscillations does not depend strongly on the twist of the flux rope. Nonlinearity is responsible for triggering the Kelvin-Helmholtz instability associated with the vertical oscillations and that eventually produces horizontal structures. Contrary to other configurations in which the longitudinal axis of the prominence is permeated by a perpendicular magnetic field, like in unsheared arcades, the orientation of the prominence along the flux rope axis prevents the development of Rayleigh-Taylor instabilities and therefore the appearance of vertical structuring along this axis.

  9. COMPARING SPATIAL DISTRIBUTIONS OF SOLAR PROMINENCE MASS DERIVED FROM CORONAL ABSORPTION

    SciTech Connect

    Gilbert, Holly; Kilper, Gary; Kucera, Therese; Alexander, David

    2011-01-20

    In a previous study, Gilbert et al. derived the column density and total mass of solar prominences using a new technique, which measures how much coronal radiation in the Fe XII (195 A) spectral band is absorbed by prominence material, while considering the effects of both foreground and background radiation. In the present work, we apply this method to a sample of prominence observations in three different wavelength regimes: one in which only H{sup 0} is ionized (504 A < {lambda} < 911 A), a second where both H{sup 0} and He{sup 0} are ionized (228 A < {lambda} < 504 A), and finally at wavelengths where H{sup 0}, He{sup 0}, and He{sup +} are all ionized ({lambda} < 228 A). This approach, first suggested by Kucera et al., permits the separation of the contributions of neutral hydrogen and helium to the total column density in prominences. Additionally, an enhancement of the technique allowed the calculation of the two-dimensional (2D) spatial distribution of the column density from the continuum absorption in each extreme-ultraviolet observation. We find the total prominence mass is consistently lower in the 625 A observations compared to lines in the other wavelength regimes. There is a significant difference in total mass between the 625 A and 195 A lines, indicating the much higher opacity at 625 A is causing a saturation of the continuum absorption and thus, a potentially large underestimation of mass.

  10. Comparing Spatial Distributions of Solar Prominence Mass Derived from Coronal Absorption

    NASA Astrophysics Data System (ADS)

    Gilbert, Holly; Kilper, Gary; Alexander, David; Kucera, Therese

    2011-01-01

    In a previous study, Gilbert et al. derived the column density and total mass of solar prominences using a new technique, which measures how much coronal radiation in the Fe XII (195 Å) spectral band is absorbed by prominence material, while considering the effects of both foreground and background radiation. In the present work, we apply this method to a sample of prominence observations in three different wavelength regimes: one in which only H0 is ionized (504 Å < λ < 911 Å), a second where both H0 and He0 are ionized (228 Å < λ < 504 Å), and finally at wavelengths where H0, He0, and He+ are all ionized (λ < 228 Å). This approach, first suggested by Kucera et al., permits the separation of the contributions of neutral hydrogen and helium to the total column density in prominences. Additionally, an enhancement of the technique allowed the calculation of the two-dimensional (2D) spatial distribution of the column density from the continuum absorption in each extreme-ultraviolet observation. We find the total prominence mass is consistently lower in the 625 Å observations compared to lines in the other wavelength regimes. There is a significant difference in total mass between the 625 Å and 195 Å lines, indicating the much higher opacity at 625 Å is causing a saturation of the continuum absorption and thus, a potentially large underestimation of mass.

  11. Identification of rat lung – prominent genes by a parallel DNA microarray hybridization

    PubMed Central

    Chen, Zhongming; Chen, Jiwang; Weng, Tingting; Jin, Nili; Liu, Lin

    2006-01-01

    Background The comparison of organ transcriptomes is an important strategy for understanding gene functions. In the present study, we attempted to identify lung-prominent genes by comparing the normal transcriptomes of rat lung, heart, kidney, liver, spleen, and brain. To increase the efficiency and reproducibility, we first developed a novel parallel hybridization system, in which 6 samples could be hybridized onto a single slide at the same time. Results We identified the genes prominently expressed in the lung (147) or co-expressed in lung-heart (23), lung-liver (37), lung-spleen (203), and lung-kidney (98). The known functions of the lung-prominent genes mainly fell into 5 categories: ligand binding, signal transducer, cell communication, development, and metabolism. Real-time PCR confirmed 13 lung-prominent genes, including 5 genes that have not been investigated in the lung, vitamin D-dependent calcium binding protein (Calb3), mitogen activated protein kinase 13 (Mapk13), solute carrier family 29 transporters, member 1 (Slc29a1), corticotropin releasing hormone receptor (Crhr1), and lipocalin 2 (Lcn2). Conclusion The lung-prominent genes identified in this study may provide an important clue for further investigation of pulmonary functions. PMID:16533406

  12. Are Tornado-Like Magnetic Structures Able to Support Solar Prominence Plasma?

    NASA Astrophysics Data System (ADS)

    Ogunjo, S. T.; Luna Bennasar, M.; Moreno-Insertis, F.; Priest, E. R.

    2015-12-01

    Recent high-resolution and high-cadence observations have surprisingly suggested that prominence barbs exhibit apparent rotating motions suggestive of a tornado-like structure. Additional evidence has been provided by Doppler measurements. The observations reveal opposite velocities for both hot and cool plasma on the two sides of a prominence barb. This motion is persistent for several hours and has been interpreted in terms of rotational motion of prominence feet. Several authors suggest that such barb motions are rotating helical structures around a vertical axis similar to tornadoes on Earth. One of the difficulties of such a proposal is how to support cool prominence plasma in almost-vertical structures against gravity. In this work we model analytically a tornado-like structure and try to determine possible mechanisms to support the prominence plasma. We have found that the Lorentz force can indeed support the barb plasma provided the magnetic structure is sufficiently twisted and/or significant poloidal flows are present.

  13. Are Tornado-like Magnetic Structures Able to Support Solar Prominence Plasma?

    NASA Astrophysics Data System (ADS)

    Luna, M.; Moreno-Insertis, F.; Priest, E.

    2015-07-01

    Recent high-resolution and high-cadence observations have surprisingly suggested that prominence barbs exhibit apparent rotating motions suggestive of a tornado-like structure. Additional evidence has been provided by Doppler measurements. The observations reveal opposite velocities for both hot and cool plasma on the two sides of a prominence barb. This motion is persistent for several hours and has been interpreted in terms of rotational motion of prominence feet. Several authors suggest that such barb motions are rotating helical structures around a vertical axis similar to tornadoes on Earth. One of the difficulties of such a proposal is how to support cool prominence plasma in almost-vertical structures against gravity. In this work we model analytically a tornado-like structure and try to determine possible mechanisms to support the prominence plasma. We have found that the Lorentz force can indeed support the barb plasma provided the magnetic structure is sufficiently twisted and/or significant poloidal flows are present.

  14. Stereoscopic Analysis of the 31 August 2007 Prominence Eruption and Coronal Mass Ejection

    NASA Astrophysics Data System (ADS)

    Liewer, P. C.; Panasenco, O.; Hall, J. R.

    2013-01-01

    The spectacular prominence eruption and CME of 31 August 2007 are analyzed stereoscopically using data from NASA's twin Solar Terrestrial Relations Observatory (STEREO) spacecraft. The technique of tie pointing and triangulation (T&T) is used to reconstruct the prominence (or filament when seen on the disk) before and during the eruption. For the first time, a filament barb is reconstructed in three-dimensions, confirming that the barb connects the filament spine to the solar surface. The chirality of the filament system is determined from the barb and magnetogram and confirmed by the skew of the loops of the post-eruptive arcade relative to the polarity reversal boundary below. The T&T analysis shows that the filament rotates as it erupts in the direction expected for a filament system of the given chirality. While the prominence begins to rotate in the slow-rise phase, most of the rotation occurs during the fast-rise phase, after formation of the CME begins. The stereoscopic analysis also allows us to analyze the spatial relationships among various features of the eruption including the pre-eruptive filament, the flare ribbons, the erupting prominence, and the cavity of the coronal mass ejection (CME). We find that erupting prominence strands and the CME have different (non-radial) trajectories; we relate the trajectories to the structure of the coronal magnetic fields. The possible cause of the eruption is also discussed.

  15. A Prominence Account of Syllable Reduction in Early Speech Development: The Child's Prosodic Phonology of "Tiger" and "Giraffe."

    ERIC Educational Resources Information Center

    Snow, David

    1998-01-01

    This paper tested a theory of syllable prominence with 11 children (ages 11 to 26 months). The theory proposes that syllable prominence is a product of two orthogonal suprasegmental systems: stress/accent peaks and phrase boundaries. Use of the developed prominence scale found it parsimoniously accounted for observed biases in syllable omissions…

  16. 3D conductive coupling for efficient generation of prominent Fano resonances in metamaterials.

    PubMed

    Liu, Zhiguang; Liu, Zhe; Li, Jiafang; Li, Wuxia; Li, Junjie; Gu, Changzhi; Li, Zhi-Yuan

    2016-01-01

    We demonstrate a 3D conductive coupling mechanism for the efficient generation of prominent and robust Fano resonances in 3D metamaterials (MMs) formed by integrating vertical U-shape split-ring resonators (SRRs) or vertical rectangular plates along a planar metallic hole array with extraordinary optical transmission (EOT). In such a configuration, intensified vertical E-field is induced along the metallic holes and naturally excites the electric resonances of the vertical structures, which form non-radiative "dark" modes. These 3D conductive "dark" modes strongly interfere with the "bright" resonance mode of the EOT structure, generating significant Fano resonances with both prominent destructive and constructive interferences. The demonstrated 3D conductive coupling mechanism is highly universal in that both 3D MMs with vertical SRRs and vertical plates exhibit the same prominent Fano resonances despite their dramatic structural difference, which is conceptually different from conventional capacitive and inductive coupling mechanisms that degraded drastically upon small structural deviations. PMID:27296109

  17. Subcision using a spinal needle cannula and a thread for prominent nasolabial fold correction.

    PubMed

    Lee, Sang-Yeul; Sung, Kun-Yong

    2013-05-01

    Deepening of the nasolabial crease is an esthetically unpleasing aging phenomenon occurring in the midface. Various treatment modalities have been introduced to improve the appearance of prominent nasolabial folds, all of which have pros and cons. Currently, a minimally invasive technique using synthetic dermal fillers is most commonly used. A simple and easy subcision procedure using a wire scalpel has also been used and reported to be effective for prominent nasolabial fold correction, with minimal complications. As an alternative to the wire scalpel, we used a 20-gauge metal type spinal needle cannula (Hakko Co.) and 4-0 Vicryl suture (Ethicon Inc.) for subcision of nasolabial folds. This technique is less expensive than the use of a wire scalpel and easily available when needed. Therefore, on the basis of favorable results, our modified subcision technique may be considered effective for prominent nasolabial fold correction. PMID:23730604

  18. Synthetic Hydrogen Spectra of Oscillating Prominence Slabs Immersed in the Solar Corona

    NASA Astrophysics Data System (ADS)

    Zapiór, M.; Oliver, R.; Ballester, J. L.; Heinzel, P.

    2016-08-01

    We study the behavior of Hα and Hβ spectral lines and their spectral indicators in an oscillating solar prominence slab surrounded by the solar corona, using an MHD model combined with a 1D radiative transfer code taken in the line of sight perpendicular to the slab. We calculate the time variation of the Doppler shift, half-width, and maximum intensity of the Hα and Hβ spectral lines for different modes of oscillation. We find a non-sinusoidal time dependence of some spectral parameters with time. Because Hα and Hβ spectral indicators have different behavior for different modes, caused by differing optical depths of formation and different plasma parameter variations in time and along the slab, they may be used for prominence seismology, especially to derive the internal velocity field in prominences.

  19. IRIS Observations of a Novel, Hybrid Prominence-Coronal Rain Complex

    NASA Astrophysics Data System (ADS)

    Liu, Wei; Antolin, Patrick; Sun, Xudong

    2016-05-01

    Solar prominences and coronal rain are intimately related phenomena, both involving cool material at chromospheric temperatures within the hot corona and both playing important roles as part of the return flow of the chromosphere-corona mass cycle. At the same time, they exhibit distinct morphologies and dynamics not yet well understood. Quiescent prominences consist of numerous long-lasting, filamentary downflow threads, while coronal rain is more transient and falls comparably faster along well-defined curved paths. We report here a novel, hybrid prominence-coronal rain complex in an arcade-fan geometry observed by IRIS and SDO/AIA, which provides new insights to the underlying physics of such contrasting behaviors. We found that the supra-arcade fan region hosts a prominence sheet consisting of meandering threads with broad Mg II k/h line widths. As the prominence material descends to the arcade, it turns into coronal rain sliding down coronal loops with line widths 2-3 times narrower. This contrast suggests that distinct local plasma and magnetic conditions determine the fate of the cool material, a scenario supported by our magnetic field extrapolations from SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar flares; e.g., McKenzie 2013) is likely situated in a current sheet, where the magnetic field is weak and the plasma-beta could be close to unity, thus favoring turbulent flows like those prominence threads. In contrast, the underlying arcade has a stronger magnetic field and most likely a low-beta environment, such that the material is guided along magnetic field lines to appear as coronal rain. We will discuss the implications of these novel results for future observations e.g., with DKIST.

  20. Evidence for a Magnetic Flux Rope in Observations of a Solar Prominence-Cavity System

    NASA Astrophysics Data System (ADS)

    Jibben, Patricia; Reeves, Katharine; Su, Yingna

    2016-03-01

    Coronal cavities are regions of low coronal emission that usually sit above solar prominences. These systems can exist for days or months before erupting. The magnetic structure of the prominence-cavity system during the quiescent period is important to understanding the pre-eruption phase. We describe observations of a coronal cavity situated above a solar prominence observed on the western limb as part of an Interface Region Imaging Spectrograph (IRIS) and Hinode coordinated Observation Program (IHOP 264). During the observation run, an inflow of hot plasma observed by the Hinode X-Ray Telescope (XRT) envelopes the coronal cavity and triggers an eruption of chromospheric plasma near the base of the prominence. During and after the eruption, bright X-ray emission forms within the cavity and above the prominence. IRIS and the Hinode EUV Imaging Spectrometer (EIS) show strong blue shifts in both chromospheric and coronal lines during the eruption. The Hinode Solar Optical Telescope (SOT) Ca II H-line data show bright emission during the ejection with complex, turbulent, flows near the prominence and along the cavity wall. These observations suggest a cylindrical flux rope best represents the cavity structure with the ejected material flowing along magnetic field lines supporting the cavity. We also find evidence for heating of the plasma inside the cavity after the flows. A model of the magnetic structure of the cavity comprised of a weakly twisted flux rope can explain the observed loops in the X-ray and EUV data. Observations from the Coronal Multichannel Polarimeter (CoMP) are compared to predicted models and are inconclusive. We find that more sensitive measurements of the magnetic field strength along the line-of-sight are needed to verify this configuration.

  1. TIME EVOLUTION OF PLASMA PARAMETERS DURING THE RISE OF A SOLAR PROMINENCE INSTABILITY

    SciTech Connect

    Orozco Suárez, D.; Asensio Ramos, A.; Trujillo Bueno, J.; Díaz, A. J.

    2014-04-10

    We present high-spatial resolution spectropolarimetric observations of a quiescent hedgerow prominence taken in the He I 1083.0 nm triplet. The observation consisted of a time series in sit-and-stare mode of ∼36 minutes duration. The spectrograph's slit crossed the prominence body and we recorded the time evolution of individual vertical threads. Eventually, we observed the development of a dark Rayleigh-Taylor plume that propagated upward with a velocity, projected onto the plane of the sky, of 17 km s{sup –1}. Interestingly, the plume apex collided with the prominence threads pushing them aside. We inferred Doppler shifts, Doppler widths, and magnetic field strength variations by interpreting the He I Stokes profiles with the HAZEL code. The Doppler shifts show that clusters of threads move coherently while individual threads have oscillatory patterns. Regarding the plume we found strong redshifts (∼9-12 km s{sup –1}) and large Doppler widths (∼10 km s{sup –1}) at the plume apex when it passed through the prominence body and before it disintegrated. We associate the redshifts with perspective effects while the Doppler widths are more likely due to an increase in the local temperature. No local variations of the magnetic field strength associated with the passage of the plume were found; this leads us to conclude that the plumes are no more magnetized than the surroundings. Finally, we found that some of the threads' oscillations are locally damped, what allowed us to apply prominence seismology techniques to infer additional prominence physical parameters.

  2. Inflammatory Myofibroblastic Tumour of Thyroid with its Prominent Spindle Cell Pattern: A Rare Case Report

    PubMed Central

    Marylilly, S.; Ramya, V.

    2016-01-01

    Inflammatory myofibroblastic tumour of thyroid is very rare. Only 18 cases reported so far. Here we report a case of Inflammatory myofibroblastic tumour with its prominent spindle cell (fibrohistiocytic) pattern in a 61-year-old male patient. The dominant histological pattern in our case was myofibroblastic in contrast to prominent lymphoplasmocytic pattern in other previously reported cases. The tumour was strongly positive for vimentin, Anaplastic lymphoma kinase and showed focal positivity for Smooth Muscle Actin. The patient was treated with total thyroidectomy and he is comfortable after surgery. PMID:27190815

  3. Comparing Spatial Distributions of Solar Prominence Mass Derived from Coronal Absorption

    NASA Technical Reports Server (NTRS)

    Gilbert, Holly; Kilper, Gary; Alexander, David; Kucera, Therese

    2010-01-01

    In the present work we extend the use of this mass-inference technique to a sample of prominences observed in at least two coronal lines. This approach, in theory, allows a direct calculation of prominence mass and helium abundance and how these properties vary spatially and temporally. Our motivation is two-fold: to obtain a He(exp 0)/H(exp 0) abundance ratio, and to determine how the relative spatial distribution of the two species varies in prominences. The first of these relies on the theoretical expectation that the amount of absorption at each EUV wavelength is well-characterized. However, in this work we show that due to a saturation of the continuum absorption in the 625 A and 368 A lines (which have much higher opacity compared to 195 A-) the uncertainties in obtaining the relative abundances are too high to give meaningful estimates. This is an important finding because of its impact on future studies in this area. The comparison of the spatial distribution of helium and hydrogen presented here augments previous observational work indicating that cross-field diffusion of neutrals is an important mechanism for mass loss. Significantly different loss timescales for neutral He and H (helium drains much more rapidly than hydrogen) can impact prominence structure, and both the present and past studies suggest this mechanism is playing a role in structure and possibly dynamics. Section 2 of this paper contains a description of the observations and Section 3 summarizes the method used to infer mass along with the criteria imposed in choosing prominences appropriate for this study. Section 3 also contains a discussion of the problems due to limitations of the available data and the implications for determining relative abundances. We present our results in Section 4, including plots of radial-like scans of prominence mass in different lines to show the spatial distribution of the different species. The last section contains a discussion summarizing the importance

  4. A Novel Presenilin 1 Mutation in Early-Onset Alzheimer's Disease With Prominent Frontal Features.

    PubMed

    Nygaard, Haakon B; Lippa, Carol F; Mehdi, Djekidel; Baehring, Joachim M

    2014-08-01

    Familial Alzheimer's disease (AD) is a rare disorder involving known autosomal dominant mutations in the amyloid precursor protein and presenilin (PSEN) 1 and 2. Here, we present a case of early-onset AD with prominent frontal features associated with a novel deletion of codon 40 in the PSEN1 gene. Serial brain magnetic resonance imaging and(18)F florbetapir imaging show prominent involvement of the frontal lobes, corresponding with the clinical presentation. This case report illustrates a possible link between a novel PSEN1 mutation and frontal variant AD. PMID:24463146

  5. Formation, levitation, and stability of prominences in the magnetized solar atmosphere

    NASA Technical Reports Server (NTRS)

    Drake, J. F.; Mok, Y.; Van Hoven, G.

    1993-01-01

    The dynamic formation of prominences in the initial magnetothermal equilibrium and their stability to sideward displacements are investigated focusing on the structure of the 2D solar atmosphere in the presence of coronal arcades or loops. A model based on 2D magnetohydrodynamic equations takes into account gravity, compressible flows, heating, radiation, anisotropic thermal conduction, and coupling to a deep chromosphere. It is found that prominences in simple arcades characterized by magnetic field with significant curvature at the apex are unstable to a lateral displacement.

  6. Direct Detection of the Helical Magnetic Field Geometry from 3D Reconstruction of Prominence Knot Trajectories

    NASA Astrophysics Data System (ADS)

    Zapiór, Maciej; Martínez-Gómez, David

    2016-02-01

    Based on the data collected by the Vacuum Tower Telescope located in the Teide Observatory in the Canary Islands, we analyzed the three-dimensional (3D) motion of so-called knots in a solar prominence of 2014 June 9. Trajectories of seven knots were reconstructed, giving information of the 3D geometry of the magnetic field. Helical motion was detected. From the equipartition principle, we estimated the lower limit of the magnetic field in the prominence to ≈1-3 G and from the Ampère’s law the lower limit of the electric current to ≈1.2 × 109 A.

  7. On the formation of Mg ii h and k lines in solar prominences

    NASA Astrophysics Data System (ADS)

    Heinzel, P.; Vial, J.-C.; Anzer, U.

    2014-04-01

    Aims: With the recent launch of the IRIS mission, it has become urgent to develop the spectral diagnostics using the Mg ii resonance h and k lines. In this paper, we aim to demonstrate the behavior of these lines under various prominence conditions. Our results serve as a basis for analysis of new IRIS data and for more sophisticated prominence modeling. Methods: For this exploratory work, we use a canonical 1D prominence-slab model, which is isobaric and may have three different temperature structures: isothermal, PCTR-like (prominence-corona transition region), and consistent with the radiative equilibrium. The slabs are illuminated by a realistic incident solar radiation obtained from the UV observations. A five-level plus continuum Mg ii model atom is used to solve the full NLTE problem of the radiative transfer. We use the numerical code based on the ALI techniques and apply the partial frequency redistribution for both Mg ii resonance lines. We also use the velocity-dependent boundary conditions to study the effect of Doppler dimming in the case of moving prominences. Finally, the relaxation technique is used to compute a grid of models in radiative equilibrium. Results: We computed the Mg ii h and k line profiles that are emergent from prominence-slab models and show their dependence on kinetic temperature, gas pressure, geometrical extension, and microturbulent velocity. By increasing the line opacity, significant departures from the complete frequency redistribution take place in the line wings. Models with a PCTR temperature structure show that Mg ii becomes ionized to Mg iii in the temperature range between roughly 15 000 and 30 000 K. Doppler dimming is significant for Mg ii resonance lines. At the velocity 300 km s-1, the line intensity decreases to about 20% of the value for static prominences. Finally, we demonstrate the role of Mg ii h and k radiation losses on the prominence energy balance. Their dominant role is at lower pressures, while the

  8. Three-dimensional prominence-hosting magnetic configurations: Creating a helical magnetic flux rope

    SciTech Connect

    Xia, C.; Keppens, R.; Guo, Y.

    2014-01-10

    The magnetic configuration hosting prominences and their surrounding coronal structure is a key research topic in solar physics. Recent theoretical and observational studies strongly suggest that a helical magnetic flux rope is an essential ingredient to fulfill most of the theoretical and observational requirements for hosting prominences. To understand flux rope formation details and obtain magnetic configurations suitable for future prominence formation studies, we here report on three-dimensional isothermal magnetohydrodynamic simulations including finite gas pressure and gravity. Starting from a magnetohydrostatic corona with a linear force-free bipolar magnetic field, we follow its evolution when introducing vortex flows around the main polarities and converging flows toward the polarity inversion line near the bottom of the corona. The converging flows bring the feet of different loops together at the polarity inversion line, where magnetic reconnection and flux cancellation happen. Inflow and outflow signatures of the magnetic reconnection process are identified, and thereby the newly formed helical loops wind around preexisting ones so that a complete flux rope grows and ascends. When a macroscopic flux rope is formed, we switch off the driving flows and find that the system relaxes to a stable state containing a helical magnetic flux rope embedded in an overlying arcade structure. A major part of the formed flux rope is threaded by dipped field lines that can stably support prominence matter, while the total mass of the flux rope is in the order of 4-5× 10{sup 14} g.

  9. Global and National Prominent Universities: Internationalization, Competitiveness and the Role of the State

    ERIC Educational Resources Information Center

    Horta, Hugo

    2009-01-01

    This article provides a characterization of the internationalization of "global" European universities and discusses the role of the State in promoting greater internationalization and competitiveness levels of prominent national universities. The analysis supports previous arguments stating that global ranking of universities is strongly based on…

  10. Anxiety and Antisocial Behavior: The Moderating Role of Perceptions of Social Prominence among Incarcerated Females

    ERIC Educational Resources Information Center

    Monahan, Kathryn C.; Goldweber, Aska; Meyer, Kristen; Cauffman, Elizabeth

    2012-01-01

    The present study examines how perceptions of social prominence and attitudes toward antisocial behavior among peers moderate the association between anxiety and antisocial behavior among incarcerated females. Latent profile analysis identified two classes of females distinguished by their perceptions and attitudes. Individuals in both classes…

  11. What Happened (and What Didn't): Prominence Promotes Representation of Salient Alternatives in Discourse

    ERIC Educational Resources Information Center

    Fraundorf, Scott

    2012-01-01

    In five experiments, I investigated how readers and listeners generate relevant contrasts in comprehending and remembering discourse. Past work has suggested that prominent words promote encoding of salient alternatives and that this benefits later memory, but it is unclear exactly which alternatives are considered or how consistent these benefits…

  12. The Role of Prominence in Pronoun Resolution: Active versus Passive Representations

    ERIC Educational Resources Information Center

    Foraker, Stephani; McElree, Brian

    2007-01-01

    A prominent antecedent facilitates anaphor resolution. Speed-accuracy tradeoff modeling in Experiments 1 and 3 indicated that clefting did not affect the speed of accessing an antecedent representation, which is inconsistent with claims that discourse-focused information is actively maintained in focal attention [e.g., Gundel, J. K. (1999). "On…

  13. Thermal and Kinetic Properties of Motions in a Prominence Activation and Nearby Loop

    NASA Technical Reports Server (NTRS)

    Kucera, Therese; Landi, E.

    2005-01-01

    We perform a quantitative analysis of the thermal properties of a prominence activation and motions in a nearby loop. In order to make measurements of the quickly moving features seen in prominences in the UV we use the SOHO/SUMER spectrograph to take a time series of exposures from a single pointing position, providing a measurement of spectral line properties as a function of time and position along the slit. The lines observed cover a broad range of temperatures from 80,000 - 1.6 million K. These measurements are combined with TRACE movies in transition region and coronal temperature bands to obtain more complete information concerning prominence structure and motions. The resulting observations allow us to analyze the thermal and kinetic energy of the moving sources as functions of time. The loop and prominence are most apparent in lines formed at temperatures below 250,000 K. We find that in most cases the temperature distribution of plasma in a moving feature changes relatively little over time periods of about 20 minutes.

  14. 21 CFR 501.15 - Animal food; prominence of required statements.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 21 Food and Drugs 6 2013-04-01 2013-04-01 false Animal food; prominence of required statements. 501.15 Section 501.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) ANIMAL DRUGS, FEEDS, AND RELATED PRODUCTS ANIMAL FOOD LABELING General...

  15. 21 CFR 501.15 - Animal food; prominence of required statements.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 21 Food and Drugs 6 2014-04-01 2014-04-01 false Animal food; prominence of required statements. 501.15 Section 501.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) ANIMAL DRUGS, FEEDS, AND RELATED PRODUCTS ANIMAL FOOD LABELING General...

  16. 21 CFR 501.15 - Animal food; prominence of required statements.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 21 Food and Drugs 6 2012-04-01 2012-04-01 false Animal food; prominence of required statements. 501.15 Section 501.15 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) ANIMAL DRUGS, FEEDS, AND RELATED PRODUCTS ANIMAL FOOD LABELING General...

  17. Neighborhood-Level Factors and Youth Violence: Giving Voice to the Perceptions of Prominent Neighborhood Individuals

    ERIC Educational Resources Information Center

    Yonas, Michael A.; O'Campo, Patricia; Burke, Jessica G.; Gielen, Andrea C.

    2007-01-01

    Youth violence is a significant public health problem. Although the relationship between neighborhood-level factors and urban youth violence is recognized, the specific mechanisms of this relationship are often unclear. Prominent neighborhood individuals were identified within four select low-income urban neighborhoods in Baltimore City. In-depth…

  18. 21 CFR 801.15 - Medical devices; prominence of required label statements.

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... 21 Food and Drugs 8 2011-04-01 2011-04-01 false Medical devices; prominence of required label... SERVICES (CONTINUED) MEDICAL DEVICES LABELING General Labeling Provisions § 801.15 Medical devices... information, resulting from the use of label space for any word, statement, design, or device which is...

  19. 21 CFR 801.15 - Medical devices; prominence of required label statements.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... 21 Food and Drugs 8 2010-04-01 2010-04-01 false Medical devices; prominence of required label... SERVICES (CONTINUED) MEDICAL DEVICES LABELING General Labeling Provisions § 801.15 Medical devices... information, resulting from the use of label space for any word, statement, design, or device which is...

  20. Numerous Academics Have Been Duped by a Scam Using Names of Prominent Scholars.

    ERIC Educational Resources Information Center

    Leatherman, Courtney

    1997-01-01

    A convicted criminal, eluding police, has conned dozens of college faculty out of over $200,000 over two years by pretending to be a prominent scholar, calling on colleagues to provide financial assistance to a friend, and offering academic services or personal favors in return. Targeted professors have been in the fields of history, sociology,…

  1. An Empirical Study on Information Prominence Reflected in Sentence Structures of Chinese College EFL Argumentative Writing

    ERIC Educational Resources Information Center

    Ningling, Wei

    2015-01-01

    Prominence, as an important dimension of cognitive construal, refers to the capacity to evoke a certain substructure as the focus of attention, which can be materialized in a variety of semantic and grammatical expressions (Langacker, 1987). Subject of a sentence (Zhang, 2011) and specific sentence structures (Lin, 2013) can bring a substructure…

  2. Kappa-distributions and Temperature Structure of the Prominence-Corona Transition Region

    NASA Astrophysics Data System (ADS)

    Dzifčáková, Elena; Mackovjak, Šimon; Heinzel, Petr

    2014-01-01

    The influence of the electron κ - distributions on the differential emission measure (DEM) of the prominence-corona transition region (PCTR) derived from observed line intensities has been investigated. An important consequence of the κ - distribution is formation of the emission lines in much wider temperature ranges. The implications for the formation temperature of the observed SDO/AIA band emissions are shown.

  3. Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

    NASA Astrophysics Data System (ADS)

    Schwartz, P.; Gunár, S.; Curdt, W.

    2015-05-01

    Aims: We perform a detailed statistical analysis of the spectral Lyman-line observations of the quiescent prominence observed on May 18, 2005. Methods: We used a profile-to-profile comparison of the synthetic Lyman spectra obtained by 2D single-thread prominence fine-structure model as a starting point for a full statistical analysis of the observed Lyman spectra. We employed 2D multi-thread fine-structure models with random positions and line-of-sight velocities of each thread to obtain a statistically significant set of synthetic Lyman-line profiles. We used for the first time multi-thread models composed of non-identical threads and viewed at line-of-sight angles different from perpendicular to the magnetic field. Results: We investigated the plasma properties of the prominence observed with the SoHO/SUMER spectrograph on May 18, 2005 by comparing the histograms of three statistical parameters characterizing the properties of the synthetic and observed line profiles. In this way, the integrated intensity, Lyman decrement ratio, and the ratio of intensity at the central reversal to the average intensity of peaks provided insight into the column mass and the central temperature of the prominence fine structures.

  4. 21 CFR 801.15 - Medical devices; prominence of required label statements.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 21 Food and Drugs 8 2014-04-01 2014-04-01 false Medical devices; prominence of required label... SERVICES (CONTINUED) MEDICAL DEVICES LABELING General Labeling Provisions § 801.15 Medical devices... information, resulting from the use of label space for any word, statement, design, or device which is...

  5. 21 CFR 801.15 - Medical devices; prominence of required label statements.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 21 Food and Drugs 8 2013-04-01 2013-04-01 false Medical devices; prominence of required label... SERVICES (CONTINUED) MEDICAL DEVICES LABELING General Labeling Provisions § 801.15 Medical devices... information, resulting from the use of label space for any word, statement, design, or device which is...

  6. 21 CFR 801.15 - Medical devices; prominence of required label statements.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 21 Food and Drugs 8 2012-04-01 2012-04-01 false Medical devices; prominence of required label... SERVICES (CONTINUED) MEDICAL DEVICES LABELING General Labeling Provisions § 801.15 Medical devices... information, resulting from the use of label space for any word, statement, design, or device which is...

  7. 16 CFR 1500.121 - Labeling requirements; prominence, placement, and conspicuousness.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 16 Commercial Practices 2 2012-01-01 2012-01-01 false Labeling requirements; prominence, placement, and conspicuousness. 1500.121 Section 1500.121 Commercial Practices CONSUMER PRODUCT SAFETY COMMISSION FEDERAL HAZARDOUS SUBSTANCES ACT REGULATIONS HAZARDOUS SUBSTANCES AND ARTICLES; ADMINISTRATION AND ENFORCEMENT REGULATIONS § 1500.121...

  8. From Wilhelm von Humboldt to Hitler-are prominent people more prone to have Parkinson's disease?

    PubMed

    Horowski; Horowski; Calne; Calne

    2000-10-01

    We describe Parkinsonism in prominent people, where Wilhelm von Humboldt and Adolf Hitler provide just two spectacular, opposing examples. In both of them, there is little if any evidence that the disease did influence their life ambitions, methods of achieving them or cognitive function in general. Thus, Hitler's Parkinsonism should remain a 'footnote' to history, and historians should acknowledge that in his last years, his trembling, his curbed posture, his slow walking, mask-like face and low voice did not indicate remorse, fear or depression as a consequence of his crimes, but were mere expressions of his disease which, until the end, had no impact on his intellectual skills and methods. The apparently higher incidence of Parkinsonism in prominent people may be just due to their higher visibility, or a consequence of disease-related personality traits (e.g. ambition, perfectionism, rigidity) which may contribute to becoming, e.g., a prominent authoritarian person. Perhaps even some early behaviour pattern (such as repressed emotions or acting in public-which could even increase the risk of some infection) contributes to a greater vulnerability for developing Parkinsonism. Further studying other prominent cases might lead us to better understanding of risk factors and the expression of early Parkinsonism. PMID:10900395

  9. On the Robustness of the Pendulum Model for Large-amplitude Longitudinal Oscillations in Prominences

    NASA Astrophysics Data System (ADS)

    Luna, M.; Terradas, J.; Khomenko, E.; Collados, M.; de Vicente, A.

    2016-02-01

    Large-amplitude longitudinal oscillations (LALOs) in prominences are spectacular manifestations of solar activity. In such events nearby energetic disturbances induce periodic motions on filaments with displacements comparable to the size of the filaments themselves and with velocities larger than 20 {km} {{{s}}}-1. The pendulum model, in which the gravity projected along a rigid magnetic field is the restoring force, was proposed to explain these events. However, it can be objected that in a realistic situation where the magnetic field reacts to the mass motion of the heavy prominence, the simplified pendulum model could be no longer valid. We have performed nonlinear time-dependent numerical simulations of LALOs considering a dipped magnetic field line structure. In this work we demonstrate that for even relatively weak magnetic fields the pendulum model works very well. We therefore validate the pendulum model and show its robustness, with important implications for prominence seismology purposes. With this model it is possible to infer the geometry of the dipped field lines that support the prominence.

  10. PROMINENCE THREAD SEISMOLOGY USING THE P{sub 1}/2P{sub 2} RATIO

    SciTech Connect

    DIaz, A. J.; Oliver, R.; Ballester, J. L. E-mail: ramon.oliver@uib.e

    2010-12-20

    Prominence threads are expected to be cold plasma condensations in a long magnetic tube. Because of this density inhomogeneity along the magnetic field, the ratio of the fundamental transverse mode period to twice that of its first overtone, P{sub 1}/2P{sub 2}, must differ from 1. We investigate the dependence of this ratio on the equilibrium parameters of prominence threads and its possible use as a diagnostic tool for prominence seismology. Using the low-beta plasma approximation, we follow the procedure of previous works to obtain the frequencies and spatial distribution of the modes. We also check the thin tube approximation and find it reasonably accurate. The period ratio P{sub 1}/2P{sub 2} is found to be greater than unity, in contrast with coronal loops, for which the effect of inhomogeneities is to make this ratio smaller than 1. The ratio is very sensitive to the thread length, while the dependence on other parameters is less important for threads than for coronal loops. Hence, the period ratio can be used to obtain an estimation of the length of the supporting magnetic tube, since the thread length is known from observations. The obtained value of the tube length does not depend on other parameters, so their potential for prominence seismology may be great.

  11. A Qualitative Study of Interference with Communicative Participation across Communication Disorders in Adults

    ERIC Educational Resources Information Center

    Baylor, Carolyn; Burns, Michael; Eadie, Tanya; Britton, Deanna; Yorkston, Kathryn

    2011-01-01

    Purpose: To explore the similarities and differences in self-reported restrictions in communicative participation across different communication disorders in community-dwelling adults. Method: Interviews were conducted with 44 adults representing 7 different medical conditions: spasmodic dysphonia, multiple sclerosis, stroke, stuttering,…

  12. Longitudinal Phonatory Characteristics after Botulinum Toxin Type A Injection.

    ERIC Educational Resources Information Center

    Fisher, Kimberly V.; And Others

    1996-01-01

    A study investigated the long-term effects of a Botulinum Toxin Type A injection on the glottal competency of a man with adductor spasmodic dysphonia. Results suggest that change in degree of glottal adduction over time can be observed even when vocal instability is present within each recording session. (CR)

  13. UNDERSTANDING THE MG II AND Hα SPECTRA IN A HIGHLY DYNAMICAL SOLAR PROMINENCE

    SciTech Connect

    Heinzel, P.; Schmieder, B.; Mein, N.; Gunár, S.

    2015-02-10

    Mg ii h and k and Hα spectra in a dynamical prominence have been obtained along the slit of the Interface Region Imaging Spectrograph (IRIS) and with the Meudon Multi-channel Subtractive Double Pass spectrograph on 2013 September 24, respectively. Single Mg ii line profiles are not much reversed, while at some positions along the IRIS slit the profiles show several discrete peaks that are Doppler-shifted. The intensity of these peaks is generally decreasing with their increasing Doppler shift. We interpret this unusual behavior as being due to the Doppler dimming effect. We discuss the possibility to interpret the unreversed single profiles by using a two-dimensional (2D) model of the entire prominence body with specific radiative boundary conditions. We have performed new 2D isothermal–isobaric modeling of both Hα and Mg ii lines and show the ability of such models to account for the line profile variations as observed. However, the Mg ii line-center intensities require the model with a temperature increase toward the prominence boundary. We show that even simple one-dimensional (1D) models with a prominence-to-corona transition region (PCTR) fit the observed Mg ii and Hα lines quite well, while the isothermal–isobaric models (1D or 2D) are inconsistent with simultaneous observations in the Mg ii h and k and Hα lines, meaning that the Hα line provides a strong additional constraint on the modeling. IRIS far-UV detection of the C ii lines in this prominence seems to provide a direct constraint on the PCTR part of the model.

  14. Simulating the Formation and Evolution of Solar Prominences in Coronal Cavities

    NASA Astrophysics Data System (ADS)

    Xia, C.; Keppens, R.

    2015-12-01

    The physical mechanism responsible for the formation and the mass cycling of solar prominences has been uncertain for decades, because of the difficulty of knowing the three-dimensional (3D) magnetic field hosting prominences and the mass supply from chromosphere to prominences. Here we report comprehensive 3D simulations which demonstrate that the chromospheric evaporation and the coronal condensation in a magnetic flux rope lead to the formation of a quiescent prominence with complex internal fluid dynamics. First, we simulate the formation of a stable magnetic flux rope in the corona starting from a sheared magnetic bipolar arcade driven by shearing and converging flows at the bottom, using isothermal magnetohydrodynamics (MHD) modeling including gravity. Second, we fill the magnetic flux rope with hydrostatic plasma from chromosphere to corona and simulate a quiet sun in an equilibrium using full thermodynamic MHD with anisotropic thermal conduction, optically thin radiative losses, and parameterized heating. Then, we add extra strong heating localized in two circular regions covering chromospheric foot points of the flux rope. As the plasma is evaporated into corona, the lower part of the flux rope evolve into thermally unstable situation due to dominative radiative losses, where multiple blobs and threads of condensations form and move continuously mainly along local magnetic field. Some of the condensations fall down to chromosphere without support of magnetic dips near the foot region of the flux rope. Others linger in magnetic dips and descend slowly. Synthetic images of Solar Dynamics Observatory views with the Atmospheric Imaging Assembly shows many properties of quiescent prominences from real observations, such as, dynamics dark threads under elliptical coronal cavity.

  15. ERRATUM: Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

    NASA Technical Reports Server (NTRS)

    Schmieder, B.; Kucera, T. A.; Knizhnik, K.; Luna, M.; Lopez-Ariste, A.; Toot, D.

    2014-01-01

    We report an unusual set of observations of waves in a large prominence pillar that consist of pulses propagating perpendicular to the prominence magnetic field. We observe a huge quiescent prominence with the Solar Dynamics Observatory Atmospheric Imaging Assembly in EUV on 2012 October 10 and only a part of it, the pillar, which is a foot or barb of the prominence, with the Hinode Solar Optical Telescope (SOT; in Ca II and Halpha lines), Sac Peak (in Ha, Hß, and Na-D lines), and THEMIS ("Télescope Héliographique pour l' Etude du Magnétisme et des Instabilités Solaires") with the MTR (MulTi-Raies) spectropolarimeter (in He D3 line). The THEMIS/MTR data indicates that the magnetic field in the pillar is essentially horizontal and the observations in the optical domain show a large number of horizontally aligned features on a much smaller scale than the pillar as a whole. The data are consistent with a model of cool prominence plasma trapped in the dips of horizontal field lines. The SOT and Sac Peak data over the four hour observing period show vertical oscillations appearing as wave pulses. These pulses, which include a Doppler signature, move vertically, perpendicular to the field direction, along thin quasi-vertical columns in the much broader pillar. The pulses have a velocity of propagation of about 10 km/s, a period of about 300 s, and a wavelength around 2000 km. We interpret these waves in terms of fast magnetosonic waves and discuss possible wave drivers.

  16. PROPAGATING WAVES TRANSVERSE TO THE MAGNETIC FIELD IN A SOLAR PROMINENCE

    SciTech Connect

    Schmieder, B.; Kucera, T. A.; Knizhnik, K.; Luna, M.; Lopez-Ariste, A.; Toot, D.

    2013-11-10

    We report an unusual set of observations of waves in a large prominence pillar that consist of pulses propagating perpendicular to the prominence magnetic field. We observe a huge quiescent prominence with the Solar Dynamics Observatory Atmospheric Imaging Assembly in EUV on 2012 October 10 and only a part of it, the pillar, which is a foot or barb of the prominence, with the Hinode Solar Optical Telescope (SOT; in Ca II and Hα lines), Sac Peak (in Hα, Hβ, and Na-D lines), and THEMIS ({sup T}élescope Héliographique pour l' Etude du Magnétisme et des Instabilités Solaires{sup )} with the MTR (MulTi-Raies) spectropolarimeter (in He D{sub 3} line). The THEMIS/MTR data indicates that the magnetic field in the pillar is essentially horizontal and the observations in the optical domain show a large number of horizontally aligned features on a much smaller scale than the pillar as a whole. The data are consistent with a model of cool prominence plasma trapped in the dips of horizontal field lines. The SOT and Sac Peak data over the four hour observing period show vertical oscillations appearing as wave pulses. These pulses, which include a Doppler signature, move vertically, perpendicular to the field direction, along thin quasi-vertical columns in the much broader pillar. The pulses have a velocity of propagation of about 10 km s{sup –1}, a period of about 300 s, and a wavelength around 2000 km. We interpret these waves in terms of fast magnetosonic waves and discuss possible wave drivers.

  17. Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

    NASA Astrophysics Data System (ADS)

    Schmieder, B.; Kucera, T. A.; Knizhnik, K.; Luna, M.; Lopez-Ariste, A.; Toot, D.

    2013-11-01

    We report an unusual set of observations of waves in a large prominence pillar that consist of pulses propagating perpendicular to the prominence magnetic field. We observe a huge quiescent prominence with the Solar Dynamics Observatory Atmospheric Imaging Assembly in EUV on 2012 October 10 and only a part of it, the pillar, which is a foot or barb of the prominence, with the Hinode Solar Optical Telescope (SOT; in Ca II and Hα lines), Sac Peak (in Hα, Hβ, and Na-D lines), and THEMIS ("Télescope Héliographique pour l' Etude du Magnétisme et des Instabilités Solaires") with the MTR (MulTi-Raies) spectropolarimeter (in He D3 line). The THEMIS/MTR data indicates that the magnetic field in the pillar is essentially horizontal and the observations in the optical domain show a large number of horizontally aligned features on a much smaller scale than the pillar as a whole. The data are consistent with a model of cool prominence plasma trapped in the dips of horizontal field lines. The SOT and Sac Peak data over the four hour observing period show vertical oscillations appearing as wave pulses. These pulses, which include a Doppler signature, move vertically, perpendicular to the field direction, along thin quasi-vertical columns in the much broader pillar. The pulses have a velocity of propagation of about 10 km s-1, a period of about 300 s, and a wavelength around 2000 km. We interpret these waves in terms of fast magnetosonic waves and discuss possible wave drivers.

  18. Indications of stellar prominence oscillations on fast rotating stars: the cases of HK Aqr and PZ Tel

    NASA Astrophysics Data System (ADS)

    Leitzinger, M.; Odert, P.; Zaqarashvili, T. V.; Greimel, R.; Hanslmeier, A.; Lammer, H.

    2016-08-01

    We present the analysis of six nights of spectroscopic monitoring of two young and fast rotating late-type stars, namely the dMe star HK Aqr and the dG/dK star PZ Tel. On both stars we detect absorption features reminiscent of signatures of co-rotating cool clouds or prominences visible in Hα. Several prominences on HK Aqr show periodic variability in the prominence tracks which follow a sinusoidal motion (indication of prominence oscillations). On PZ Tel we could not find any periodic variability in the prominence tracks. By fitting sinusoidal functions to the prominence tracks we derive amplitudes and periods which are similar to those of large amplitude oscillations seen in solar prominences. In one specific event we also derive a periodic variation of the prominence track in the Hβ spectral line which shows an anti-phase variation with the one derived for the Hα spectral line. Using these parameters and estimated mass density of a prominence on HK Aqr we derive a minimum magnetic field strength of ˜2 G. The relatively low strength of the magnetic field is explained by the large height of this stellar prominence (≥ 0.67 stellar radii above the surface).

  19. EUV lines observed with EIS/Hinode in a solar prominence

    NASA Astrophysics Data System (ADS)

    Labrosse, N.; Schmieder, B.; Heinzel, P.; Watanabe, T.

    2011-07-01

    Context. During a multi-wavelength observation campaign with Hinode and ground-based instruments, a solar prominence was observed for three consecutive days as it crossed the western limb of the Sun in April 2007. Aims: We report on observations obtained on 26 April 2007 using EIS (Extreme ultraviolet Imaging Spectrometer) on Hinode. They are analysed to provide a qualitative diagnostic of the plasma in different parts of the prominence. Methods: After correcting for instrumental effects, the rasters at different wavelengths are presented. Several regions within the same prominence are identified for further analysis. Selected profiles for lines with formation temperatures between log (T) = 4.7 and log (T) = 6.3, as well as their integrated intensities, are given. The profiles of coronal, transition region, and He ii lines are discussed. We pay special attention to the He ii line, which is blended with coronal lines. Results: Some quantitative results are obtained by analysing the line profiles. They confirm that depression in EUV lines can be interpreted in terms of two mechanisms: absorption of coronal radiation by the hydrogen and neutral helium resonance continua, and emissivity blocking. We present estimates of the He ii line integrated intensity in different parts of the prominence according to different scenarios for the relative contribution of absorption and emissivity blocking to the coronal lines blended with the He ii line. We estimate the contribution of the He ii 256.32 Å line to the He ii raster image to vary between ~44% and 70% of the raster's total intensity in the prominence according to the different models used to take into account the blending coronal lines. The inferred integrated intensities of the He ii 256 Å line are consistent with the theoretical intensities obtained with previous 1D non-LTE radiative transfer calculations, yielding a preliminary estimate of the central temperature of 8700 K, a central pressure of 0.33 dyn cm-2, and a

  20. Prominent ears: Anthropometric study of the external ear of primary school children of Harare, Zimbabwe

    PubMed Central

    Muteweye, Wilfred; Muguti, Godfrey I.

    2015-01-01

    Background Prominent ear is the most common congenital ear deformity affecting 5% of children in the Western world and has profound psychosocial effects on the bearer. It is important to know the prevalence in the local population to have a better appreciation of the local burden of the abnormality as well as to know the parameters of ear morphology locally. These parameters can be useful in the diagnosis and evaluation of ear anomalies and may help reconstructive surgeons in reproducing an anatomically correct ear of an African/Zimbabwean child. Objectives To evaluate the frequency of prominent ears in black school going children in Zimbabwe and to establish morphometric properties of the ear. Design Prospective observational, cross sectional study. Setting Three Primary schools in Harare. Two in a high density area and one in a low density area. Materials and methods Three Primary schools in Harare were selected at random. The following measurements were taken: ear lengths, ear projection and face height using a sliding caliper. Three hundred and five healthy pupils of the age range 9–13 years of both sexes were included in the study, whilst children with congenital anomalies, ear tumours and history of ear trauma were excluded. Results The mean ear height across the cohort was 56.95 ± 5.00 (right ear) and 56.86 ± 4.92 (left ear). Ear projection was 19.52 ± 2.14 (right ear) and 19.59 ± 2.09 (left ear). Gender related differences were noted. Mean ear height was significantly higher in males (p-value = 0.000). Ear projection was higher in males compared to females. A total of 6.89% had prominent ears. Among males, 7.69% had prominent ears whilst 6.17% of females had prominent ears. Conclusion The prevalence of prominent ear among black African children in the studied population is comparable to that of Caucasians. The study provides a set of biometric data of auricular dimensions for normal black African children aged 9–13 years. PMID:26468372

  1. Comparative Analysis of Global Digital Elevation Models and Ultra-Prominent Mountain Peaks

    NASA Astrophysics Data System (ADS)

    Grohmann, Carlos H.

    2016-06-01

    Global Digital Elevation Models (GDEMs) are datasets of vital importance for regional-scale analysis in areas such as geomorphology, [paleo]climatology, oceanography and biodiversity. In this work I present a comparative assessment of the datasets ETOPO1 (1' resolution), GTOPO30, GLOBE, SRTM30 PLUS, GMTED2010 and ACE2 (30") against the altitude of the world's ultra prominent peaks. GDEMs' elevations show an expected tendency of underestimating the peak's altitude, but differences reach 3,500 m. None of the GDEMs captures the full range of elevation on Earth and they do not represent well the altitude of the most prominent peaks. Some of these problems could be addressed with the release of NASADEM, but the smoothing effect caused by moving-window resampling can only be tackled by using new techniques, such as scale-adaptative kernels and curvature-based terrain generalisation.

  2. The role of condensation and heat conduction in the formation of prominences - An MHD simulation

    NASA Technical Reports Server (NTRS)

    Wu, S. T.; Bao, J. J.; An, C. H.; Tandberg-Hanssen, E.

    1990-01-01

    The effects of condensation and thermal conduction on the formation of Kippenhahn-Schlueter (K-S) type prominences in quiet regions (QP) due to symmetric mass injection are investigated. To implement this investigation a self-consistent, two-dimensional, nonplanar, time-dependent MHD simulation model is developed. In the model, various values of the injection velocity, density, and magnetic field strength are used to determine the most favorable conditions for the QP formation. Based on these simulation results, it is found that the formation of a K-S type field configuration should be considered as a dynamic process which needs both condensation amd mass injection to supply enough mass to maintain such a configuration to complete the quiescent prominence formation process.

  3. Two-Dimensional Mapping of the He D3/Hβ Emission Ratio in Solar Prominences

    NASA Astrophysics Data System (ADS)

    Wiehr, Eberhard; Stellmacher, Goetz; Hirzberger, Johann

    2007-01-01

    Solar prominences have been simultaneously observed in the integrated light of the He D3 and the Hβ emissions on two successive days, using the SST on La Palma with its tip-tilt mirror locked on a nearby white-light limb facular grain. The spatial and the temporal variation of the integrated line intensities and their ratio shows mainly two characteristics: (A) Constant emission ratio (even) in regions with substantial intensity variations and (B) varying emission ratio (often) tightly related to intensity structures of the prominence. (A) May be explained by a different number of superposing threads along the line of sight having very similar physical state. (B) Indicates threads with different intrinsic physical states; these may depend on the gas pressure or the inner structure of each thread, i.e., the “packing density,” affecting the penetration of ionizing EUV radiation, which affects the He I level populations and thus the rate of the triplet excitation.

  4. Lexical and Phrasal Prominence Patterns in School-Aged Children's Speech

    PubMed Central

    Shport, Irina A.; Redford, Melissa A.

    2013-01-01

    This study investigated the integration of word- and phrase-level prominences in speech produced by 25 school-aged children (6;2 to 7;3) and 25 adults. Participants produced disyllabic number words in a straight count condition and in two phrasal conditions, namely, a stress clash and non-clash phrasal context. Duration and amplitude measures of syllable rhymes were used to assess the realization of lexical stress, and fundamental frequency (F0) measures were used to assess the realization of phrasal pitch accents across conditions. Results showed that the duration and F0 correlates varied independently of each other as a function of condition in child speech, but much less so in adult speech. The group differences were taken to indicate that 6-year-old children have yet to develop prosodic structures with integrated prominence. Structural and pragmatic interpretations of the results are discussed. PMID:24020889

  5. A case of brugada syndrome presenting with ventricular fibrillation storm and prominent early repolarization.

    PubMed

    Iizuka, Chifumi; Sato, Masahito; Kitazawa, Hitoshi; Ikeda, Yoshio; Okabe, Masaaki; Kugiyama, Kiyotaka; Aizawa, Yoshifusa

    2016-01-01

    A 21-year-old man developed ventricular fibrillation (VF) while drinking alcohol and was admitted to our hospital. An electrocardiogram (ECG) on admission revealed remarkably prominent slurs on the terminal part of QRS complexes in the left precordial leads and a coved type ST elevation at higher intercostal spaces. After hypothermia therapy, he underwent implantation of an implantable cardioverter-defibrillator (ICD). Standard twelve-lead follow-up ECGs revealed early repolarization pattern and an intermittent coved type ST elevation. When the coved type ST elevation appeared, the early repolarization pattern in the inferior and left precordial leads was attenuated. Prominent early repolarization pattern was the most likely trigger of the VF storm in this Brugada patient. PMID:27038845

  6. Properties of Active and Quiescent Prominences from Mid-Infrared Line Analysis

    NASA Astrophysics Data System (ADS)

    Chang, Edward S.; Deming, Drake

    1997-05-01

    We have analyzed all lines in the MIR (8 to 20 micron) spectra of a quiescent(Q) and two time-frames of an active (A1 and A2) prominence. In addition to those found by Zirker(1985), we have identified a higher excitation hydrogen line and two helium recombination lines. Accounting for instrumental broadening, we can separate out the Doppler and the Stark contributions. The former yields maximum temperatures of 6200K, 34000K and 22000K and the latter electron densities (Ne) of 8(1), 30(3) and 14(2) in units of 10(10) cm(-3) for Q, A1 and A2 respectively. Using the same assumptions made by Zirker, namely, (1) the strongest line (7-6) is optically thin, (2) the population of the lower level(n=6) is determined by direct radiative recombination and photo-ionization, (3) the equality of proton and electron densities, and (4) the thickness of the prominence is at least 10(8) cm, we derive a new inequality, Ne <= 1.83 *E(8) T(0.75) e(-2195/T) . Substituting our maximum temperatures into the RHS, we find upper bound Ne values of 9, 43 and 30 in the same units as above. We have now found the helium recombination spectrum which has been postulated by Tandberg-Hanssen as one of three possible ways of equilibrating the triplet/ singlet ratio. Surprisingly, it is present in the quiescent as well as the active prominence. We will report on utilizing the helium line widths to further constrain the temperature and to find the turbulence velocities. Ref. Zirker, J.B. (1985), Solar Physics, 102, 33. Tandberg-Hanssen,E. (1978) Solar Prominences.

  7. Numerical simulation of mass injection for the formation of prominence magnetic field configurations. II - Symmetric injection

    NASA Technical Reports Server (NTRS)

    An, C.-H.; Bao, J. J.; Wu, S. T.; Suess, S. T.

    1988-01-01

    A two-dimensional MHD model simulating the formation of Kippenhahn-Schluter (1957) quiescent prominence (QP) magnetic field configurations is used to explore symmetric mass injection into a dipole magnetic field. An optimum magnetic field strength for QP formation by mass injection is obtained. It is found that a weaker magnetic field strength is more favorable for the condensation of the injected plasma but that a stronger field is more favorable for supporting the condensed plasma against gravity.

  8. ROTATING MOTIONS AND MODELING OF THE ERUPTING SOLAR POLAR-CROWN PROMINENCE ON 2010 DECEMBER 6

    SciTech Connect

    Su, Yingna; Van Ballegooijen, Adriaan

    2013-02-10

    A large polar-crown prominence composed of different segments spanning nearly the entire solar disk erupted on 2010 December 6. Prior to the eruption, the filament in the active region part split into two layers: a lower layer and an elevated layer. The eruption occurs in several episodes. Around 14:12 UT, the lower layer of the active region filament breaks apart: One part ejects toward the west, while the other part ejects toward the east, which leads to the explosive eruption of the eastern quiescent filament. During the early rise phase, part of the quiescent filament sheet displays strong rolling motion (observed by STEREO-B) in the clockwise direction (viewed from east to west) around the filament axis. This rolling motion appears to start from the border of the active region, then propagates toward the east. The Atmospheric Imaging Assembly (AIA) observes another type of rotating motion: In some other parts of the erupting quiescent prominence, the vertical threads turn horizontal, then turn upside down. The elevated active region filament does not erupt until 18:00 UT, when the erupting quiescent filament has already reached a very large height. We develop two simplified three-dimensional models that qualitatively reproduce the observed rolling and rotating motions. The prominence in the models is assumed to consist of a collection of discrete blobs that are tied to particular field lines of a helical flux rope. The observed rolling motion is reproduced by continuous twist injection into the flux rope in Model 1 from the active region side. Asymmetric reconnection induced by the asymmetric distribution of the magnetic fields on the two sides of the filament may cause the observed rolling motion. The rotating motion of the prominence threads observed by AIA is consistent with the removal of the field line dips in Model 2 from the top down during the eruption.

  9. Study of a Prominence Eruption using PROBA2/SWAP and STEREO/EUVI Data

    NASA Astrophysics Data System (ADS)

    Mierla, M.; Seaton, D. B.; Berghmans, D.; Chifu, I.; De Groof, A.; Inhester, B.; Rodriguez, L.; Stenborg, G.; Zhukov, A. N.

    2013-08-01

    Observations of the early rise and propagation phases of solar eruptive prominences can provide clues about the forces acting on them through the behavior of their acceleration with height. We have analyzed such an event, observed on 13 April 2010 by SWAP on PROBA2 and EUVI on STEREO. A feature at the top of the erupting prominence was identified and tracked in images from the three spacecraft. The triangulation technique was used to derive the true direction of propagation of this feature. The reconstructed points were fitted with two mathematical models: i) a power-law polynomial function and ii) a cubic smoothing spline, in order to derive the accelerations. The first model is characterized by five degrees of freedom while the second one is characterized by ten degrees of freedom. The results show that the acceleration increases smoothly, and it is continuously increasing with height. We conclude that the prominence is not accelerated immediately by local reconnection, but rather is swept away as part of a large-scale relaxation of the coronal magnetic field.

  10. Evaluation of Subcision for the Correction of the Prominent Nasolabial Folds

    PubMed Central

    Robati, R. M.; Abdollahimajd, F.; Robati, A. M.

    2015-01-01

    Background. A prominent nasolabial fold (NLF) is a cosmetic problem. Currently, numerous therapeutic modalities are available for pronounced NLFs with variable efficacy. Objective. To determine the efficacy and safety of subcision using a hypodermic needle for the correction of the prominent NLFs and its effect on skin elasticity. Methods. Sixteen patients with prominent NLFs underwent subcision. The investigators' assessment of improvement and the patients' satisfaction were both recorded 1 and 6 months after the procedure. Also, we evaluate the skin elasticity of NLFs before and after the treatment using a sensitive biometrologic device with the measurement of cutaneous resonance running time (CRRT). Results. Thirteen (81.25%) patients showed a moderate improvement at 1st month and 13 (81.25%) patients had at least a mild improvement at 6th month. There was no persistent side effect lasting more than a few days. Mean CRRT at 1 and 6 months after the treatment was significantly higher compared to the baseline. Conclusion. Subcision may be considered effective for the correction of pronounced NLFs. However, further controlled studies with larger sample size are necessary to assess the efficacy of this technique in particular with use of more objective assessment of skin biometric characteristics. This trial is registered with IRCT201108097270N1 (registered on January 27, 2012). PMID:26788052

  11. 3D conductive coupling for efficient generation of prominent Fano resonances in metamaterials

    NASA Astrophysics Data System (ADS)

    Liu, Zhiguang; Liu, Zhe; Li, Jiafang; Li, Wuxia; Li, Junjie; Gu, Changzhi; Li, Zhi-Yuan

    2016-06-01

    We demonstrate a 3D conductive coupling mechanism for the efficient generation of prominent and robust Fano resonances in 3D metamaterials (MMs) formed by integrating vertical U-shape split-ring resonators (SRRs) or vertical rectangular plates along a planar metallic hole array with extraordinary optical transmission (EOT). In such a configuration, intensified vertical E-field is induced along the metallic holes and naturally excites the electric resonances of the vertical structures, which form non-radiative “dark” modes. These 3D conductive “dark” modes strongly interfere with the “bright” resonance mode of the EOT structure, generating significant Fano resonances with both prominent destructive and constructive interferences. The demonstrated 3D conductive coupling mechanism is highly universal in that both 3D MMs with vertical SRRs and vertical plates exhibit the same prominent Fano resonances despite their dramatic structural difference, which is conceptually different from conventional capacitive and inductive coupling mechanisms that degraded drastically upon small structural deviations.

  12. 3D conductive coupling for efficient generation of prominent Fano resonances in metamaterials

    PubMed Central

    Liu, Zhiguang; Liu, Zhe; Li, Jiafang; Li, Wuxia; Li, Junjie; Gu, Changzhi; Li, Zhi-Yuan

    2016-01-01

    We demonstrate a 3D conductive coupling mechanism for the efficient generation of prominent and robust Fano resonances in 3D metamaterials (MMs) formed by integrating vertical U-shape split-ring resonators (SRRs) or vertical rectangular plates along a planar metallic hole array with extraordinary optical transmission (EOT). In such a configuration, intensified vertical E-field is induced along the metallic holes and naturally excites the electric resonances of the vertical structures, which form non-radiative “dark” modes. These 3D conductive “dark” modes strongly interfere with the “bright” resonance mode of the EOT structure, generating significant Fano resonances with both prominent destructive and constructive interferences. The demonstrated 3D conductive coupling mechanism is highly universal in that both 3D MMs with vertical SRRs and vertical plates exhibit the same prominent Fano resonances despite their dramatic structural difference, which is conceptually different from conventional capacitive and inductive coupling mechanisms that degraded drastically upon small structural deviations. PMID:27296109

  13. Flux Collision Models of Prominence Formation, or Breaking Up is Hard to Do

    NASA Astrophysics Data System (ADS)

    Welsch, B. T.; DeVore, C. R.; Antiochos, S. K.

    2004-05-01

    To investigate the hypothesis that the prominences form by magnetic reconnection between initially distinct flux systems above the solar photosphere, we employ the ARMS code, a 3D, flux-corrected transport MHD code with adaptive mesh refinement, to simulate magnetic field evolution when two flux systems are driven to collide by photospheric boundary motions. In particular, we focus on driving configurations similar to the prominence model of Martens and Zwaan (2001). We find that: 1) reconnection proceeds only weakly, if at all, in typical active region configurations driven with differential-rotation-like shear, which leads to glancing collisions; 2) reconnection proceeds efficiently in configurations that are driven to collide directly, with converging motions along the neutral line; and 3) reconnected fields from this process can exhibit sheared, dipped field lines along the neutral line, consistent with prominence observations. As our field configurations do not posses the ``breakout'' topology, eruptions are not observed. This work was supported by ONR, NASA's SEC Theory program, and by a grant of computer time from the DOD High Performance Computing Modernization Program at the ERDC MSRC.

  14. SDO and STEREO Observations of Prominence Dynamics During a Series of Eight Homologous Flares

    NASA Technical Reports Server (NTRS)

    Panesar, Navdeep K.; Innes, Davina E.; Sterling, Alphonse C.; Moore, Ronald L.

    2014-01-01

    Homologous flares are eruptive events that occur repetitively in the same active region, with similar structure and morphology. A series of at least eight homologous flares occurred in active region NOAA 11237 over 16 - 17 June 2011. A filament is rooted in the active region with an overlying coronal cavity. The active region appears on the southeast solar limb as seen from SDO/AIA, and on the disk as viewed from STEREO-B/EUVI; the dual perspective allows us to study in detail behavior of prominence/filament material entrained in the magnetic field of the repeatedly-erupting system. Each of the eruptions was mainly confined, with active-region prominence material being ejected from the core of the erupting region onto outer-lobe loops of the active region. The eruption series repeatedly disrupted material of a quiet-Sun extension of the prominence, and that material became suspended at progressively higher heights above the surface. Two final eruptions from the core region destabilized the field holding that material, instigating a coronal mass ejection (CME).

  15. Can patients without early, prominent visual deficits still be diagnosed of posterior cortical atrophy?

    PubMed Central

    Suárez-González, A.; Crutch, S.J.; Roldán Lora, F.; Franco-Macías, E.; Gil-Néciga, E.

    2016-01-01

    Background Early and progressive disabling visual impairment is a core feature for the diagnosis of posterior cortical atrophy (PCA). However, some individuals that fulfil criteria over time might initially present with an onset of prominent posterior dysfunction other than visuoperceptual. Methods The clinical profile of five patients with a predominantly ‘non-visual’ posterior presentation (PCA2) was investigated and compared with sixteen individuals with visually predominant PCA (PCA1) and eighteen with typical amnestic Alzheimer disease (tAD). Results PCA2 patients showed significantly better performance than PCA1 in one visuospatial task and were free of Balint's syndrome and visual agnosia. Compared to tAD, PCA2 showed trends towards significantly lower performance in visuoperceptual tasks, more severe apraxia and more symptoms of Gerstmann's syndrome. Conclusions Our sample of PCA2 patients did not present with clinically prominent visual symptoms but did show visual dysfunction on formal neuropsychological assessment (less pronounced than in PCA1 but more than in tAD) in addition to other posterior deficits. Broadening the definition of PCA to encompass individuals presenting with prominent ‘non-visual’ posterior dysfunction should be potentially considered in clinical and research contexts. PMID:27423559

  16. Numerical simulation of mass injection for the formation of prominence magnetic field configurations. I - Asymmetric injection

    NASA Technical Reports Server (NTRS)

    An, Chang-Hyuk; Bao, J. J.; Wu, S. T.

    1988-01-01

    A two-dimensional ideal MHD numerical model is used to investigate chromospheric mass injection into an overlying coronal dipole magnetic field. Such injection is shown to produce magnetic field deformations conducive to the formation of active region prominences. The results support a model in which an absorptive strand is formed by chromospheric asymmetric mass injection into the overlying coronal magnetic field. A necessary condition for the accumulation of the strands is that the mass injection forms a Kippenhahn-Schluter-type (1957) field configuration.

  17. PROM4: 1D isothermal and isobaric modeler for solar prominences

    NASA Astrophysics Data System (ADS)

    Gouttebroze, P.; Labrosse, N.

    2013-06-01

    PROM4 computes simple models of solar prominences which consist of plane-parallel slabs standing vertically above the solar surface. Each model is defined by 5 parameters: temperature, density, geometrical thickness, microturbulent velocity and height above the solar surface. PROM4 solves the equations of radiative transfer, statistical equilibrium, ionization and pressure equilibria, and computes electron and hydrogen level populations and hydrogen line profiles. Written in Fortran 90 and with two versions available (one with text in English, one with text in French), the code needs 64-bit arithmetic for real numbers.

  18. Magnetohydrodynamic waves in two-dimensional prominences embedded in coronal arcades

    SciTech Connect

    Terradas, J.; Soler, R.; Díaz, A. J.; Oliver, R.; Ballester, J. L.

    2013-11-20

    Solar prominence models used so far in the analysis of MHD waves in two-dimensional structures are quite elementary. In this work, we calculate numerically magnetohydrostatic models in two-dimensional configurations under the presence of gravity. Our interest is in models that connect the magnetic field to the photosphere and include an overlying arcade. The method used here is based on a relaxation process and requires solving the time-dependent nonlinear ideal MHD equations. Once a prominence model is obtained, we investigate the properties of MHD waves superimposed on the structure. We concentrate on motions purely two-dimensional, neglecting propagation in the ignorable direction. We demonstrate how, by using different numerical tools, we can determine the period of oscillation of stable waves. We find that vertical oscillations, linked to fast MHD waves, are always stable and have periods in the 4-10 minute range. Longitudinal oscillations, related to slow magnetoacoustic-gravity waves, have longer periods in the range of 28-40 minutes. These longitudinal oscillations are strongly influenced by the gravity force and become unstable for short magnetic arcades.

  19. Fine Magnetic Structure and Origin of Counter-streaming Mass Flows in a Quiescent Solar Prominence

    NASA Astrophysics Data System (ADS)

    Shen, Yuandeng; Liu, Yu; Liu, Ying D.; Chen, P. F.; Su, Jiangtao; Xu, Zhi; Liu, Zhong

    2015-11-01

    We present high-resolution observations of a quiescent solar prominence that consists of a vertical and a horizontal foot encircled by an overlying spine and has ubiquitous counter-streaming mass flows. While the horizontal foot and the spine were connected to the solar surface, the vertical foot was suspended above the solar surface and was supported by a semicircular bubble structure. The bubble first collapsed, then reformed at a similar height, and finally started to oscillate for a long time. We find that the collapse and oscillation of the bubble boundary were tightly associated with a flare-like feature located at the bottom of the bubble. Based on the observational results, we propose that the prominence should be composed of an overlying horizontal spine encircling a low-lying horizontal and vertical foot, in which the horizontal foot consists of shorter field lines running partially along the spine and has ends connected to the solar surface, while the vertical foot consists of piling-up dips due to the sagging of the spine fields and is supported by a bipolar magnetic system formed by parasitic polarities (i.e., the bubble). The upflows in the vertical foot were possibly caused by the magnetic reconnection at the separator between the bubble and the overlying dips, which intruded into the persistent downflow field and formed the picture of counter-streaming mass flows. In addition, the counter-streaming flows in the horizontal foot were possibly caused by the imbalanced pressure at the both ends.

  20. Novel large-range mitochondrial DNA deletions and fatal multisystemic disorder with prominent hepatopathy

    SciTech Connect

    Bianchi, Marzia; Rizza, Teresa; Verrigni, Daniela; Martinelli, Diego; Tozzi, Giulia; Torraco, Alessandra; Piemonte, Fiorella; Dionisi-Vici, Carlo; Nobili, Valerio; Francalanci, Paola; Boldrini, Renata; Callea, Francesco; Santorelli, Filippo Maria; Bertini, Enrico; and others

    2011-11-18

    Highlights: Black-Right-Pointing-Pointer Expanded array of mtDNA deletions. Black-Right-Pointing-Pointer Pearson syndrome with prominent hepatopathy associated with single mtDNA deletions. Black-Right-Pointing-Pointer Detection of deletions in fibroblasts and blood avoids muscle and liver biopsy. Black-Right-Pointing-Pointer Look for mtDNA deletions before to study nuclear genes related to mtDNA depletion. -- Abstract: Hepatic involvement in mitochondrial cytopathies rarely manifests in adulthood, but is a common feature in children. Multiple OXPHOS enzyme defects in children with liver involvement are often associated with dramatically reduced amounts of mtDNA. We investigated two novel large scale deletions in two infants with a multisystem disorder and prominent hepatopathy. Amount of mtDNA deletions and protein content were measured in different post-mortem tissues. The highest levels of deleted mtDNA were in liver, kidney, pancreas of both patients. Moreover, mtDNA deletions were detected in cultured skin fibroblasts in both patients and in blood of one during life. Biochemical analysis showed impairment of mainly complex I enzyme activity. Patients manifesting multisystem disorders in childhood may harbour rare mtDNA deletions in multiple tissues. For these patients, less invasive blood specimens or cultured fibroblasts can be used for molecular diagnosis. Our data further expand the array of deletions in the mitochondrial genomes in association with liver failure. Thus analysis of mtDNA should be considered in the diagnosis of childhood-onset hepatopathies.

  1. Observational Detection of Drift Velocity between Ionized and Neutral Species in Solar Prominences

    NASA Astrophysics Data System (ADS)

    Khomenko, Elena; Collados, Manuel; Díaz, Antonio J.

    2016-06-01

    We report the detection of differences in the ion and neutral velocities in prominences using high-resolution spectral data obtained in 2012 September at the German Vacuum Tower Telescope (Observatorio del Teide, Tenerife). A time series of scans of a small portion of a solar prominence was obtained simultaneously with high cadence using the lines of two elements with different ionization states, namely, Ca ii 8542 Å and He i 10830 Å. The displacements, widths, and amplitudes of both lines were carefully compared to extract dynamical information about the plasma. Many dynamical features are detected, such as counterstreaming flows, jets, and propagating waves. In all of the cases, we find a very strong correlation between the parameters extracted from the lines of both elements, confirming that both lines trace the same plasma. Nevertheless, we also find short-lived transients where this correlation is lost. These transients are associated with ion-neutral drift velocities of the order of several hundred m s‑1. The patches of non-zero drift velocity show coherence in time–distance diagrams.

  2. Reduction in Prosodic Prominence Predicts Speakers’ Recall: Implications for Theories of Prosody

    PubMed Central

    Watson, Duane G.; Benjamin, Aaron S.

    2014-01-01

    Repeated words are often reduced in prosodic prominence, but the underlying mechanisms remain unclear. The present study contrasted two theories: does prosodic reduction reflect the choice of a particular linguistic form, or does ease of retrieval within the language production system lead to facilitated, less prominent productions? One test of facilitation-based theories is suggested by findings on human memory: Whether a second presentation of an item benefits later memory is predicted by the item’s availability at the time of the second presentation. If prosodic reduction partially reflects facilitated retrieval, it should predict later memory. One naïve participant described to another participant routes on a map. Critical items were mentioned twice. Following the map task, the speaker attempted written recall of the mentioned items. As expected, acoustic intensity of the second mentions predicted later recall in the same way that difficulty of retrieval has in other tasks. This pattern suggests that one source of prosodic reduction is facilitation within the language production system. PMID:26594647

  3. Dynamics of a prominence observed in Mg II lines by IRIS

    NASA Astrophysics Data System (ADS)

    Schmieder, Brigitte; Mein, Pierre; Dalmasse, Kévin; Tian, Hui; Kucera, Therese; Lopez-Ariste, Arturo

    In September 2013 several prominences were observed with the IRIS spectrograph during a 60 day-long international program. We will present one set of observations obtained using multiple instruments on September 24. SDO/AIA and IRIS slit jaws provided images of the prominence corresponding to different physical conditions of the transition region between the cool plasma and the corona. The vector magnetic field was derived from THEMIS (Tenerife) observations using the He D3 depolarisation due to the magnetic field. The inversion code (CPA) takes into account the Hanle and the Zeeman effects. Movies from SDO/AIA in 304 A and Hinode/SOT in Ca II show the dynamics of the fine structures in the plane of the sky. From Mg II and Si IV line spectra observed by IRIS and H-alpha observed by the Multi-channel subtractive spectrograph (MSDP) in the Meudon solar tower we derived the Dopplershifts of the fine structures. The profiles of the Mg II lines are narrow (FHWM =0.15 A) and not reversed, contrary to the predictions of the theoretical models (Paletou et al 1993). We could resolve the velocity of several structures along the LOS with Dopplershifts as high as 60 km/s.

  4. Study of H-alpha emission from solar limb prominences using Fabry-Perot interferometry

    NASA Astrophysics Data System (ADS)

    Jarrett, A. H.; Stapelberg, J.; Lategan, A. H.

    1981-02-01

    The Fabry-Perot interferometer is an effective dispersing element for studying H-alpha emission from solar limb prominences. Having a reflecting coefficient in the range 0.85-0.95, the Fabry-Perot multiple beam interferometer behaves as an angular filter, forming circular interference fringes. Results from an investigation performed at the solar installation at Boyden Observatory in South Africa are presented, where a photographic Fabry-Perot interferometer was used to obtain fringes from the 656.3-nm H-alpha emission during April and May 1980. Successful scans were made with air admitted to the interferometer pressure chamber, and reduction of the data on photon count and chamber pressure was made by a UNIVAC 1108 computer. Sketches and profiles from the limb prominences are shown; a table of fringe half-widths, corrected for the instrumental width of the interferometer, were obtained by matching a Voigt function by a least-squares computer fit to the observed scanned Fabry-Perot fringe profiles.

  5. Resonant Absorption of Transverse Oscillations and Associated Heating in a Solar Prominence. II. Numerical Aspects

    NASA Astrophysics Data System (ADS)

    Antolin, P.; Okamoto, T. J.; De Pontieu, B.; Uitenbroek, H.; Van Doorsselaere, T.; Yokoyama, T.

    2015-08-01

    Transverse magnetohydrodynamic (MHD) waves are ubiquitous in the solar atmosphere and may be responsible for generating the Sun’s million-degree outer atmosphere. However, direct evidence of the dissipation process and heating from these waves remains elusive. Through advanced numerical simulations combined with appropriate forward modeling of a prominence flux tube, we provide the observational signatures of transverse MHD waves in prominence plasmas. We show that these signatures are characterized by a thread-like substructure, strong transverse dynamical coherence, an out-of-phase difference between plane-of-the-sky motions and line-of-sight velocities, and enhanced line broadening and heating around most of the flux tube. A complex combination between resonant absorption and Kelvin-Helmholtz instabilities (KHIs) takes place in which the KHI extracts the energy from the resonant layer and dissipates it through vortices and current sheets, which rapidly degenerate into turbulence. An inward enlargement of the boundary is produced in which the turbulent flows conserve the characteristic dynamics from the resonance, therefore guaranteeing detectability of the resonance imprints. We show that the features described in the accompanying paper through coordinated Hinode and Interface Region Imaging Spectrograph observations match the numerical results well.

  6. Exploring the prominence-corona connection and its expansion into the outer corona using total solar eclipse observations

    SciTech Connect

    Habbal, Shadia Rifai; Morgan, Huw; Druckmüller, Miloslav

    2014-10-01

    Prominences constitute the most complex magnetic structures in the solar corona. The ubiquitous presence of their seemingly confined dense and cool plasma in an otherwise million-degree environment remains a puzzle. Using a decade of white light total solar eclipse observations, we show how these images reveal an intricate relationship between prominences and coronal structures both in their immediate vicinity, known as coronal cavities, and in the extended corona out to several solar radii. Observations of suspended prominences and twisted helical structures spanning several solar radii are central to these findings. The different manifestations of the prominence-corona interface that emerge from this study underscore the fundamental role played by prominences in defining and controlling the complex expansion and dynamic behavior of the solar magnetic field in the neighborhood of magnetic polarity reversal regions. This study suggests that the unraveling of prominences and the outward expansion of the helical twisted field lines linked to them could be the solar origin of twisted magnetic flux ropes detected in interplanetary space, and of the mechanism by which the Sun sheds its magnetic helicity. This work also underscores the likely role of the prominence-corona interface as a source of the slow solar wind.

  7. STEREOSCOPIC RECONSTRUCTION FROM STEREO/EUV IMAGERS DATA OF THE THREE-DIMENSIONAL SHAPE AND EXPANSION OF AN ERUPTING PROMINENCE

    SciTech Connect

    Bemporad, A.

    2009-08-10

    On 2007 May 9, a prominence eruption was observed in the He II {lambda}304 filter by the two EUV Imagers (EUVI) telescopes aboard the STEREO A and B spacecrafts. The high spatial resolution ({approx}1.''5 pixel{sup -1}) EUVI images have been used to infer via triangulation the three-dimensional (3D) shape and orientation of the prominence {approx_equal}12 minutes after the beginning (13:40 UT) of the eruption. At this time, the prominence has the shape of a 'hook' with the base anchored at the Sun. The 'hook' prominence is highly inclined southward with respect to the radial direction, has an average thickness of 0.061 R {sub sun}, a length of 0.43 R {sub sun}, and lies in first approximation on a plane inclined by {approx}54.{sup 0}5 with respect to the line of sight. Thanks to the very high temporal cadence ({approx}37 s) of EUVI observations it has been possible also to infer the 3D early eruption trajectory. In the following {approx}20 minutes the prominence rotates westward, undergoing a strong latitudinal acceleration, {approx}3 times larger than the radial acceleration. In this time interval, the prominence expands in a direction mainly parallel to the plane of the sky; the total volume occupied by the plasma increases by a factor of {approx}8, while the prominence thickness increases only by {approx}12%. This is related to the fact that the early prominence expansion is anisotropic and occurs mainly on a plane parallel to the plane of the sky. Even if the small-scale spatial distribution of the erupting material observed in the He II EUVI images is quite complex, both the approximately planar shape and the successive planar expansion suggest that on larger spatial scales the prominence can be globally approximated as a two-dimensional 'ribbon-like' feature, instead of a 3D twisted flux tube.

  8. Poorly differentiated salivary gland carcinoma with prominent squamous metaplasia in a pregnant Wistar Hannover rat.

    PubMed

    Shimada, Yuko; Yoshida, Toshinori; Takahashi, Naofumi; Akema, Satoshi; Soma, Katsumi; Ohnuma-Koyama, Aya; Sato, Akira; Kuwahara, Maki; Harada, Takanori

    2016-06-01

    A subcutaneous pale brown-colored mass was observed macroscopically in the ventral neck of a 16-week-old Wistar rat on day 18 of gestation. The mass was well demarcated from the adjacent tissues with partial invasion into connective tissues. Necrosis and hemorrhage were evident throughout the mass. The mass comprised a diffuse sheet and a nest-like structure of epithelial cells with prominent squamous metaplasia. The neoplastic cells tested immunopositive for keratin, vimentin, glial fibrillary acidic protein and p63. A portion of the neoplastic cells exhibited a similar immunoreaction of prominin-1 to the ductal and acinar cells in normal submandibular and parotid glands. Collectively, the tumor was diagnosed as a poorly differentiated carcinoma derived from epithelial/myoepithelial lineages in the submandibular and/or parotid glands. PMID:26782134

  9. Prominent electrochromism through vacancy-order melting in a complex oxide.

    PubMed

    Seidel, J; Luo, W; Suresha, S J; Nguyen, P-K; Lee, A S; Kim, S-Y; Yang, C-H; Pennycook, S J; Pantelides, S T; Scott, J F; Ramesh, R

    2012-01-01

    Electrochromes are materials that have the ability to reversibly change from one colour state to another with the application of an electric field. Electrochromic colouration efficiency is typically large in organic materials that are not very stable chemically. Here we show that inorganic Bi(0.9)Ca(0.1)FeO(3-0.05) thin films exhibit a prominent electrochromic effect arising from an intrinsic mechanism due to the melting of oxygen-vacancy ordering and the associated redistribution of carriers. We use a combination of optical characterization techniques in conjunction with high-resolution transmission electron microscopy and first-principles theory. The absorption change and colouration efficiency at the band edge (blue-cyan region) are 4.8×10(6) m(-1) and 190 cm(2) C(-1), respectively, which are the highest reported values for inorganic electrochromes, even exceeding values of some organic materials. PMID:22531184

  10. Poorly differentiated salivary gland carcinoma with prominent squamous metaplasia in a pregnant Wistar Hannover rat

    PubMed Central

    SHIMADA, Yuko; YOSHIDA, Toshinori; TAKAHASHI, Naofumi; AKEMA, Satoshi; SOMA, Katsumi; OHNUMA-KOYAMA, Aya; SATO, Akira; KUWAHARA, Maki; HARADA, Takanori

    2016-01-01

    A subcutaneous pale brown-colored mass was observed macroscopically in the ventral neck of a 16-week-old Wistar rat on day 18 of gestation. The mass was well demarcated from the adjacent tissues with partial invasion into connective tissues. Necrosis and hemorrhage were evident throughout the mass. The mass comprised a diffuse sheet and a nest-like structure of epithelial cells with prominent squamous metaplasia. The neoplastic cells tested immunopositive for keratin, vimentin, glial fibrillary acidic protein and p63. A portion of the neoplastic cells exhibited a similar immunoreaction of prominin-1 to the ductal and acinar cells in normal submandibular and parotid glands. Collectively, the tumor was diagnosed as a poorly differentiated carcinoma derived from epithelial/myoepithelial lineages in the submandibular and/or parotid glands. PMID:26782134

  11. Starch Catabolism by a Prominent Human Gut Symbiont Is Directed by the Recognition of Amylose Helices

    SciTech Connect

    Koropatkin, Nicole M.; Martens, Eric C.; Gordon, Jeffrey I.; Smith, Thomas J.

    2009-01-12

    The human gut microbiota performs functions that are not encoded in our Homo sapiens genome, including the processing of otherwise undigestible dietary polysaccharides. Defining the structures of proteins involved in the import and degradation of specific glycans by saccharolytic bacteria complements genomic analysis of the nutrient-processing capabilities of gut communities. Here, we describe the atomic structure of one such protein, SusD, required for starch binding and utilization by Bacteroides thetaiotaomicron, a prominent adaptive forager of glycans in the distal human gut microbiota. The binding pocket of this unique {alpha}-helical protein contains an arc of aromatic residues that complements the natural helical structure of starch and imposes this conformation on bound maltoheptaose. Furthermore, SusD binds cyclic oligosaccharides with higher affinity than linear forms. The structures of several SusD/oligosaccharide complexes reveal an inherent ligand recognition plasticity dominated by the three-dimensional conformation of the oligosaccharides rather than specific interactions with the composite sugars.

  12. Action in Perception: Prominent Visuo-Motor Functional Symmetry in Musicians during Music Listening

    PubMed Central

    Burunat, Iballa; Brattico, Elvira; Puoliväli, Tuomas; Ristaniemi, Tapani; Sams, Mikko; Toiviainen, Petri

    2015-01-01

    Musical training leads to sensory and motor neuroplastic changes in the human brain. Motivated by findings on enlarged corpus callosum in musicians and asymmetric somatomotor representation in string players, we investigated the relationship between musical training, callosal anatomy, and interhemispheric functional symmetry during music listening. Functional symmetry was increased in musicians compared to nonmusicians, and in keyboardists compared to string players. This increased functional symmetry was prominent in visual and motor brain networks. Callosal size did not significantly differ between groups except for the posterior callosum in musicians compared to nonmusicians. We conclude that the distinctive postural and kinematic symmetry in instrument playing cross-modally shapes information processing in sensory-motor cortical areas during music listening. This cross-modal plasticity suggests that motor training affects music perception. PMID:26422790

  13. Too good to be true: publication bias in two prominent studies from experimental psychology.

    PubMed

    Francis, Gregory

    2012-04-01

    Empirical replication has long been considered the final arbiter of phenomena in science, but replication is undermined when there is evidence for publication bias. Evidence for publication bias in a set of experiments can be found when the observed number of rejections of the null hypothesis exceeds the expected number of rejections. Application of this test reveals evidence of publication bias in two prominent investigations from experimental psychology that have purported to reveal evidence of extrasensory perception and to indicate severe limitations of the scientific method. The presence of publication bias suggests that those investigations cannot be taken as proper scientific studies of such phenomena, because critical data are not available to the field. Publication bias could partly be avoided if experimental psychologists started using Bayesian data analysis techniques. PMID:22351589

  14. Observations of Linear Polarization in a Solar Coronal Loop Prominence System Observed near 6173 Å

    NASA Astrophysics Data System (ADS)

    Saint-Hilaire, Pascal; Schou, Jesper; Martínez Oliveros, Juan-Carlos; Hudson, Hugh S.; Krucker, Säm; Bain, Hazel; Couvidat, Sébastien

    2014-05-01

    White-light observations by the Solar Dynamics Observatory's Helioseismic and Magnetic Imager of a loop-prominence system occurring in the aftermath of an X-class flare on 2013 May 13 near the eastern solar limb show a linearly polarized component, reaching up to ~20% at an altitude of ~33 Mm, about the maximum amount expected if the emission were due solely to Thomson scattering of photospheric light by the coronal material. The mass associated with the polarized component was 8.2 × 1014 g. At 15 Mm altitude, the brightest part of the loop was 3(±0.5)% linearly polarized, only about 20% of that expected from pure Thomson scattering, indicating the presence of an additional unpolarized component at wavelengths near Fe I (617.33 nm). We estimate the free electron density of the white-light loop system to possibly be as high as 1.8 × 1012 cm-3.

  15. Self-report symptoms that predict major depression in patients with prominent physical symptoms.

    PubMed

    Abbey, S E; Toner, B B; Garfinkel, P E; Kennedy, S H; Kaplan, A S

    1990-01-01

    The diagnosis of depression in patients presenting with both depressive and physical symptoms is potentially confounded and problematic. The present study of 271 patients with four types of illness all with prominent physical symptoms--end-stage renal disease (n = 99), irritable bowel syndrome (n = 21), post-infectious neuromyasthenia (n = 25) and eating disorders (n = 126)--investigates if there are a group of symptoms on the Beck Depression Inventory (BDI) which predict the diagnosis of major depressive episode (MDE) made using the Diagnostic Interview Schedule (DIS). Discriminant function analysis of BDI responses yielded a four item function--self-hate, indecisiveness, loss of appetite and suicidal thoughts--which maximally discriminated between patients with and without a current MDE and correctly classified 75 percent of subjects. PMID:2265887

  16. Prominent electrochromism through vacancy-order melting in a complex oxide

    NASA Astrophysics Data System (ADS)

    Seidel, J.; Luo, W.; Suresha, S. J.; Nguyen, P.-K.; Lee, A. S.; Kim, S.-Y.; Yang, C.-H.; Pennycook, S. J.; Pantelides, S. T.; Scott, J. F.; Ramesh, R.

    2012-04-01

    Electrochromes are materials that have the ability to reversibly change from one colour state to another with the application of an electric field. Electrochromic colouration efficiency is typically large in organic materials that are not very stable chemically. Here we show that inorganic Bi0.9Ca0.1FeO3-0.05 thin films exhibit a prominent electrochromic effect arising from an intrinsic mechanism due to the melting of oxygen-vacancy ordering and the associated redistribution of carriers. We use a combination of optical characterization techniques in conjunction with high-resolution transmission electron microscopy and first-principles theory. The absorption change and colouration efficiency at the band edge (blue-cyan region) are 4.8×106 m-1 and 190 cm2 C-1, respectively, which are the highest reported values for inorganic electrochromes, even exceeding values of some organic materials.

  17. Action in Perception: Prominent Visuo-Motor Functional Symmetry in Musicians during Music Listening.

    PubMed

    Burunat, Iballa; Brattico, Elvira; Puoliväli, Tuomas; Ristaniemi, Tapani; Sams, Mikko; Toiviainen, Petri

    2015-01-01

    Musical training leads to sensory and motor neuroplastic changes in the human brain. Motivated by findings on enlarged corpus callosum in musicians and asymmetric somatomotor representation in string players, we investigated the relationship between musical training, callosal anatomy, and interhemispheric functional symmetry during music listening. Functional symmetry was increased in musicians compared to nonmusicians, and in keyboardists compared to string players. This increased functional symmetry was prominent in visual and motor brain networks. Callosal size did not significantly differ between groups except for the posterior callosum in musicians compared to nonmusicians. We conclude that the distinctive postural and kinematic symmetry in instrument playing cross-modally shapes information processing in sensory-motor cortical areas during music listening. This cross-modal plasticity suggests that motor training affects music perception. PMID:26422790

  18. H-alpha and H-beta emission in quiescent prominences

    NASA Technical Reports Server (NTRS)

    Landman, D. A.; Mongillo, M.

    1979-01-01

    High-resolution H-alpha and H-beta line profiles in a number of quiescent prominences were measured at positions of weak to moderate brightness (for H-alpha integrated intensity of not less than 1.35 x 10 to the 5th ergs/sq cm/s/sr). Those profiles that appear to originate primarily in a single physical element can be accurately fitted with a two-component model, each component being characterized by a temperature, a Gaussian microturbulence distribution, and a constant source function. The various values of integrated intensity, optical thickness, and Doppler width are compared with previous measurements and recent theoretical calculations; several discrepancies are noted and discussed.

  19. An analysis of concert saxophone vibrato through the examination of recordings by eight prominent soloists

    NASA Astrophysics Data System (ADS)

    Zinninger, Thomas

    This study examines concert saxophone vibrato through the analysis of several recordings of standard repertoire by prominent soloists. The vibrato of Vincent Abato, Arno Bornkamp, Claude Delangle, Jean-Marie Londeix, Marcel Mule, Otis Murphy, Sigurd Rascher, and Eugene Rousseau is analyzed with regards to rate, extent, shape, and discretionary use. Examination of these parameters was conducted through both general observation and precise measurements with the aid of a spectrogram. Statistical analyses of the results provide tendencies for overall vibrato use, as well as the effects of certain musical attributes (note length, tempo, dynamic, range) on vibrato. The results of this analysis are also compared among each soloist and against pre-existing theories or findings in vibrato research.

  20. The foxconn suicides and their media prominence: is the werther effect applicable in china?

    PubMed Central

    2011-01-01

    Background Media reporting of suicide and its relationship with actual suicide has rarely been investigated in Mainland China. The "Foxconn suicides" is a description referring to a string of suicides/attempts during 2010, all of which were related to a giant electrical manufacturing company, Foxconn. This study aimed to examine the clustering and copycat effects of the Foxconn suicides, and to investigate temporal patterns in how they were reported by the media in Mainland China, Hong Kong (HK), and Taiwan (TW). Methods Relevant articles were collected from representative newspapers published in three big cities in Mainland China (Beijing (BJ), Shenzhen (SZ), and Guangzhou (GZ)), HK, and TW, together with searching intensity data on the topic conducted using the Baidu search engine in Mainland China. The temporal clustering effects of the Foxconn suicides and their media prominence were assessed using the Kolmogorov-Smirnov test. The media reports of the Foxconn suicides' temporal patterns were explored using a nonparametric curve estimation method (that is, the local linear method). The potential mutual interactions between the Foxconn suicides and their media prominence were also examined, using logistic and Poisson regression methods. Results The results support a temporal clustering effect for the Foxconn suicides. The BJ-based newspapers' reporting and the occurrence of a Foxconn suicide/attempt are each found to be associated with an elevated chance of a further Foxconn suicide 3 days later. The occurrence of a Foxconn suicide also immediately influenced the intensity of both Baidu searching and newspaper reporting. Regional diversity in suicide reporting tempo-patterns within Mainland China, and similarities between HK and TW, are also demonstrated. Conclusions The Foxconn suicides were temporally clustered. Their occurrences were influenced by the reporting of BJ-based newspapers, and contagion within the company itself. Further suicide research and

  1. DYNAMICS OF VERTICAL THREADS AND DESCENDING KNOTS IN A HEDGEROW PROMINENCE

    SciTech Connect

    Chae, Jongchul

    2010-05-01

    The existence and behavior of vertical fine structures of plasma-threads and knots-are a significant observational clue to understanding the magnetic structure and dynamics of quiescent prominences on the quiet Sun. Based on the equation of motion in ideal MHD, we reason that the non-hydrostatic support of plasma against gravity in general requires either the motion of plasma with a high value of downward acceleration (dynamical support) or the role of horizontal magnetic fields (magnetic support). By carefully tracking the motion of several bright threads seen in a hedgerow prominence observed by the Solar Optical Telescope aboard Hinode, we confirm that these threads are essentially static and stable, which negates the dynamic support. The application of the Kippenhahn-Schlueter solution suggests that they may be supported by sagged magnetic field lines with a sag angle of about 43{sup 0}. We also track several bright descending knots and find that their descending speeds range from 10 to 30 km s{sup -1}, with a mean value of 16 km s{sup -1}, and their vertical accelerations from -0.10 to 0.10 km s{sup -2}, with a mean of practically zero. This finding suggests that these knots are basically supported by horizontal magnetic fields against gravity even when they descend, and the complex variations of their descending speeds should be attributed to small imbalances between gravity and the force of magnetic tension. Furthermore, some knots are observed to impulsively get accelerated downward from time to time. We conjecture that these impulsive accelerations are a result of magnetic reconnection and the subsequent interchange of magnetic configuration between a knot and its surrounding structure. It is proposed that this process of reconnection and interchange not only initiates the descending motion of the knots, but also allows knots to keep falling long distance through the medium permeated by horizontal magnetic fields.

  2. IRIS Observations of Coronal Rain and Prominences: Return Flows of the Chromosphere-Corona Mass Cycle

    NASA Astrophysics Data System (ADS)

    Liu, Wei; Berger, Thomas; Antolin, Patrick; Schrijver, Karel

    2014-06-01

    It has recently been recognized that a mass cycle (e.g., Berger et al. 2011; McIntosh et al. 2012) between the hot, tenuous solar corona and the cool, dense chromosphere underneath it plays an important role in the mass budget and dynamic evolution of the solar atmosphere. Although the corona ultimately loses mass through the solar wind and coronal mass ejections, a fraction of its mass returns to the chromosphere in coronal rain, downflows of prominences, and other as-yet unidentified processes. We present here analysis of joint observations of IRIS, SDO/AIA, and Hinode/SOT of such phenomena. By utilizing the wide temperature coverage (logT: 4 - 7) provided by these instruments combined, we track the coronal cooling sequence (e.g., Schrijver 2001; Liu et al. 2012; Berger et al. 2012) leading to the formation of such material at transition region or chromospheric temperatures (logT: 4 - 5) in the million-degree corona. We compare the cooling times with those expected from the radiative cooling instability. We also measure the kinematics and densities of such downflows and infer their mass fluxes, which are compared to the upward mass fluxes into the corona, e.g., those associated with spicules and flux emergence. Special attention is paid to coronal rain formed near cusp-shaped portions of coronal loops, funnel-shaped prominences at dips of coronal loops, and their respective magnetic environments. With the information about where and when such catastrophic cooling events take place, we discuss the implications for the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010).

  3. Relating a Prominence Observed from the Solar Optical Telescope on the Hinode Satellite to Known 3-D Structures of Filaments

    NASA Astrophysics Data System (ADS)

    Martin, S. F.; Panasenco, O.; Agah, Y.; Engvold, O.; Lin, Y.

    2009-12-01

    We address only a first step in relating limb and disk observations by illustrating and comparing the spines and barbs of three different quiescent prominences and filaments observed in Hα by three different telescopes. Although the appearance of the three quiescent prominences is quite different, we show that each consists of a spine, barbs extending from the spine, and arcs at the base of some of the curtains of barb threads.

  4. Dynamics of quiescent prominence fine structures analyzed by 2D non-LTE modelling of the Hα line

    NASA Astrophysics Data System (ADS)

    Gunár, S.; Mein, P.; Schmieder, B.; Heinzel, P.; Mein, N.

    2012-07-01

    Aims: We analyze the dynamics of the prominence fine structures of a quiescent prominence observed on April 26, 2007 during a coordinated campaign of several spaceborne and ground-based instruments. We use Lyman spectra observed by SOHO/SUMER and the Hα line spectra obtained by MSDP spectrograph working at the Meudon Solar Tower. Methods: We employ the 2D multi-thread prominence fine-structure modelling that includes randomly distributed line-of-sight (LOS) velocities of individual threads to derive models producing synthetic Lyman lines in good agreement with the SOHO/SUMER observations. We then use these models to produce synthetic Hα line spectra that we compare with the observed spectra using three statistical parameters: the line integrated intensity, the line full-width at half-maximum (FWHM), and the Doppler velocity derived from shifts of the line profiles. Results: We demonstrate that the 2D multi-thread models that produce synthetic Lyman spectra in agreement with observations also generate synthetic Hα spectra in good agreement with the observed ones. The statistical analysis of the FWHM and Doppler velocities of the synthetic Hα line profiles show that the overall LOS velocities in the April 26, 2007 prominence at the time of the observations were below 15 km s-1 and in the prominence core were close to 10 km s-1. In combination with the analysis of the Lyman spectra, we determine several physical parameters of the observed prominence fine-structures that show that the April 26, 2007 prominence had a relatively low-mass weakly magnetized structure. We are also able to impose some constraints on the prominence core temperature, which may be relatively low, with values below 6000 K. Conclusions: The combination of 2D non-LTE prominence fine-structure modelling with the statistical analysis of the observed and synthetic Lyman and Hα spectra allows us to analyze the influence of the model input parameters and the velocity fields on the synthetic H

  5. Prominent reflector beneath around the segmentation boundary between Tonankai-Nankai earthquake area

    NASA Astrophysics Data System (ADS)

    Nakanishi, A.; Shimomura, N.; Fujie, G.; Kodaira, S.; Obana, K.; Takahashi, T.; Yamamoto, Y.; Yamashita, M.; Takahashi, N.; Kaneda, Y.; Mochizuki, K.; Kato, A.; Iidaka, T.; Kurashimo, E.; Shinohara, M.; Takeda, T.; Shiomi, K.

    2013-12-01

    In the Nankai Trough subduction seismogenic zone, the Nankai and Tonankai earthquakes had often occurred simultaneously, and caused a great event. In most cases, first break of such large events of Nankai Trough usually begins from southwest off the Kii Peninsula so far. The idea of split Philippine Sea plate between the Kii Peninsula and the Shikoku Island, which explains seismicity, tectonic background, receiver function image and historical plate motion, was previously suggested. Moreover, between the Kii Peninsula and the Shikoku Island, there is a gap of deep low-frequency events observed in the belt-like zone along the strike of the subducting Philippine Sea plate. In 2010 and 2011, we conducted the large-scale high-resolution wide-angle and reflection (MCS) seismic study, and long-term observation from off Shikoku and Kii Peninsula. Marine active source seismic data have been acquired along grid two-dimensional profiles having the total length of ~800km/year. A three-dimensional seismic tomography using active and passive seismic data observed both land and ocean bottom stations have been also performed. From those data, we found a possible prominent reflector imaged in the offshore side in the Kii channel at the depth of ~18km. The velocity just beneath the reflector cannot be determined due to the lack of ray paths. Based of the amplitude information, we interpret the reflector as the forearc Moho based on the velocity gap (from ~6.4km/s to ~7.4km/s). However, the reflector is shallower than the forearc Moho of other area along the Nankai Trough. Similar reflectors are recognized along other seismic profiles around the Kii channel. In this presentation, we will show the result of structure analysis to understand the peculiar structure including the prominent reflector around the Kii channel. Relation between the structure and the existence of the segmentation of the Nankai megathrust earthquake or seismic gap of the deep low-frequency events will be also

  6. OBSERVATIONS OF LINEAR POLARIZATION IN A SOLAR CORONAL LOOP PROMINENCE SYSTEM OBSERVED NEAR 6173 Å

    SciTech Connect

    Saint-Hilaire, Pascal; Martínez Oliveros, Juan-Carlos; Hudson, Hugh S.; Krucker, Säm; Bain, Hazel; Schou, Jesper; Couvidat, Sébastien

    2014-05-10

    White-light observations by the Solar Dynamics Observatory's Helioseismic and Magnetic Imager of a loop-prominence system occurring in the aftermath of an X-class flare on 2013 May 13 near the eastern solar limb show a linearly polarized component, reaching up to ∼20% at an altitude of ∼33 Mm, about the maximum amount expected if the emission were due solely to Thomson scattering of photospheric light by the coronal material. The mass associated with the polarized component was 8.2 × 10{sup 14} g. At 15 Mm altitude, the brightest part of the loop was 3(±0.5)% linearly polarized, only about 20% of that expected from pure Thomson scattering, indicating the presence of an additional unpolarized component at wavelengths near Fe I (617.33 nm). We estimate the free electron density of the white-light loop system to possibly be as high as 1.8 × 10{sup 12} cm{sup –3}.

  7. Temperature and Extreme-ultraviolet Intensity in a Coronal Prominence Cavity and Streamer

    NASA Astrophysics Data System (ADS)

    Kucera, T. A.; Gibson, S. E.; Schmit, D. J.; Landi, E.; Tripathi, D.

    2012-09-01

    We analyze the temperature and EUV line emission of a coronal cavity and surrounding streamer in terms of a morphological forward model. We use a series of iron line ratios observed with the Hinode Extreme-ultraviolet Imaging Spectrograph (EIS) on 2007 August 9 to constrain temperature as a function of altitude in a morphological forward model of the streamer and cavity. We also compare model predictions to the EIS EUV line intensities and polarized brightness (pB) data from the Mauna Loa Solar Observatory (MLSO) Mark 4 K-coronameter. This work builds on earlier analysis using the same model to determine geometry of and density in the same cavity and streamer. The fit to the data with altitude-dependent temperature profiles indicates that both the streamer and cavity have temperatures in the range 1.4-1.7 MK. However, the cavity exhibits substantial substructure such that the altitude-dependent temperature profile is not sufficient to completely model conditions in the cavity. Coronal prominence cavities are structured by magnetism so clues to this structure are to be found in their plasma properties. These temperature substructures are likely related to structures in the cavity magnetic field. Furthermore, we find that the model overestimates the EUV line intensities by a factor of 4-10, without overestimating pB. We discuss this difference in terms of filling factors and uncertainties in density diagnostics and elemental abundances.

  8. Yolk sac tumor with a prominent polyvesicular vitelline pattern: a report of three cases.

    PubMed

    Young, Robert H; Ulbright, Thomas M; Policarpio-Nicolas, Maria Luisa C

    2013-03-01

    We report 3 cases of the rare polyvesicular vitelline variant of ovarian yolk sac tumor (YST). The patients were 23, 29, and 43 years old, and all presented with large unilateral adnexal masses confined to the ovary. One tumor was predominantly cystic, and the other 2 had prominent cystic components; all 3 also had solid components. Microscopic examination of the cystic regions showed dilated cysts that largely effaced the stroma resulting in a honeycomb-like appearance. The solid foci were characterized predominantly by small tubules in a fibrous stroma; the tubules exhibited variably conspicuous cystic dilatation to merge with the microcystic appearance. The tumor cells varied from large and primitive-appearing to flattened and deceptively innocuous when lining large cysts. They were immunoreactive for α-fetoprotein and glypican-3. Non-polyvesicular vitelline components of YST were present focally in 2 cases (hepatoid in one, reticular and endometrioid like in the second). Two patients are disease free after 20 and 26 years, respectively; disease-free follow-up is of short duration in the third case (2 years). The good long-term outcome in 2 cases supports prior evidence that suggests that the natural history of this form of YST may be more indolent than conventional forms of the tumor. PMID:23348213

  9. Developing legally defensible physiological employment standards for prominent physically demanding public safety occupations: a Canadian perspective.

    PubMed

    Jamnik, V; Gumienak, R; Gledhill, N

    2013-10-01

    Canadian court decisions and human rights legislation impose strict legal criteria for developing applicant and incumbent physiological employment standards to qualify as a bona fide occupational requirement. These legal criteria compel researchers and employers to ensure that the standards are criterion-based and validly linked to the critical life threatening physically demanding tasks of the occupation, and this has led to the establishment of a systematic research process template to ensure this connection. Validation of job-related physiological employment standards is achieved using both construct and content procedures and reliability is established via test-retest procedures. The 1999 Supreme Court of Canada Meiorin Decision also obliges employers to demonstrate that it is impossible to accommodate an individual applicant or employee who is adversely impacted by lowering the physiological employment standards without imposing undue hardship on the employer. Recent evidence has demonstrated convincingly that familiarization opportunities, motivational feedback/coaching during test performance, and participation in a 6-week job-specific physical fitness training program can overcome the adverse impact of a physiological employment standards on a sub-group of participants, thereby providing "de facto" accommodation. In this article, the authors review the physiological employment standards for prominent Canadian physically demanding public safety occupations; police, correctional officers, nuclear emergency personnel, structural fire fighters, and wildland fire fighters, to illustrate the steps, challenges, and solutions involved in developing and implementing physiological employment standards designed to meet the requirements to qualify as a bona fide occupational requirement. PMID:23494548

  10. Coordinate Regulation of Glycan Degradation and Polysaccharide Capsule Biosynthesis by a Prominent Human Gut Symbiont*

    PubMed Central

    Martens, Eric C.; Roth, Robyn; Heuser, John E.; Gordon, Jeffrey I.

    2009-01-01

    Bacteria in the distal human gut have evolved diverse abilities to metabolize complex glycans, including the capacity to degrade these compounds as nutrients and to assemble their component sugars into new polymers such as extracellular capsules. The human gut bacterium Bacteroides thetaiotaomicron is well endowed with the ability to metabolize both host- and diet-derived glycans. Its genome contains 88 different polysaccharide utilization loci (PULs) for complex glycan catabolism and eight different gene clusters for capsular polysaccharide biosynthesis. Here, we investigate one of the prominent mechanisms by which this gut symbiont regulates many PULs involved in host mucin O-glycan degradation; namely, transcriptional regulation via the concerted interactions of cell-envelope-localized TonB-dependent transporters, extra-cytoplasmic function σ factors and anti-σ factors, which participate together in a regulatory pathway termed trans-envelope signaling. Unexpectedly, we found that several different trans-envelope signaling switches involved in PUL-mediated O-glycan degradation also modulate capsular polysaccharide synthesis. A novel regulatory pathway, which is dependent on expression of O-glycan-targeting outer membrane proteins, governs this coordinated regulation of glycan catabolism and capsule synthesis. This latter finding provides a new link in the dynamic interplay between complex glycan metabolism, microbial physiology, and host responses that occurs during colonization of the gut. PMID:19403529

  11. Prominent role of exopeptidase DPP III in estrogen-mediated protection against hyperoxia in vivo

    PubMed Central

    Sobočanec, Sandra; Filić, Vedrana; Matovina, Mihaela; Majhen, Dragomira; Šafranko, Željka Mačak; Hadžija, Marijana Popović; Krsnik, Željka; Kurilj, Andrea Gudan; Šarić, Ana; Abramić, Marija; Balog, Tihomir

    2016-01-01

    A number of age-related diseases have a low incidence in females, which is attributed to a protective effect of sex hormones. For instance, the female sex hormone estrogen (E2) has a well established cytoprotective effect against oxidative stress, which strongly contributes to ageing. However, the mechanism by which E2 exerts its protective activity remains elusive. In this study we address the question whether the E2-induced protective effect against hyperoxia is mediated by the Nrf-2/Keap-1 signaling pathway. In particular, we investigate the E2-induced expression and cellular distribution of DPP III monozinc exopeptidase, a member of the Nrf-2/Keap-1 pathway, upon hyperoxia treatment. We find that DPP III accumulates in the nucleus in response to hyperoxia. Further, we show that combined induction of hyperoxia and E2 administration have an additive effect on the nuclear accumulation of DPP III. The level of nuclear accumulation of DPP III is comparable to nuclear accumulation of Nrf-2 in healthy female mice exposed to hyperoxia. In ovariectomized females exposed to hyperoxia, supplementation of E2 induced upregulation of DPP III, Ho-1, Sirt-1 and downregulation of Ppar-γ. While other cytoprotective mechanisms cannot be excluded, these findings demonstrate a prominent role of DPP III, along with Sirt-1, in the E2-mediated protection against hyperoxia. PMID:26774752

  12. Spatial Gene-Expression Gradients Underlie Prominent Heterogeneity of CA1 Pyramidal Neurons.

    PubMed

    Cembrowski, Mark S; Bachman, Julia L; Wang, Lihua; Sugino, Ken; Shields, Brenda C; Spruston, Nelson

    2016-01-20

    Tissue and organ function has been conventionally understood in terms of the interactions among discrete and homogeneous cell types. This approach has proven difficult in neuroscience due to the marked diversity across different neuron classes, but it may be further hampered by prominent within-class variability. Here, we considered a well-defined canonical neuronal population—hippocampal CA1 pyramidal cells (CA1 PCs)—and systematically examined the extent and spatial rules of transcriptional heterogeneity. Using next-generation RNA sequencing, we identified striking variability in CA1 PCs, such that the differences within CA1 along the dorsal-ventral axis rivaled differences across distinct pyramidal neuron classes. This variability emerged from a spectrum of continuous gene-expression gradients, producing a transcriptional profile consistent with a multifarious continuum of cells. This work reveals an unexpected amount of variability within a canonical and narrowly defined neuronal population and suggests that continuous, within-class heterogeneity may be an important feature of neural circuits. PMID:26777276

  13. Helioseismic and Magnetic Imager Observations of Linear Polarization from a Loop Prominence System

    NASA Astrophysics Data System (ADS)

    Saint-Hilaire, Pascal; Schou, Jesper; Martinez Oliveros, Juan Carlos; Hudson, Hugh S.; Krucker, Sam; Bain, Hazel; Couvidat, Sebastien

    2014-06-01

    White-light observations by the Solar Dynamics Observatory's Helioseismic and Magnetic Imager of a loop-prominence system occurring in the aftermath of an X-class flare on 2013 May 13 near the eastern solar limb show a linearly polarized component, reaching up to 20% at an altitude of 33 Mm, about the maximal amount expected if the emission were due solely to Thomson scattering of photospheric light by the coronal material. The mass associated with the polarized component was 8.2x10^14 g. At 15 Mm altitude, the brightest part of the loop was 3(+/-0.5)% linearly polarized, only about 20% of that expected from pure Thomson scattering, indicating the presence of an additional unpolarized component at wavelengths near Fe I (617.33 nm), probably thermal emission. We estimated the free electron density of the white-light loop system to possibly be as high as 1.8x10^12 cm^-3.

  14. The Effects of Magnetic-field Geometry on Longitudinal Oscillaitons of Solar Prominences

    NASA Technical Reports Server (NTRS)

    Luna, M.; Diaz, A. J.; Karpen, J.

    2013-01-01

    We investigate the influence of the geometry of the solar filament magnetic structure on the large-amplitude longitudinal oscillations. A representative filament flux tube is modeled as composed of a cool thread centered in a dipped part with hot coronal regions on either side.We have found the normal modes of the system and establish that the observed longitudinal oscillations are well described with the fundamental mode. For small and intermediate curvature radii and moderate to large density contrast between the prominence and the corona, the main restoring force is the solar gravity. In this full wave description of the oscillation a simple expression for the oscillation frequencies is derived in which the pressure-driven term introduces a small correction. We have also found that the normal modes are almost independent of the geometry of the hot regions of the tube. We conclude that observed large-amplitude longitudinal oscillations are driven by the projected gravity along the flux tubes and are strongly influenced by the curvature of the dips of the magnetic field in which the threads reside.

  15. Acoustic markers of prominence influence infants' and adults' segmentation of speech sequences.

    PubMed

    Bion, Ricardo A H; Benavides-Varela, Silvia; Nespor, Marina

    2011-03-01

    Two experiments investigated the way acoustic markers of prominence influence the grouping of speech sequences by adults and 7-month-old infants. In the first experiment, adults were familiarized with and asked to memorize sequences of adjacent syllables that alternated in either pitch or duration. During the test phase, participants heard pairs of syllables with constant pitch and duration and were asked whether the syllables had appeared adjacently during familiarization. Adults were better at remembering pairs of syllables that during familiarization had short syllables preceding long syllables, or high-pitched syllables preceding low-pitched syllables. In the second experiment, infants were familiarized and tested with similar stimuli as in the first experiment, and their preference for pairs of syllables was accessed using the head-turn preference paradigm.When familiarized with syllables alternating in pitch, infants showed a preference to listen to pairs of syllables that had high pitch in the first syllable. However, no preference was found when the familiarization stream alternated in duration. It is proposed that these perceptual biases help infants and adults find linguistic units in the continuous speech stream.While the bias for grouping based on pitch appears early in development, biases for durational grouping might rely on more extensive linguistic experience. PMID:21524015

  16. N-acetyl-L-histidine, a Prominent Biomolecule in Brain and Eye of Poikilothermic Vertebrates.

    PubMed

    Baslow, Morris H; Guilfoyle, David N

    2015-01-01

    N-acetyl-L-histidine (NAH) is a prominent biomolecule in brain, retina and lens of poikilothermic vertebrates. In fish lens, NAH exhibits an unusual compartmentalized metabolism. It is synthesized from L-histidine (His) and acetyl Co-enzyme A. However, NAH cannot be catabolized by lens cells. For its hydrolysis, NAH is exported to ocular fluid where a specific acylase cleaves His which is then actively taken up by lens and re-synthesized into NAH. This energy-dependent cycling suggested a pump mechanism operating at the lens/ocular fluid interface. Additional studies led to the hypothesis that NAH functioned as a molecular water pump (MWP) to maintain a highly dehydrated lens and avoid cataract formation. In this process, each NAH molecule released to ocular fluid down its gradient carries with it 33 molecules of bound water, effectively transporting the water against a water gradient. In ocular fluid the bound water is released for removal from the eye by the action of NAH acylase. In this paper, we demonstrate for the first time the identification of NAH in fish brain using proton magnetic resonance spectroscopy (MRS) and describe recent evidence supporting the NAH MWP hypothesis. Using MRS, we also document a phylogenetic transition in brain metabolism between poikilothermic and homeothermic vertebrates. PMID:25919898

  17. N-acetyl-l-histidine, a Prominent Biomolecule in Brain and Eye of Poikilothermic Vertebrates

    PubMed Central

    Baslow, Morris H.; Guilfoyle, David N.

    2015-01-01

    N-acetyl-l-histidine (NAH) is a prominent biomolecule in brain, retina and lens of poikilothermic vertebrates. In fish lens, NAH exhibits an unusual compartmentalized metabolism. It is synthesized from l-histidine (His) and acetyl Co-enzyme A. However, NAH cannot be catabolized by lens cells. For its hydrolysis, NAH is exported to ocular fluid where a specific acylase cleaves His which is then actively taken up by lens and re-synthesized into NAH. This energy-dependent cycling suggested a pump mechanism operating at the lens/ocular fluid interface. Additional studies led to the hypothesis that NAH functioned as a molecular water pump (MWP) to maintain a highly dehydrated lens and avoid cataract formation. In this process, each NAH molecule released to ocular fluid down its gradient carries with it 33 molecules of bound water, effectively transporting the water against a water gradient. In ocular fluid the bound water is released for removal from the eye by the action of NAH acylase. In this paper, we demonstrate for the first time the identification of NAH in fish brain using proton magnetic resonance spectroscopy (MRS) and describe recent evidence supporting the NAH MWP hypothesis. Using MRS, we also document a phylogenetic transition in brain metabolism between poikilothermic and homeothermic vertebrates. PMID:25919898

  18. Dynamics of coronal rain and descending plasma blobs in solar prominences. I. Fully ionized case

    SciTech Connect

    Oliver, R.; Soler, R.; Terradas, J.; Zaqarashvili, T. V.; Khodachenko, M. L.

    2014-03-20

    Observations of active regions and limb prominences often show cold, dense blobs descending with an acceleration smaller than that of free fall. The dynamics of these condensations falling in the solar corona is investigated in this paper using a simple fully ionized plasma model. We find that the presence of a heavy condensation gives rise to a dynamical rearrangement of the coronal pressure that results in the formation of a large pressure gradient that opposes gravity. Eventually this pressure gradient becomes so large that the blob acceleration vanishes or even points upward. Then, the blob descent is characterized by an initial acceleration phase followed by an essentially constant velocity phase. These two stages can be identified in published time-distance diagrams of coronal rain events. Both the duration of the first stage and the velocity attained by the blob increase for larger values of the ratio of blob to coronal density, for larger blob mass, and for smaller coronal temperature. Dense blobs are characterized by a detectable density growth (up to 60% in our calculations) and by a steepening of the density in their lower part, that could lead to the formation of a shock. They also emit sound waves that could be detected as small intensity changes with periods of the order of 100 s and lasting between a few and about 10 periods. Finally, the curvature of falling paths with large radii is only relevant when a very dense blob falls along inclined magnetic field lines.

  19. Study of Distribution and Asymmetry of Solar Active Prominences during Solar Cycle 23

    NASA Astrophysics Data System (ADS)

    Joshi, Navin Chandra; Bankoti, Neeraj Singh; Pande, Seema; Pande, Bimal; Pandey, Kavita

    2009-12-01

    In this article we present the results of a study of the spatial distribution and asymmetry of solar active prominences (SAP) for the period 1996 through 2007 (solar cycle 23). For more meaningful statistical analysis we analyzed the distribution and asymmetry of SAP in two subdivisions viz. Group1 (ADF, APR, DSF, CRN, CAP) and Group2 (AFS, ASR, BSD, BSL, DSD, SPY, LPS). The North - South (N - S) latitudinal distribution shows that the SAP events are most prolific in the 21° to 30° slice in the Northern and Southern Hemispheres; the East - West (E - W) longitudinal distribution study shows that the SAP events are most prolific (best observable) in the 81° to 90° slice in the Eastern and Western Hemispheres. It was found that the SAP activity during this cycle is low compared to previous solar cycles. The present study indicates that during the rising phase of the cycle the number of SAP events are roughly equal in the Northern and Southern Hemispheres. However, activity in the Southern Hemisphere has been dominant since 1999. Our statistical study shows that the N - S asymmetry is more significant then the E - W asymmetry.

  20. The coordination of boundary tones and its interaction with prominence1

    PubMed Central

    Katsika, Argyro; Krivokapić, Jelena; Mooshammer, Christine; Tiede, Mark; Goldstein, Louis

    2014-01-01

    This study investigates the coordination of boundary tones as a function of stress and pitch accent. Boundary tone coordination has not been experimentally investigated previously, and the effect of prominence on this coordination, and whether it is lexical (stress-driven) or phrasal (pitch accent-driven) in nature is unclear. We assess these issues using a variety of syntactic constructions to elicit different boundary tones in an Electromagnetic Articulography (EMA) study of Greek. The results indicate that the onset of boundary tones co-occurs with the articulatory target of the final vowel. This timing is further modified by stress, but not by pitch accent: boundary tones are initiated earlier in words with non-final stress than in words with final stress regardless of accentual status. Visual data inspection reveals that phrase-final words are followed by acoustic pauses during which specific articulatory postures occur. Additional analyses show that these postures reach their achievement point at a stable temporal distance from boundary tone onsets regardless of stress position. Based on these results and parallel findings on boundary lengthening reported elsewhere, a novel approach to prosody is proposed within the context of Articulatory Phonology: rather than seeing prosodic (lexical and phrasal) events as independent entities, a set of coordination relations between them is suggested. The implications of this account for prosodic architecture are discussed. PMID:25300341

  1. How Is RAN Related to Reading Fluency? A Comprehensive Examination of the Prominent Theoretical Accounts.

    PubMed

    Papadopoulos, Timothy C; Spanoudis, George C; Georgiou, George K

    2016-01-01

    We examined the prominent theoretical explanations of the RAN-reading relationship in a relatively transparent language (Greek) in a sample of children (n = 286) followed from Grade 1 to Grade 2. Specifically, we tested the fit of eight different models, as defined by the type of reading performance predicted (oral vs. silent word reading fluency), the type of RAN tasks (non-alphanumeric vs. alphanumeric), and the RAN effects (direct vs. indirect). Working memory, attention, processing speed, and motor skills were used as "common cause" variables predicting both RAN and reading fluency and phonological awareness and orthographic processing were used as mediators of RAN's effects on reading fluency. The findings of both concurrent and longitudinal analyses indicated that RAN is a unique predictor of oral reading fluency, but not silent reading fluency. Using alphanumeric or non-alphanumeric RAN did not particularly affect the RAN-reading relationship. Both phonological awareness and orthographic processing partly mediated RAN's effects on reading fluency. Theoretical implications of these findings are discussed. PMID:27605918

  2. Targeting frequent users of emergency departments: Prominent risk factors and policy implications.

    PubMed

    Leporatti, Lucia; Ameri, Marta; Trinchero, Chiara; Orcamo, Patrizia; Montefiori, Marcello

    2016-05-01

    This study investigates the characteristics of frequent users of accident and emergency departments (AEDs) and recommends alternative medical services for such patients. Prominent demographic and clinical risk factors for individuals accessing seven AEDs located in the metropolitan area of Genoa, Italy are identified and analysed. A truncated count data model is implemented to establish the determinants of access, while a multinomial logistic regression is used to highlight potential differences among different user categories. According to previous studies, empirical findings suggest that despite the relevance of demographic drivers, vulnerability conditions (e.g. abuse of alcohol and drugs, chronic conditions, and psychological distress) are the main reasons behind frequent AED use; the analysis seems to confirm an association between AED frequent use and lower level of urgency. Since frequent and highly frequent users are found responsible for disproportionate resource absorption with respect to total amount of AED costs (they represent roughly 10% of the total number of patients, but contribute to more than 19% of the total annual AED cost), policies aiming to reduce frequent use of AEDs could bring significant savings in economic resources. Thus, efficient actions could be oriented toward extending primary care services outside AED and toward instituting local aid services specifically addressed to people under the influence of substances or in conditions of mental distress. PMID:27033015

  3. TEMPERATURE AND EXTREME-ULTRAVIOLET INTENSITY IN A CORONAL PROMINENCE CAVITY AND STREAMER

    SciTech Connect

    Kucera, T. A.; Tripathi, D.

    2012-09-20

    We analyze the temperature and EUV line emission of a coronal cavity and surrounding streamer in terms of a morphological forward model. We use a series of iron line ratios observed with the Hinode Extreme-ultraviolet Imaging Spectrograph (EIS) on 2007 August 9 to constrain temperature as a function of altitude in a morphological forward model of the streamer and cavity. We also compare model predictions to the EIS EUV line intensities and polarized brightness (pB) data from the Mauna Loa Solar Observatory (MLSO) Mark 4 K-coronameter. This work builds on earlier analysis using the same model to determine geometry of and density in the same cavity and streamer. The fit to the data with altitude-dependent temperature profiles indicates that both the streamer and cavity have temperatures in the range 1.4-1.7 MK. However, the cavity exhibits substantial substructure such that the altitude-dependent temperature profile is not sufficient to completely model conditions in the cavity. Coronal prominence cavities are structured by magnetism so clues to this structure are to be found in their plasma properties. These temperature substructures are likely related to structures in the cavity magnetic field. Furthermore, we find that the model overestimates the EUV line intensities by a factor of 4-10, without overestimating pB. We discuss this difference in terms of filling factors and uncertainties in density diagnostics and elemental abundances.

  4. Dynamics of Coronal Rain and Descending Plasma Blobs in Solar Prominences. II. Partially Ionized Case

    NASA Astrophysics Data System (ADS)

    Oliver, R.; Soler, R.; Terradas, J.; Zaqarashvili, T. V.

    2016-02-01

    Coronal rain clumps and prominence knots are dense condensations with chromospheric to transition region temperatures that fall down in the much hotter corona. Their typical speeds are in the range 30-150 km s-1 and of the order of 10-30 km s-1, respectively, i.e., they are considerably smaller than free-fall velocities. These cold blobs contain a mixture of ionized and neutral material that must be dynamically coupled in order to fall together, as observed. We investigate this coupling by means of hydrodynamic simulations in which the coupling arises from the friction between ions and neutrals. The numerical simulations presented here are an extension of those of Oliver et al. to the partially ionized case. We find that, although the relative drift speed between the two species is smaller than 1 m s-1 at the blob center, it is sufficient to produce the forces required to strongly couple charged particles and neutrals. The ionization degree has no discernible effect on the main results of our previous work for a fully ionized plasma: the condensation has an initial acceleration phase followed by a period with roughly constant velocity, and, in addition, the maximum descending speed is clearly correlated with the ratio of initial blob to environment density.

  5. Mass Estimates of Rapidly Moving Prominence Material from High-cadence EUV Images

    NASA Astrophysics Data System (ADS)

    Williams, David R.; Baker, Deborah; van Driel-Gesztelyi, Lidia

    2013-02-01

    We present a new method for determining the column density of erupting filament material using state-of-the-art multi-wavelength imaging data. Much of the prior work on filament/prominence structure can be divided between studies that use a polychromatic approach with targeted campaign observations and those that use synoptic observations, frequently in only one or two wavelengths. The superior time resolution, sensitivity, and near-synchronicity of data from the Solar Dynamics Observatory's Advanced Imaging Assembly allow us to combine these two techniques using photoionization continuum opacity to determine the spatial distribution of hydrogen in filament material. We apply the combined techniques to SDO/AIA observations of a filament that erupted during the spectacular coronal mass ejection on 2011 June 7. The resulting "polychromatic opacity imaging" method offers a powerful way to track partially ionized gas as it erupts through the solar atmosphere on a regular basis, without the need for coordinated observations, thereby readily offering regular, realistic mass-distribution estimates for models of these erupting structures.

  6. How Is RAN Related to Reading Fluency? A Comprehensive Examination of the Prominent Theoretical Accounts

    PubMed Central

    Papadopoulos, Timothy C.; Spanoudis, George C.; Georgiou, George K.

    2016-01-01

    We examined the prominent theoretical explanations of the RAN-reading relationship in a relatively transparent language (Greek) in a sample of children (n = 286) followed from Grade 1 to Grade 2. Specifically, we tested the fit of eight different models, as defined by the type of reading performance predicted (oral vs. silent word reading fluency), the type of RAN tasks (non-alphanumeric vs. alphanumeric), and the RAN effects (direct vs. indirect). Working memory, attention, processing speed, and motor skills were used as “common cause” variables predicting both RAN and reading fluency and phonological awareness and orthographic processing were used as mediators of RAN's effects on reading fluency. The findings of both concurrent and longitudinal analyses indicated that RAN is a unique predictor of oral reading fluency, but not silent reading fluency. Using alphanumeric or non-alphanumeric RAN did not particularly affect the RAN-reading relationship. Both phonological awareness and orthographic processing partly mediated RAN's effects on reading fluency. Theoretical implications of these findings are discussed. PMID:27605918

  7. Prominent role of exopeptidase DPP III in estrogen-mediated protection against hyperoxia in vivo.

    PubMed

    Sobočanec, Sandra; Filić, Vedrana; Matovina, Mihaela; Majhen, Dragomira; Šafranko, Željka Mačak; Hadžija, Marijana Popović; Krsnik, Željka; Kurilj, Andrea Gudan; Šarić, Ana; Abramić, Marija; Balog, Tihomir

    2016-08-01

    A number of age-related diseases have a low incidence in females, which is attributed to a protective effect of sex hormones. For instance, the female sex hormone estrogen (E2) has a well established cytoprotective effect against oxidative stress, which strongly contributes to ageing. However, the mechanism by which E2 exerts its protective activity remains elusive. In this study we address the question whether the E2-induced protective effect against hyperoxia is mediated by the Nrf-2/Keap-1 signaling pathway. In particular, we investigate the E2-induced expression and cellular distribution of DPP III monozinc exopeptidase, a member of the Nrf-2/Keap-1 pathway, upon hyperoxia treatment. We find that DPP III accumulates in the nucleus in response to hyperoxia. Further, we show that combined induction of hyperoxia and E2 administration have an additive effect on the nuclear accumulation of DPP III. The level of nuclear accumulation of DPP III is comparable to nuclear accumulation of Nrf-2 in healthy female mice exposed to hyperoxia. In ovariectomized females exposed to hyperoxia, supplementation of E2 induced upregulation of DPP III, Ho-1, Sirt-1 and downregulation of Ppar-γ. While other cytoprotective mechanisms cannot be excluded, these findings demonstrate a prominent role of DPP III, along with Sirt-1, in the E2-mediated protection against hyperoxia. PMID:26774752

  8. Radiative modeling of solar prominences, two-dimensional transfer plus partial frequency redistribution

    NASA Astrophysics Data System (ADS)

    Paletou, F.; Vial, Jean-Claude; Auer, L. H.

    1992-11-01

    The two dimensional (2D) PRD (Partial Redistribution) radiative transfer code of Auer and Paletou was used to compute the resonance lines of HI, MgII and CaII in quiescent prominences, which are modeled as isothermal freestanding slabs illuminated from the sides as well as from below. PRD and 2D effects are evidenced and compared to Complete Redistribution (CRD) computations for both 1D and 2D geometries. Important edge variations are found at the bottom and the top that should be observed with a spatial resolution of one arcsecond. As in 1D, PRD effects allow for greater penetration of the incident radiation into the layer. The 2D code computes both the radial emergent intensity and the amount of radiation backscattered into the chromosphere. It can accordingly, be used to estimate the visibility of filaments. It will be of special interest to build nonisothermal models and compare, for example the Ly alpha profiles with the SUMER/SOHO (Solar Ultraviolet Measurement of Emitted Radiation)/(Solar and Heliospheric Observatory) observations.

  9. Prominent scapulae mimicking an inherited myopathy expands the phenotype of CHD7-related disease.

    PubMed

    O'Grady, Gina L; Ma, Alan; Sival, Deborah; Wong, Monica T Y; Peduto, Tony; Menezes, Manoj P; Young, Helen; Waddell, Leigh; Ghaoui, Roula; Needham, Merrilee; Lek, Monkol; North, Kathryn N; MacArthur, Daniel G; van Ravenswaaij-Arts, Conny Ma; Clarke, Nigel F

    2016-08-01

    CHD7 variants are a well-established cause of CHARGE syndrome, a disabling multi-system malformation disorder that is often associated with deafness, visual impairment and intellectual disability. Less severe forms of CHD7-related disease are known to exist, but the full spectrum of phenotypes remains uncertain. We identified a de novo missense variant in CHD7 in a family presenting with musculoskeletal abnormalities as the main manifestation of CHD7-related disease, representing a new phenotype. The proband presented with prominent scapulae, mild shoulder girdle weakness and only subtle dysmorphic features. Investigation revealed hypoplasia of the trapezius and sternocleidomastoid muscles and semicircular canal defects, but he did not fulfill diagnostic criteria for CHARGE syndrome. Although the shoulders are often sloping and anteverted in CHARGE syndrome, the underlying neuromuscular cause has never been investigated. This report expands the phenotypes associated with CHD7 mutations to include a musculoskeletal presentation, with hypoplasia of the shoulder and neck muscles. CHD7 should be considered in patients presenting in childhood with stable scapular winging, particularly if accompanied by dysmorphic features and balance difficulties. PMID:26813943

  10. A modification of incisionless otoplasty for correcting the prominent ear deformity.

    PubMed

    Haytoglu, Suheyl; Haytoglu, Tahir Gokhan; Yildirim, Ilhami; Arikan, Osman Kursat

    2015-11-01

    This article describes a modification of the incisionless otoplasty. We investigated the complication rates, recurrence risks, and patient satisfaction with this modified procedure. In total, 26 patients (49 ears) complaining of prominent ear were operated on. Auriculocephalic distances were measured at three different levels, pre-operatively, at the end of the surgery, and at 4 weeks and 6 months after surgery to evaluate the efficacy of the technique. Patient satisfaction was evaluated using a visual analog scale and the global aesthetic improvement scale was applied by an independent non-participating plastic surgeon at 6 months after the surgery. The mean loss of medialization was ~1 mm at 4 weeks after surgery and 2 mm at 6 months after surgery for all levels. According to visual analog scale, patient or parent satisfaction increased significantly. The global aesthetic improvement scale rated the patients as 93.9% "improved" and 6.1% as "no change." No rating was "worse." There are many advantages of this technique. The operation is not time-consuming, does not require a dressing, and it can be performed in adults with local anesthesia under office conditions, with no need for hospitalization. After the operation, patients can return to their daily activities immediately. It is associated with a low complication rate and high patient satisfaction. This technique is a good option for otoplasty in patients with isolated, inadequate development of anti-helical ridge, and with soft auricular cartilage. PMID:25311308

  11. NONLINEAR STABILITY OF A CLASS OF MAGNETOSTATIC EQUILIBRIA WITH AN APPLICATION TO SOLAR PROMINENCES

    SciTech Connect

    Aly, J.-J.

    2012-02-10

    We consider a particular class of three-dimensional magnetostatic equilibria in which the plasma is submitted to a vertical gravitational field and the gradient of the total (thermal+magnetic) pressure vanishes. We show analytically that an equilibrium in that class makes the energy an absolute minimum in the set of all the configurations accessible from it by an arbitrary finite deformation constrained by ideal MHD and imposed to vanish on a rigid conducting wall (line-tying condition). Along with energy conservation, this implies the nonlinear ideal stability of that equilibrium in the following sense. Suppose that a perturbation of energy w(0) is applied at time t = 0 and thus evolves by obeying the nonlinear MHD equations. Then some measure of the sizes of the plasma velocity and the deformation of the structure can be made to stay at any t {>=} 0 below an arbitrarily prescribed value by choosing w(0) small enough. Nonlinear stability also holds true for a configuration obtained by superposing an equilibrium of the previous type and a nonmagnetic equilibrium which is also an energy minimizer-for instance an equilibrium with uniform specific entropy, which is shown to have that property. Our result applies to a subset of a family of equilibria, computed by B. C. Low, which includes in particular the standard Kippenhahn-Schlueter model describing the magnetic support of solar corona prominences.

  12. Effects of topography on the interpretation of the deformation field of prominent volcanoes - Application to Etna

    USGS Publications Warehouse

    Cayol, V.; Cornet, F.H.

    1998-01-01

    We have investigated the effects of topography on the surface-deformation field of volcanoes. Our study provides limits to the use of classical half-space models. Considering axisymmetrical volcanoes, we show that interpreting ground-surface displacements with half-space models can lead to erroneous estimations of the shape of the deformation source. When the average slope of the flanks of a volcano exceeds 20??, tilting in the summit area is reversed to that expected for a flat surface. Thus, neglecting topography may lead to misinterpreting an inflation of the source as a deflation. Comparisons of Mogi's model with a three-dimensional model shows that ignoring topography may lead to an overestimate of the source-volume change by as much as 50% for a slope of 30??. This comparison also shows that the depths calculated by using Mogi's solution for prominent volcanoes should be considered as depths from the summit of the edifices. Finally, we illustrate these topographic effects by analyzing the deformation field measured by radar interferometry at Mount Etna during its 1991-1993 eruption. A three-dimensional modeling calculation shows that the flattening of the deflation field near the volcano's summit is probably a topographic effect.

  13. Role of the Resistive and Thermal Instabilities in Dynamics of Quiescent Prominences

    NASA Astrophysics Data System (ADS)

    Frank, Z.; Ryutova, M.; Berger, T. E.; Title, A. M.; Tarbell, T. D.

    2009-12-01

    We present the observations taken with the SOT instrument on Hinode in G-band and Ca H lines. High cadence data compiled in movies show clear evidence for several fundamental plasma instabilities. We combine the observational evidence and theoretical estimates to identify these instabilities. The following can be given as examples. (1) An analogue of the Kelvin-Helmholtz instability develops at the prominence/corona interface that manifests itself in growing ripples during a linear growth phase and may be followed by a nonlinear stage taking the form of an explosive instability corresponding to a CME ejection. This instability also includes the regime of "smoke ring" formation. (2) The appearence of "bubbles and spikes" typical to the Rayleigh-Taylor instability are observed. Their evolution and growth rates are found to be modified by both poloidal and toroidal components of magnetic field. (3) A resistive interchange instability, associated with an "unfavorable" magnetic field curvature relative to the density/temperature gradients, may be responsible for a hot barb formation, its evolution and collapse.

  14. A SOLAR TORNADO OBSERVED BY AIA/SDO: ROTATIONAL FLOW AND EVOLUTION OF MAGNETIC HELICITY IN A PROMINENCE AND CAVITY

    SciTech Connect

    Li, Xing; Morgan, Huw; Leonard, Drew; Jeska, Lauren

    2012-06-20

    During 2011 September 24, as observed by the Atmospheric Imaging Assembly instrument of the Solar Dynamic Observatory and ground-based H{alpha} telescopes, a prominence and associated cavity appeared above the southwest limb. On 2011 September 25 8:00 UT, material flows upward from the prominence core along a narrow loop-like structure, accompanied by a rise ({>=}50,000 km) of the prominence core and the loop. As the loop fades by 10:00, small blobs and streaks of varying brightness rotate around the top part of the prominence and cavity, mimicking a cyclone. The most intense and coherent rotation lasts for over three hours, with emission in both hot ({approx}1 MK) and cold (hydrogen and helium) lines. We suggest that the cyclonic appearance and overall evolution of the structure can be interpreted in terms of the expansion of helical structures into the cavity, and the movement of plasma along helical structures which appears as a rotation when viewed along the helix axis. The coordinated movement of material between prominence and cavity suggests that they are structurally linked. Complexity is great due to the combined effect of these actions and the line-of-sight integration through the structure which contains tangled fields.

  15. Detection of prominent left anterior descending coronary artery stenosis for patients with stable angina using Doppler tissue echocardiography.

    PubMed

    Veyrat, Colette; Larrazet, Fabrice; Cohen, Laurent; Laborde, François; Pellerin, Denis

    2005-08-01

    The midseptum has an elective left anterior descending coronary artery (LAD) supply. Septal peak velocity (PkV) and myocardial velocity gradient (MVG) were studied at rest with M-mode Doppler tissue echocardiography during the cardiac cycle including the septal active relaxation (SAR) outward wall motion preceding isovolumic relaxation. In all, 33 patients had significant multivessel coronary artery disease. Group A (15 patients) had prominent LAD stenosis. Group B (18 patients) had prominent circumflex (15) or right (3) coronary artery stenoses. The goal was to detect a prominent LAD stenosis. During SAR, sensitivity to detect a prominent LAD stenosis was 86% for PkV < 20 mm/s and 80% for MVG < 1.1 s(-1); specificity was 83% for both variables. During systole, sensitivity was 86% with a 55% specificity for MVG < 2.0 s(-1), whereas sensitivity was 73% and specificity 66% for PkV < 30 mm/s. Areas under receiver operating characteristic curves were over 0.90 during SAR and only 0.70 for PkV and 0.80 for MVG during systole. In multivessel coronary artery disease, SAR variables better identified a prominent LAD stenosis than systolic variables. Moreover, SAR PkVs were informative per se, whereas systole required MVG calculation. PMID:16084334

  16. Prominence material embedded in coronal mass ejections as observed with the LASCO-C2 coronagraph using polarization diagnostic

    NASA Astrophysics Data System (ADS)

    Lamy, Philippe; Boclet, Brice; Koutchmy, Serge

    2016-07-01

    Prominences are believed to be caused by the formation of a flux rope low in the magnetic structure that eventually erupts to form the CME. Indeed, many CME onset models (e.g., flux cancellation, mass loading) require the presence or formation of a prominence in order for the CME to erupt. The remnants of the cool prominence material is often seen as recognizable twisted structures inside the CME in the lines of He II at 304 Å, of D3 HeI at 587.5 nm, and of Hα at 656 nm, sometime up to a distance of several solar radii from the surface in the latter lines. The orange filter of the LASCO-C2 coronagraph includes the D3 HeI line and its presence in the core of CMEs can be unambiguously detected on polarized images as polarization allows disentangling the contributions from the hot coronal plasma (the polarized Thomson scattered light by electrons) and from the unpolarised emission of cool prominence material. This has been made possible by an in-depth calibration that removes adverse instrumental effects. We will show several examples of CME with embedded prominence material and we will attempt to estimate the mass of this material to be compared with that of the CME. We will also exploit the polarization measurements to reconstruct the 3D geometry of the observed CMEs.

  17. Measurements of H-beta, He D3, and Ca/+/ 8542-A line emission in quiescent prominences

    NASA Technical Reports Server (NTRS)

    Landman, D. A.; Edberg, S. J.; Laney, C. D.

    1977-01-01

    Measurements of H-beta, He D3, and Ca(+) 8542-A line emission in 18 quiescent prominences are presented which were performed with a 25-cm coronagraph/coude spectrograph system and an optical multichannel analyzer utilizing a Si-vidicon detector assembly mounted at the single-pass spectrograph port. The data obtained show that the line profiles deviate in the wings from those calculated on the basis of an isothermal atmosphere and a Gaussian absorption coefficient. Both a non-Gaussian microturbulence component and a temperature gradient from prominence-core to coronal values can successfully account for this phenomenon. The line widths from a given line of sight of prominence material are reduced on the basis of a common core emitting region with a temperature of 7500 to 11,600 K and a microturbulent velocity of 4.5 to 7.1 km/s for the isothermal model (these values are 5% to 10% less for the two-temperature model). It is noted that long-period low-amplitude oscillations in the D3 line width and intensity were observed when a specific line of sight in a quiescent prominence was followed. These oscillations are found to remain coherent for as many as 3 or 4 cycles and to be associated with prominence structural activation.

  18. THE ROLE OF THE INNER CORONAL NULL POINT IN THE FORMATION AND EVOLUTION OF SOLAR QUIESCENT PROMINENCES

    SciTech Connect

    Zhang, Y. Z.

    2015-02-10

    Using a 2.5-dimensional MHD simulation, we investigate the role played by the inner coronal null point in the formation and evolution of solar quiescent prominences. The flux rope is characterized by its magnetic fluxes, the toroidal magnetic flux Φ {sub p} and the poloidal flux Φ{sub ψ}. It is found that for a given Φ {sub p}, the catastrophe does not occur in the flux rope system until Φ{sub ψ} increases to a critical point. Moreover, the magnetic flux of the null point is the maximum value of the magnetic flux in the quadrupole background magnetic field, and represented by ψ {sub N}. The results show that the bigger ψ {sub N} usually corresponds to the smaller catastrophic point, the lower magnetic energy of the flux rope system, and the lesser magnetic energy inside the flux rope. Our results confirm that catastrophic disruption of the prominence occurs more easily when there is a bigger ψ {sub N}. However, ψ {sub N} has little influence on the maximum speed of the coronal mass ejections (CMEs) with an erupted prominence. Thus we argue that a topological configuration with the inner coronal null point is a necessary structure for the formation and evolution of solar quiescent prominences. In conclusion, it is easier for the prominences to form and to erupt as a core part of the CMEs in the magnetic structure with a greater ψ {sub N}.

  19. Investigation of the prominent barriers to lean manufacturing implementation in Malaysian food and beverages industry using Rasch Model

    NASA Astrophysics Data System (ADS)

    Khusaini, N. S.; Ismail, A.; Rashid, A. A.

    2016-02-01

    This paper presents a preliminary study on the prominent barriers to lean manufacturing implementation in Malaysian Food and Beverages Industry. A survey was carried out to determine the most prominent barriers of lean manufacturing implementation that are currently being faced in this industry. The amount of barriers identified for this study is twenty seven. Out of 1309 available organizations, a total of 300 organizations have been randomly selected as respondents, and 53 organizations responded. From the variable map, the analysis shows that, the negative perception towards lean manufacturing top the list as the most agreeable barrier, while the technical barriers came after it. It can also be seen from the variable map that averagely, lack of vision and direction is the barrier that is being faced. Finally, this is perhaps the first attempt in investigating the prominent barriers to Lean Manufacturing implementation in Malaysian food and beverages industry using Rasch Model.

  20. The prominent role of serotonergic degeneration in apathy, anxiety and depression in de novo Parkinson's disease.

    PubMed

    Maillet, Audrey; Krack, Paul; Lhommée, Eugénie; Météreau, Elise; Klinger, Hélène; Favre, Emilie; Le Bars, Didier; Schmitt, Emmanuelle; Bichon, Amélie; Pelissier, Pierre; Fraix, Valérie; Castrioto, Anna; Sgambato-Faure, Véronique; Broussolle, Emmanuel; Tremblay, Léon; Thobois, Stéphane

    2016-09-01

    , putamen, ventral striatum, pallidum and thalamus, but also a specific bilateral dopaminergic disruption within the substantia nigra-ventral tegmental area complex, as well as a specific serotonergic alteration within the insula, the orbitofrontal and the subgenual anterior cingulate cortices. When comparing the two parkinsonian groups, the apathetic patients mainly displayed greater serotonergic alteration in the ventral striatum, the dorsal and the subgenual parts of the anterior cingulate cortices, bilaterally, as well as in the right-sided caudate nucleus and the right-sided orbitofrontal cortex. Regression analyses also revealed that the severity of apathy was moreover mainly related to specific serotonergic lesions within the right-sided anterior caudate nucleus and the orbitofrontal cortex, while the degree of both depression and anxiety was primarily linked to serotonergic disruption within the bilateral subgenual parts and/or the right dorsal part of the anterior cingulate cortex, without prominent role of the dopaminergic degeneration in the pathogenesis of these three non-motor signs. Altogether, these findings highlight a prominent role of the serotonergic degeneration in the expression of the neuropsychiatric symptoms occurring at the onset of Parkinson's disease. PMID:27538418

  1. Temperature and EUV Intensity in a Coronal Prominence Cavity and Streamer

    NASA Technical Reports Server (NTRS)

    Kucera, T. A.; Gibson, S.E.; Schmit, D. J.; Landi, E.; Tripathi, D.

    2012-01-01

    We analyze the temperature and EUV line emission of a coronal cavity and surrounding streamer in terms of a morphological forward model. We use a series of iron line ratios observed with the Hinode Extreme-ultraviolet Imaging Spectrograph (EIS) on 2007 Aug. 9 to constrain temperature as a function of altitude in a morphological forward model of the streamer and cavity. We also compare model prediction of the EIS EUV line intensities and polarized brightness (pB) data from the Mauna Loa Solar Observatory (MLSO) MK4. This work builds on earlier analysis using the same model to determine geometry of and density in the same cavity and streamer. The fit to the data with altitude dependent temperature profiles indicates that both the streamer and cavity have temperatures in the range 1.4-1.7 MK. However, the cavity exhibits substantial substructure such that the altitude dependent temperature profile is not sufficient to completely model conditions in the cavity. Coronal prominence cavities are structured by magnetism so clues to this structure are to be found in their plasma properties. These temperature substructures are likely related to structures in the cavity magnetic field. Furthermore, we find that the model overestimates the line intensities by a factor of 4-10, while overestimating pB data by no more than a factor of 1.4. One possible explanation for this is that there may be a significant amount of material at temperatures outside of the range log T(K) approximately equals 5.8 - 6.7 in both the cavity and the streamer.

  2. Prominent pancreatic endocrinopathy and altered control of food intake disrupt energy homeostasis in prion diseases

    USGS Publications Warehouse

    Bailey, J.D.; Berardinelli, J.G.; Rocke, T.E.; Bessen, R.A.

    2008-01-01

    Prion diseases are fatal neurodegenerative diseases that can induce endocrinopathies. The basis of altered endocrine function in prion diseases is not well understood, and the purpose of this study was to investigate the spatiotemporal relationship between energy homeostasis and prion infection in hamsters inoculated with either the 139H strain of scrapie agent, which induces preclinical weight gain, or the HY strain of transmissible mink encephalopathy (TME), which induces clinical weight loss. Temporal changes in body weight, feed, and water intake were measured as well as both non-fasted and fasted concentrations of serum glucose, insulin, glucagon, ??-ketones, and leptin. In 139H scrapie-infected hamsters, polydipsia, hyperphagia, non-fasted hyperinsulinemia with hyperglycemia, and fasted hyperleptinemia were found at preclinical stages and are consistent with an anabolic syndrome that has similarities to type II diabetes mellitus and/or metabolic syndrome X. In HY TME-infected hamsters, hypodipsia, hypersecretion of glucagon (in both non-fasted and fasted states), increased fasted ??-ketones, fasted hypoglycemia, and suppressed non-fasted leptin concentrations were found while feed intake was normal. These findings suggest a severe catabolic syndrome in HY TME infection mediated by chronic increases in glucagon secretion. In both models, alterations of pancreatic endocrine function were not associated with PrPSc deposition in the pancreas. The results indicate that prominent endocrinopathy underlies alterations in body weight, pancreatic endocrine function, and intake of food. The prion-induced alterations of energy homeostasis in 139H scrapie- or HY TME-infected hamsters could occur within areas of the hypothalamus that control food satiety and/or within autonomic centers that provide neural outflow to the pancreas. ?? 2008 Society for Endocrinology.

  3. Thymomas with prominent glandular differentiation: a clinicopathologic and immunohistochemical study of 12 cases.

    PubMed

    Weissferdt, Annikka; Moran, Cesar A

    2013-08-01

    Twelve cases of thymomas with prominent glandular differentiation are presented. The patients were 7 men and 5 women aged between 45 and 68 years (average, 56.5 years). Clinically, the patients presented with nonspecific symptoms of chest pain, cough, and fatigue. None of the patients had a history of myasthenia gravis or other autoimmune syndrome. Thymectomy was performed in all patients. The tumor size ranged from 4 to 7 cm in greatest diameter. Macroscopically, the tumors were described as firm and light tan without areas of necrosis, hemorrhage, or cystic change. Histologically, 7 tumors were classified as spindle cell (World Health Organization type A), 2 as mixed spindle cell and conventional (A+B1), 2 as conventional (B1), and 1 as atypical thymoma (B3). In 4 cases, the tumors showed invasion into periadipose thymic tissue. All cases showed the typical growth patterns of their particular subtypes. In addition, a distinct glandular component was present in all cases showing mucinous differentiation in 4 of them. Immunohistochemical studies showed tumor cells positive for CAM5.2, cytokeratin 5/6, and Pax8 and negative for carcinoembryonic antigen, thyroid transcription factor 1, and epithelial membrane antigen. Calretinin showed focal weak staining in the nonmucinous glandular components in 3 cases. Follow-up information obtained in 8 patients showed that all were alive and well in a period ranging from 2 to 5 years. The possibility of a glandular component in thymomas should be kept in mind in the assessment of mediastinoscopic biopsies to avoid misdiagnosis for other neoplasms that may require different treatment modalities. PMID:23528863

  4. When and how does a Prominence-like Jet Gain Kinetic Energy?

    NASA Astrophysics Data System (ADS)

    Liu, Jiajia; Wang, Yuming; Liu, Rui; Zhang, Quanhao; Liu, Kai; Shen, Chenglong; Wang, S.

    2014-02-01

    A jet is a considerable amount of plasma being ejected from the chromosphere or lower corona into the higher corona and is a common phenomenon. Usually, a jet is triggered by a brightening or a flare, which provides the first driving force to push plasma upward. In this process, magnetic reconnection is thought to be the mechanism to convert magnetic energy into thermal, nonthermal, and kinetic energies. However, most jets could reach an unusual high altitude and end much later than the end of its associated flare. This fact implies that there is another way to continuously transfer magnetic energy into kinetic energy even after the reconnection. The picture described above is well known in the community, but how and how much magnetic energy is released through a way other than reconnection is still unclear. By studying a prominence-like jet observed by SDO/AIA and STEREO-A/EUVI, we find that the continuous relaxation of the post-reconnection magnetic field structure is an important process for a jet to climb up higher than it could through only reconnection. The kinetic energy of the jet gained through the relaxation is 1.6 times that gained from the reconnection. The resultant energy flux is hundreds of times larger than the flux required for the local coronal heating, suggesting that such jets are a possible source to keep the corona hot. Furthermore, rotational motions appear all the time during the jet. Our analysis suggests that torsional Alfvén waves induced during reconnection could not be the only mechanism to release magnetic energy and drive jets.

  5. When and How Does a Prominence-like Jet Gain Kinetic Energy?

    NASA Astrophysics Data System (ADS)

    Liu, J.; Wang, Y.; Liu, R.; Zhang, Q.; Liu, K.; Shen, C.; Wang, S.

    2014-12-01

    A jet is a considerable amount of plasma being ejected from the chromosphere or lower corona into the higher corona and is a common phenomenon. Usually, a jet is triggered by a brightening or a flare, which provides the first driving force to push plasma upward. In this process, magnetic reconnection is thought to be the mechanism to convert magnetic energy into thermal, nonthermal, and kinetic energies. However, most jets could reach an unusual high altitude and end much later than the end of its associated flare. This fact implies that there is another way to continuously transfer magnetic energy into kinetic energy even after the reconnection. The picture described above is well known in the community, but how and how much magnetic energy is released through a way other than reconnection is still unclear. By studying a prominence-like jet observed by SDO/AIA and STEREO-A/EUVI, we find that the continuous relaxation of the post-reconnection magnetic field structure is an important process for a jet to climb up higher than it could through only reconnection. The kinetic energy of the jet gained through the relaxation is 1.6 times that gained from the reconnection. The resultant energy flux is hundreds of times larger than the flux required for the local coronal heating, suggesting that such jets are a possible source to keep the corona hot. Furthermore, rotational motions appear all the time during the jet. Our analysis suggests that torsional Alfvén waves induced during reconnection could not be the only mechanism to release magnetic energy and drive jets.

  6. On the line intensity ratios of prominent Si II, Si III, and Si IV multiplets

    NASA Astrophysics Data System (ADS)

    Djeniže, S.; Srećković, A.; Bukvić, S.

    2010-01-01

    Line intensities of singly, doubly and triply ionized silicon (Si II, Si III, and Si IV, respectively) belonging to the prominent higher multiplets, are of interest in laboratory and astrophysical plasma diagnostics. We measured these line intensities in the emission spectra of pulsed helium discharge. The Si II line intensity ratios in the 3 s3 p22D-3 s24 p2Po, 3 s23 d2D-3 s24 f2Fo, and 3 s24 p2Po-3 s24 d2D transitions, the Si III line intensity ratios in the 3 s3 d3D-3 s4 p3Po, 3 s4 p3Po-3 s4 d3D, 3 s4 p3Po-3 s5 s3S, 3 s4 s3S-3 s4 p3Po, and 3 s4 f3Fo-3 s5 g3G transitions, and the Si IV line intensity ratios in the 4 p2Po-4 d2D and 4 p2Po-5 s2S transitions were obtained in a helium plasma at an electron temperature of about 17,000 ± 2000 K. Line shapes were recorded using a spectrograph and an ICCD camera as a highly-sensitive detection system. The silicon atoms were evaporated from a Pyrex discharge tube designed for the purpose. They represent impurities in the optically thin helium plasma at the silicon ionic wavelengths investigated. The line intensity ratios obtained were compared with those available in the literature, and with values calculated on the basis of available transition probabilities. The experimental data corresponded well with line intensity ratios calculated using the transition probabilities obtained from a Multi Configuration Hartree-Fock approximation for Si III and Si IV spectra. We recommend corrections of some Si II transition probabilities.

  7. Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog

    NASA Astrophysics Data System (ADS)

    McCauley, P. I.; Su, Y. N.; Schanche, N.; Evans, K. E.; Su, C.; McKillop, S.; Reeves, K. K.

    2015-06-01

    We present a statistical study of prominence and filament eruptions observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Several properties are recorded for 904 events that were culled from the Heliophysics Event Knowledgebase (HEK) and incorporated into an online catalog for general use. These characteristics include the filament and eruption type, eruption symmetry and direction, apparent twisting and writhing motions, and the presence of vertical threads and coronal cavities. Associated flares and white-light coronal mass ejections (CME) are also recorded. Total rates are given for each property along with how they differ among filament types. We also examine the kinematics of 106 limb events to characterize the distinct slow- and fast-rise phases often exhibited by filament eruptions. The average fast-rise onset height, slow-rise duration, slow-rise velocity, maximum field-of-view (FOV) velocity, and maximum FOV acceleration are 83 Mm, 4.4 hours, 2.1 km s-1, 106 km s-1, and 111 m s-2, respectively. All parameters exhibit lognormal probability distributions similar to that of CME speeds. A positive correlation between latitude and fast-rise onset height is found, which we attribute to a corresponding negative correlation in the average vertical magnetic field gradient, or decay index, estimated from potential field source surface (PFSS) extrapolations. We also find the decay index at the fast-rise onset point to be 1.1 on average, consistent with the critical instability threshold theorized for straight current channels. Finally, we explore relationships between the derived kinematics properties and apparent twisting motions. We find that events with evident twist have significantly faster CME speeds and significantly lower fast-rise onset heights, suggesting relationships between these values and flux rope helicity.

  8. When and how does a prominence-like jet gain kinetic energy?

    SciTech Connect

    Liu, Jiajia; Liu, Rui; Zhang, Quanhao; Liu, Kai; Shen, Chenglong; Wang, S.; Wang, Yuming

    2014-02-20

    A jet is a considerable amount of plasma being ejected from the chromosphere or lower corona into the higher corona and is a common phenomenon. Usually, a jet is triggered by a brightening or a flare, which provides the first driving force to push plasma upward. In this process, magnetic reconnection is thought to be the mechanism to convert magnetic energy into thermal, nonthermal, and kinetic energies. However, most jets could reach an unusual high altitude and end much later than the end of its associated flare. This fact implies that there is another way to continuously transfer magnetic energy into kinetic energy even after the reconnection. The picture described above is well known in the community, but how and how much magnetic energy is released through a way other than reconnection is still unclear. By studying a prominence-like jet observed by SDO/AIA and STEREO-A/EUVI, we find that the continuous relaxation of the post-reconnection magnetic field structure is an important process for a jet to climb up higher than it could through only reconnection. The kinetic energy of the jet gained through the relaxation is 1.6 times that gained from the reconnection. The resultant energy flux is hundreds of times larger than the flux required for the local coronal heating, suggesting that such jets are a possible source to keep the corona hot. Furthermore, rotational motions appear all the time during the jet. Our analysis suggests that torsional Alfvén waves induced during reconnection could not be the only mechanism to release magnetic energy and drive jets.

  9. When and How Does A Prominence-like Jet Gain Kinetic Energy?

    NASA Astrophysics Data System (ADS)

    Liu, J.; Wang, Y.; Zhang, Q.; Liu, K.; Shen, C.

    2013-12-01

    Usually a jet is triggered by a brightening or flare, which provides the first driving force. In this process, magnetic reconnection is thought to be the mechanism to convert magnetic energy into jet's kinetic energy. However, most jets could reach an unusual height and end far after the end of its associated flare. This fact implies another way continuously transferring magnetic energy into kinetic energy after the reconnection. This picture is well known, but how and how much magnetic energy is released through the way other than the reconnection is still unclear. Here, through studying a prominence-like jet observed by AIA and EUVI, we reveal the continuously relaxation of post-reconnection magnetic field structure is an important process to support a jet. The kinetic energy of the jet gained through this way is 1.6 times of that from the reconnection. The resultant energy flux is hundreds of the required for local coronal heating, suggesting such jets are a possible source to keep corona hot. Rotational motion appearing all the time during the jet implies the torsional Alfven wave induced during reconnection is not the only mechanism to release magnetic energy and drive jets. Left column: Difference images taken by SDO/AIA at 304A passband. The FOV of the images is 430"x430". Right column: Difference images from STEREO-A/EUVI at the same passband. The FOV is 450"x450". Since STEREO-A was 120 degree apart away from SDO on 2012 July 8, the SDO limb event right happened ondisk in the view of STEREO-A. Black and red solid curve: integrated intensity over the cross-section of the jet at different height at 19:11 UT and 19:47 UT, respectively. The two horizontal dashed lines are their average values. Black and red dashed curve with asterisks: axial speed with errors of the eight sub-jets shown in Figure 3 at 19:11 UT and 19:47 UT , respectively. Blue dashed curve with diamonds: angular speed with errors of the jet at different height.

  10. What is the most prominent factor limiting photosynthesis in different layers of a greenhouse cucumber canopy?

    PubMed Central

    Chen, Tsu-Wei; Henke, Michael; de Visser, Pieter H. B.; Buck-Sorlin, Gerhard; Wiechers, Dirk; Kahlen, Katrin; Stützel, Hartmut

    2014-01-01

    Background and Aims Maximizing photosynthesis at the canopy level is important for enhancing crop yield, and this requires insights into the limiting factors of photosynthesis. Using greenhouse cucumber (Cucumis sativus) as an example, this study provides a novel approach to quantify different components of photosynthetic limitations at the leaf level and to upscale these limitations to different canopy layers and the whole plant. Methods A static virtual three-dimensional canopy structure was constructed using digitized plant data in GroIMP. Light interception of the leaves was simulated by a ray-tracer and used to compute leaf photosynthesis. Different components of photosynthetic limitations, namely stomatal (SL), mesophyll (ML), biochemical (BL) and light (LL) limitations, were calculated by a quantitative limitation analysis of photosynthesis under different light regimes. Key Results In the virtual cucumber canopy, BL and LL were the most prominent factors limiting whole-plant photosynthesis. Diffusional limitations (SL + ML) contributed <15 % to total limitation. Photosynthesis in the lower canopy was more limited by the biochemical capacity, and the upper canopy was more sensitive to light than other canopy parts. Although leaves in the upper canopy received more light, their photosynthesis was more light restricted than in the leaves of the lower canopy, especially when the light condition above the canopy was poor. An increase in whole-plant photosynthesis under diffuse light did not result from an improvement of light use efficiency but from an increase in light interception. Diffuse light increased the photosynthesis of leaves that were directly shaded by other leaves in the canopy by up to 55 %. Conclusions Based on the results, maintaining biochemical capacity of the middle–lower canopy and increasing the leaf area of the upper canopy would be promising strategies to improve canopy photosynthesis in a high-wire cucumber cropping system. Further

  11. Prominent J-wave and T-wave alternans associated with mechanical alternans in a patient with takotsubo cardiomyopathy

    PubMed Central

    Hojo, Rintaro; Fukamizu, Seiji; Kitamura, Takeshi; Komiyama, Kota; Tanabe, Yasuhiro; Tejima, Tamotsu; Nishizaki, Mitsuhiro; Sakurada, Harumizu; Hiraoka, Masayasu

    2014-01-01

    A 74-year-old woman with takotsubo cardiomyopathy developed polymorphic ventricular tachycardia during the acute phase. She exhibited prominent J-wave and T-wave alternans preceding ventricular tachycardia. These abnormalities disappeared after recovery from myocardial stunning. PMID:26336523

  12. Prominent J-wave and T-wave alternans associated with mechanical alternans in a patient with takotsubo cardiomyopathy.

    PubMed

    Hojo, Rintaro; Fukamizu, Seiji; Kitamura, Takeshi; Komiyama, Kota; Tanabe, Yasuhiro; Tejima, Tamotsu; Nishizaki, Mitsuhiro; Sakurada, Harumizu; Hiraoka, Masayasu

    2015-02-01

    A 74-year-old woman with takotsubo cardiomyopathy developed polymorphic ventricular tachycardia during the acute phase. She exhibited prominent J-wave and T-wave alternans preceding ventricular tachycardia. These abnormalities disappeared after recovery from myocardial stunning. PMID:26336523

  13. Social Preference, Social Prominence, and Group Membership in Late Elementary School: Homophilic Concentration and Peer Affiliation Configurations

    ERIC Educational Resources Information Center

    Farmer, Thomas W.; Irvin, Matthew J.; Leung, Man-Chi; Hall, Cristin M.; Hutchins, Bryan C.; McDonough, Erin

    2010-01-01

    This study investigated the social preference and social prominence of 622 5th graders (290 boys, 332 girls) in relation to peer group membership. The sample was recruited from 11 elementary schools in a southeastern state. The ethnicity of participants was 55% European American, 41% African American, and 4% other. Peer groups were classified on…

  14. 78 FR 69691 - Draft Guidance for Industry on Product Name Placement, Size, and Prominence in Advertising and...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-11-20

    ... Federal Register of January 25, 2012 (77 FR 3779), FDA announced the availability of a guidance entitled..., and Prominence in Advertising and Promotional Labeling; Availability AGENCY: Food and Drug... Advertising and Promotional Labeling.'' When finalized, the draft guidance will replace the guidance of...

  15. On the Relationship Between a Hot-channel-like Solar Magnetic Flux Rope and its Embedded Prominence

    NASA Astrophysics Data System (ADS)

    Cheng, X.; Ding, M. D.; Zhang, J.; Srivastava, A. K.; Guo, Y.; Chen, P. F.; Sun, J. Q.

    2014-07-01

    A magnetic flux rope (MFR) is a coherent and helical magnetic field structure that has recently been found likely to appear as an elongated hot channel prior to a solar eruption. In this Letter, we investigate the relationship between the hot channel and the associated prominence through analysis of a limb event on 2011 September 12. In the early rise phase, the hot channel was initially cospatial with the prominence. It then quickly expanded, resulting in a separation of the top of the hot channel from that of the prominence. Meanwhile, they both experienced an instantaneous morphology transformation from a Λ shape to a reversed-Y shape and the top of these two structures showed an exponential increase in height. These features are a good indication of the occurrence of kink instability. Moreover, the onset of kink instability is found to coincide in time with the impulsive enhancement of flare emission underneath the hot channel, suggesting that ideal kink instability likely also plays an important role in triggering fast flare reconnection besides initiating the impulsive acceleration of the hot channel and distorting its morphology. We conclude that the hot channel is most likely the MFR system and the prominence only corresponds to the cool materials that are collected in the bottom of the helical field lines of the MFR against gravity.

  16. ON THE RELATIONSHIP BETWEEN A HOT-CHANNEL-LIKE SOLAR MAGNETIC FLUX ROPE AND ITS EMBEDDED PROMINENCE

    SciTech Connect

    Cheng, X.; Ding, M. D.; Zhang, J.; Guo, Y.; Chen, P. F.; Sun, J. Q.; Srivastava, A. K.

    2014-07-10

    A magnetic flux rope (MFR) is a coherent and helical magnetic field structure that has recently been found likely to appear as an elongated hot channel prior to a solar eruption. In this Letter, we investigate the relationship between the hot channel and the associated prominence through analysis of a limb event on 2011 September 12. In the early rise phase, the hot channel was initially cospatial with the prominence. It then quickly expanded, resulting in a separation of the top of the hot channel from that of the prominence. Meanwhile, they both experienced an instantaneous morphology transformation from a Λ shape to a reversed-Y shape and the top of these two structures showed an exponential increase in height. These features are a good indication of the occurrence of kink instability. Moreover, the onset of kink instability is found to coincide in time with the impulsive enhancement of flare emission underneath the hot channel, suggesting that ideal kink instability likely also plays an important role in triggering fast flare reconnection besides initiating the impulsive acceleration of the hot channel and distorting its morphology. We conclude that the hot channel is most likely the MFR system and the prominence only corresponds to the cool materials that are collected in the bottom of the helical field lines of the MFR against gravity.

  17. Social Cognition of Rejected Status Students in Late Elementary School: An Examination of Low, Medium, and High Social Prominence Subtypes

    ERIC Educational Resources Information Center

    Hall, Cristin M.

    2011-01-01

    The present study examined the social network perceptions of fifth grade rejected students (N = 723). Rejected students were separated into low-, medium-, and high-social prominence subtypes. Cluster analysis was also used to create analytically-derived subtypes of rejected students including the following characteristics: social network…

  18. Open questions on prominences from coordinated observations by IRIS, Hinode, SDO/AIA, THEMIS, and the Meudon/MSDP

    NASA Astrophysics Data System (ADS)

    Schmieder, B.; Tian, H.; Kucera, T.; López Ariste, A.; Mein, N.; Mein, P.; Dalmasse, K.; Golub, L.

    2014-09-01

    Context. A large prominence was observed by multiple instruments on the ground and in space during an international campaign on September 24, 2013, for three hours (12:12 UT -15:12 UT). Instruments used in the campaign included the newly launched (June 2013) Interface Region Imaging Spectrograph (IRIS), THEMIS (Tenerife), the Hinode Solar Optical Telescope (SOT), the Solar Dynamic Observatory's Atmospheric Imaging Assembly (SDO/AIA), and the Multichannel Subtractive Double Pass spectrograph (MSDP) in the Meudon Solar Tower. The movies obtained in 304 Å with the EUV imager SDO/AIA, and in Ca II line by SOT show the dynamic nature of the prominence. Aims: The aim of this work is to study the dynamics of the prominence fine structures in multiple wavelengths to understand their formation. Methods: The spectrographs IRIS and MSDP provided line profiles with a high cadence in Mg II h (2803.5 Å) and k (2796.4 Å) lines along four slit positions (IRIS), and in Hα in a 2D field of view (MSDP). The spectropolarimetry of THEMIS (Tenerife) allowed us to derive the magnetic field of the prominence using the He D3 line depolarization (Hanle effect combined with the Zeeman effect). Results: The magnetic field is found to be globally horizontal with a relatively weak field strength (8-15 Gauss). On the other hand, the Ca II movie reveals turbulent-like motion that is not organized in specific parts of the prominence. We tested the addition of a turbulent magnetic component. This model is compatible with the polarimetric observations at those places where the plasma turbulence peaks. On the other hand, the Mg II line profiles show multiple peaks well separated in wavelength. This is interpreted by the existence of small threads along the line of sight with a large dispersion of discrete values of Doppler shifts, from 5 km s-1 (a quasi-steady component) to 60-80 km s-1. Each peak corresponds to a Gaussian profile, and not to a reversed profile as was expected by the present non

  19. An assessment of prominent lines in inductively-coupled argon plasmas with special reference to spectrographic general survey analysis

    NASA Astrophysics Data System (ADS)

    Boumans, P. W. J. M.

    About 600 prominent lines for inductively-coupled plasma-atomic emission spectrometry (ICP-AES) using an argon ICP were studied with the triple objective of (1) compiling a library of prominent lines for spectrographic general survey analysis in this laboratory, (2) comparing the detection limits and sensitivities of the lines with literature data, in particular those in the author's Line Coincidence Tables for ICP-AES [Pergamon Press, Oxford (1980)], and (3) providing a list of lines with "universal" sensitivities that can be generally used for semiquantitative analysis. A 50 MHz ICP operated under compromise conditions and spectrographic detection were used. The latter limited the wavelength region of the prominent lines covered to a range between 235 and 446 nm. For 598 lines listed in the Line Coincidence Tables (LCT) the paper presents the visually estimated detection limits and an assessment of band interferences in regions of ±0.05nm about the prominent lines. Similar data are presented for 88 computer predicted, supplementary prominent lines [Spectrochim. Acta 36B, 169 (1981)] for which the predictions came true. For the 383 prominent lines located between 252 and 446 nm densitometrically determined detection limits and sensitivities are given. The sensitivities were converted to a "universal scale", independent of the spectral characteristics of the optics and the detector. The results of the visual and densitometric determinations are compared mutually and with the data given in the LCT, which are primarily based on the experimental work of Winge et al. [Appt. Specirosc. 33, 206 (1979)]; consequently the present paper also assesses the extent to which data for prominent lines can be transferred from the one ICP to the other, if both are operated under compromise conditions. The conversion of sensitivities on the "universal scale" to a scale applicable to a particular apparatus using the corresponding spectral distributions of the background intensity is

  20. FIRST SDO/AIA OBSERVATION OF SOLAR PROMINENCE FORMATION FOLLOWING AN ERUPTION: MAGNETIC DIPS AND SUSTAINED CONDENSATION AND DRAINAGE

    SciTech Connect

    Liu Wei; Berger, Thomas E.; Low, B. C.

    2012-02-15

    Imaging solar coronal condensation forming prominences was difficult in the past, a situation recently changed by Hinode and the Solar Dynamics Observatory (SDO). We present the first example observed with the SDO/Atmospheric Imaging Assembly, in which material gradually cools through multiple EUV channels in a transequatorial loop system that confines an earlier eruption. Nine hours later, this leads to eventual condensation at the dips of these loops, forming a moderate-size prominence of {approx}10{sup 14} g, to be compared to the characteristic 10{sup 15} g mass of a coronal mass ejection (CME). The prominence mass is not static but maintained by condensation at a high estimated rate of 10{sup 10} g s{sup -1} against a comparable, sustained drainage through numerous vertical downflow threads, such that 96% of the total condensation ({approx}10{sup 15} g) is drained in approximately one day. The mass condensation and drainage rates temporally correlate with the total prominence mass. The downflow velocity has a narrow Gaussian distribution with a mean of 30 km s{sup -1}, while the downward acceleration distribution has an exponential drop with a mean of {approx}1/6 g{sub Sun }, indicating a significant canceling of gravity, possibly by the Lorentz force. Our observations show that a macroscopically quiescent prominence is microscopically dynamic, involving the passage of a significant mass through it, maintained by a continual mass supply against a comparable mass drainage, which bears important implications for CME initiation mechanisms in which mass unloading is important.

  1. Dynamics of a Solar Prominence Tornado Observed by SDO/AIA on November 7-8, 2012

    NASA Astrophysics Data System (ADS)

    Mghebrishvili, Irakli; Zaqarashvili, Teimuraz V.; Kukhianidze, Vasil; Ramishvili, Giorgi; Shergelashvili, Bidzina; Veronig, Astrid; Poedts, Stefaan

    2015-09-01

    We study the detailed dynamics of a solar prominence tornado using time series of 171, 304, 193, and 211 Å spectral lines obtained by the Solar Dynamics Observatory/Atmospheric Imaging Assembly during 2012 November 7-8. The tornado first appeared at 08:00 UT, November 07, near the surface, gradually rose upwards with the mean speed of ˜1.5 km s-1 and persisted over 30 hr. Time-distance plots show two patterns of quasi-periodic transverse displacements of the tornado axis with periods of 40 and 50 minutes at different phases of the tornado evolution. The first pattern occurred during the rising phase and can be explained by the upward motion of the twisted tornado. The second pattern occurred during the later stage of evolution when the tornado already stopped rising and could be caused either by MHD kink waves in the tornado or by the rotation of two tornado threads around a common axis. The later hypothesis is supported by the fact that the tornado sometimes showed a double structure during the quasi-periodic phase. 211 and 193 Å spectral lines show a coronal cavity above the prominence/tornado, which started expansion at ˜13:00 UT and continuously rose above the solar limb. The tornado finally became unstable and erupted together with the corresponding prominence as coronal mass ejection (CME) at 15:00 UT, November 08. The final stage of the evolution of the cavity and the tornado-related prominence resembles the magnetic breakout model. On the other hand, the kink instability may destabilize the twisted tornado, and consequently prominence tornadoes can be used as precursors for CMEs.

  2. Late-onset Lafora disease with prominent parkinsonism due to a rare mutation in EPM2A.

    PubMed

    Lynch, David S; Wood, Nicholas W; Houlden, Henry

    2016-10-01

    Lafora disease (LD) is an autosomal recessive form of progressive myoclonic epilepsy that is caused by mutations in EPM2A, encoding laforin, and NHLRC1 (EPM2B), encoding malin.(1) LD is classically described with onset in early teenage years. Patients develop myoclonus, epilepsy, visual hallucinations, and psychosis. Dementia is a prominent feature and often occurs in the late teenage years. LD typically progresses quickly, and patients become bedridden and dependent within 10 years of symptom onset, with life expectancy in the early 20s.(2,3) Only a small number of late-onset cases of LD have been described. Even then, these so-called late-onset cases have typically presented in the 20s, with dementia occurring in the early 30s. We describe a patient with extremely late onset and extended survival with prominent parkinsonism due to a novel EPM2A variant. PMID:27574708

  3. Responses to antipsychotic therapy among patients with schizophrenia or schizoaffective disorder and either predominant or prominent negative symptoms.

    PubMed

    Stauffer, Virginia L; Song, Guochen; Kinon, Bruce J; Ascher-Svanum, Haya; Chen, Lei; Feldman, Peter D; Conley, Robert R

    2012-02-01

    Patients with schizophrenia who have predominant negative symptoms are often considered less responsive to treatment. This analysis of patients with schizophrenia or schizoaffective disorder compares changes in symptom severity between those with predominant versus merely prominent negative symptoms. Prominent negative symptoms were defined by a baseline score of ≥4 on at least 3, or ≥5 on at least 2, of the 7 Positive and Negative Syndrome Scale (PANSS) negative subscale items. Predominant negative symptoms were defined by the foregoing plus a PANSS positive score of <19, a Barnes Akathisia score of <2, a Simpson-Angus score of <4, and a Calgary Depressive Scale score of <9. Adult patients with schizophrenia (n=227) or schizoaffective disorder (n=116) received either olanzapine (10-20mg/day, n=169) or quetiapine (300-700mg/day, n=174) for up to 24weeks. Data for both medications were pooled. Of the 343 patients enrolled in the study, 34.7% met the criteria for predominant negative symptoms, the remaining 65.3% being characterized only by their prominent negative symptoms. Changes in the severity of negative symptoms in both patient types largely followed similar trajectories during treatment, as reflected both in Marder PANSS negative subscale scores and in the Scale for Assessment of Negative Symptoms total and domain scores. Patients with either predominant or prominent negative symptoms therefore appear to respond similarly to atypical antipsychotic treatment. This distinction, incorporating an evaluation of the presence of positive, affective, and extrapyramidal symptoms, may therefore not have prognostic implications for the responsiveness of patients' negative symptoms to treatment. PMID:22019076

  4. THE HYDROMAGNETIC INTERIOR OF A SOLAR QUIESCENT PROMINENCE. I. COUPLING BETWEEN FORCE BALANCE AND STEADY ENERGY TRANSPORT

    SciTech Connect

    Low, B. C.; Casini, R.; Berger, T.; Liu, W.

    2012-08-10

    This series of papers investigates the dynamic interiors of quiescent prominences revealed by recent Hinode and SDO/AIA high-resolution observations. This first paper is a study of the static equilibrium of the Kippenhahn-Schlueter diffuse plasma slab, suspended vertically in a bowed magnetic field, under the frozen-in condition and subject to a theoretical thermal balance among an optically thin radiation, heating, and field-aligned thermal conduction. The everywhere-analytical solutions to this nonlinear problem are an extremely restricted subset of the physically admissible states of the system. For most values of the total mass frozen into a given bowed field, force balance and steady energy transport cannot both be met without a finite fraction of the total mass having collapsed into a cold sheet of zero thickness, within which the frozen-in condition must break down. An exact, resistive hydromagnetic extension of the Kippenhahn-Schlueter slab is also presented, resolving the mass-sheet singularity into a finite-thickness layer of steadily falling dense fluid. Our hydromagnetic result suggests that the narrow, vertical prominence H{sub {alpha}} threads may be falling across magnetic fields, with optically thick cores much denser and ionized to much lower degrees than conventionally considered. This implication is discussed in relation to (1) the recent SDO/AIA observations of quiescent prominences that are massive and yet draining mass everywhere in their interiors, (2) the canonical range of 5-60 G determined from spectral polarimetric observations of prominence magnetic fields over the years, and (3) the need for a more realistic multi-fluid treatment.

  5. The Effects of B/L-Dependent Heating on the Formation and Evolution of a Multi-Threaded Prominence

    NASA Technical Reports Server (NTRS)

    Karpen, Judith T.; Luna, M.; DeVore, C. R.

    2012-01-01

    We have developed a comprehensive, multi-threaded, three-dimensional model of the plasma dynamics and energetics of a prominence and its overlying arcade (Luna et al. 2012). In this model, the basic magnetic structure is that of two interacting sheared arcades, while the cool condensations composing the prominence are formed by the well-studied thermal nonequilibrium mechanism. In a given filament-channel flux tube, the mass is evaporated from the chromosphere by heating localized near the footpoints, and condenses in the form of transient blobs or a persistent thread. Our previous studies of thermal nonequilibrium used steady or impulsive heating functions with no dependence on local physical. However, parametric active-region models with steady heating proportional to B/L, where B is the flux-tube magnetic field strength at each footpoint and L is the flux-tube length, yield the best agreement with observations (e.g., Schrijver et al. 2008). We have determined the effects of this active-region heating function on our model for the formation and evolution of prominence mass. We have also expanded the range of our computational domain to include more ofthe overlying arcade (the so-called "cavity") than in Luna et al. (2012), and have increased the number of selected flux tubes from 125 to 533. We will illustrate the time-dependent plasma behavior produced by the B/L heating function with synthetic images in several ALA passbands, and compare the resulting prominence properties with those predicted by our model with steady heating.

  6. Could prominent airway-centered fibroblast foci in lung biopsies predict underlying chronic microaspiration in idiopathic pulmonary fibrosis patients?

    PubMed

    Bois, Melanie C; Hu, Xiaowen; Ryu, Jay H; Yi, Eunhee S

    2016-07-01

    Chronic occult aspiration of small droplets (microaspiration) due to gastroesophageal reflux disease (GERD) and/or hiatal hernia is postulated to be a contributing factor in the pathogenesis of idiopathic pulmonary fibrosis (IPF). Usual interstitial pneumonia (UIP) is the histopathologic correlate of IPF. We hypothesized that chronic microaspiration may manifest as prominent airway-centered fibroblastic foci (FFs) in IPF. UIP cases diagnosed by wedge biopsies over a 6-year period (2006-2011) were identified and scored (1-3) for the prominence of airway-centered FFs by 2 authors blinded for clinical history. Relevant clinical information was obtained. Thirty-seven patients (22 men) were diagnosed with IPF by multidisciplinary approach. Thirteen cases (35.1%) demonstrated high airway-centered FF score (score 3). Twenty (54.1%) patients carried a clinical diagnosis of GERD, and 3 patients (8.1%) had hiatal hernia. High airway-centered FF score was significantly associated with hiatal hernia diagnosis (P=.037) but not with a diagnosis of GERD or the use of proton pump inhibitors/histamine-2 receptor antagonists. High airway-centered FF score was associated with airway-centered acute inflammation (P=.028) and peribronchiolar granulomas (P=.042). In summary, IPF cases with hiatal hernia were more likely to have a prominent airway-centered FF. Given the strong association between hiatal hernia and GERD and their risk for developing chronic microaspiration, the prominent airway-centered FF in UIP might predict the presence of chronic microaspiration, acknowledging that GERD and proton pump inhibitor/histamine-2 receptor antagonist use failed to demonstrate a significant association. Larger studies are warranted for further investigation. PMID:26980038

  7. [Movement disorders in David Copperfield].

    PubMed

    Garćia Ruiz, P J; Gulliksen, L L

    1999-01-01

    Charles Dickens' novels are a source of vivid neurological descriptions. Besides Pickwickian syndrome, many other neurological descriptions can be found in Dickens' novels. David Copperfield contains several characters with movement disorders including generalized dystonia (Mr. Uriah Heep), restless legs syndrome (the waiter), cervical dystonia (Mr. Sharp) and spasmodic dysphonia (Mr. Creakle). These neurological descriptions an probably based on the observation of actual patients. PMID:10570623

  8. 2D radiative-magnetohydrostatic model of a prominence observed by Hinode, SoHO/SUMER and Meudon/MSDP

    NASA Astrophysics Data System (ADS)

    Berlicki, A.; Gunar, S.; Heinzel, P.; Schmieder, B.; Schwartz, P.

    2011-06-01

    Aims: Prominences observed by Hinode show very dynamical and intriguing structures. To understand the mechanisms that are responsible for these moving structures, it is important to know the physical conditions that prevail in fine-structure threads. In the present work we analyse a quiescent prominence with fine structures, which exhibits dynamic behaviour, which was observed in the hydrogen Hα line with Hinode/SOT, Meudon/MSDP and Ondřejov/HSFA2, and simultaneously in hydrogen Lyman lines with SoHO/SUMER during a coordinated campaign. We derive the fine-structure physical parameters of this prominence and also address the questions of the role of the magnetic dips and of the interpretation of the flows. Methods: We calibrate the SoHO/SUMER and Meudon/MSDP data and obtain the line profiles of the hydrogen Lyman series (Lβ to L6), the Ciii (977.03 Å) and Svi (933.40 Å), and Hα along the slit of SoHO/SUMER that crosses the Hinode/SOT prominence. We employ a complex 2D radiation-magnetohydrostatic (RMHS) modelling technique to properly interpret the observed spectral lines and derive the physical parameters of interest. The model was constrained not only with integrated intensities of the lines, but also with the hydrogen line profiles. Results: The slit of SoHO/SUMER is crossing different prominence structures: threads and dark bubbles. Comparing the observed integrated intensities, the depressions of Hα bubbles are clearly identified in the Lyman, Ciii, and Svi lines. To fit the observations, we propose a new 2D model with the following parameters: T = 8000 K, pcen = 0.035 dyn cm-2, B = 5 Gauss, ne = 1010 cm-3, 40 threads each 1000 km wide, plasma β is 3.5 × 10-2. Conclusions: The analysis of Ciii and Svi emission in dark Hα bubbles allows us to conclude that there is no excess of a hotter plasma in these bubbles. The new 2D model allows us to diagnose the orientation of the magnetic field versus the LOS. The 40 threads are integrated along the LOS. We

  9. Is It Where You Go or Who You Know? On the Relationship Between Students, Ph.D Program Quality, Dissertation Advisor Prominence, and Early Career Publishing Success

    ERIC Educational Resources Information Center

    Hilmer, Michael J.; Hilmer, Christiana E.

    2011-01-01

    Previous research finds that both Ph.D. program quality and relative dissertation advisor prominence are positively related to early-career publishing success. We provide insight into the relative importance of those factors by estimating early-career research productivity functions that: (1) allow relative dissertation advisor prominence to vary…

  10. A model on CME/Flare initiation: Loss of Equilibrium caused by mass loss of quiescent prominences

    NASA Astrophysics Data System (ADS)

    Miley, George; Chon Nam, Sok; Kim, Mun Song; Kim, Jik Su

    2015-08-01

    Coronal Mass Ejections (CMEs) model should give an answer to enough energy storage for giant bulk plasma into interplanetary space to escape against the sun’s gravitation and its explosive eruption. Advocates of ‘Mass Loading’ model (e.g. Low, B. 1996, SP, 167, 217) suggested a simple mechanism of CME initiation, the loss of mass from a prominence anchoring magnetic flux rope, but they did not associate the mass loss with the loss of equilibrium. The catastrophic loss of equilibrium model is considered as to be a prospective CME/Flare model to explain sudden eruption of magnetic flux systems. Isenberg, P. A., et al (1993, ApJ, 417, 368)developed ideal magnetohydrodynamic theory of the magnetic flux rope to show occurrence of catastrophic loss of equilibrium according to increasing magnetic flux transported into corona.We begin with extending their study including gravity on prominence’s material to obtain equilibrium curves in case of given mass parameters, which are the strengths of the gravitational force compared with the characteristic magnetic force. Furthermore, we study quasi-static evolution of the system including massive prominence flux rope and current sheet below it to obtain equilibrium curves of prominence’s height according to decreasing mass parameter in a properly fixed magnetic environment. The curves show equilibrium loss behaviors to imply that mass loss result in equilibrium loss. Released fractions of magnetic energy are greater than corresponding zero-mass case. This eruption mechanism is expected to be able to apply to the eruptions of quiescent prominences, which is located in relatively weak magnetic environment with 105 km of scale length and 10G of photospheric magnetic field.

  11. Surface differential rotation and prominences of the Lupus post T Tauri star RX J1508.6-4423

    NASA Astrophysics Data System (ADS)

    Donati, J.-F.; Mengel, M.; Carter, B. D.; Marsden, S.; Collier Cameron, A.; Wichmann, R.

    2000-08-01

    We present in this paper a spectroscopic monitoring of the Lupus post T Tauri star RX J1508.6-4423 carried out at two closely separated epochs (1998 May 06 and 10) with the UCL Echelle Spectrograph on the 3.9-m Anglo-Australian Telescope. Applying least-squares convolution and maximum entropy image reconstruction techniques to our sets of spectra, we demonstrate that this star features on its surface a large cool polar cap with several appendages extending to lower latitudes, as well as one spot close to the equator. The images reconstructed at both epochs are in good overall agreement, except for a photospheric shear that we interpret in terms of latitudinal differential rotation. Given the spot distribution at the epoch of our observations, differential rotation could only be investigated between latitudes 15° and 60°. We find in particular that the observed differential rotation is compatible with a solar-like law (i.e., with rotation rate decreasing towards high latitudes proportionally to sin2l, where l denotes the latitude) in this particular latitude range. Assuming that such a law can be extrapolated to all latitudes, we find that the equator of RX J1508.6-4423 does one more rotational cycle than the pole every 50+/-10d, implying a photospheric shear 2 to 3 times stronger than that of the Sun. We also discover that the Hα emission profile of RX J1508.6-4423 is most of the time double-peaked and strongly modulated with the rotation period of the star. We interpret this rotationally modulated emission as being caused by a dense and complex prominence system, the circumstellar distribution of which is obtained through maximum entropy Doppler tomography. These maps show in particular that prominences form a complete and inhomogeneous ring around the star, precisely at the corotation radius. We use the total Hα and Hβ emission flux to estimate that the mass of the whole prominence system is about 1020g. From our observation that the whole cloud system

  12. Infundibulocystic Structures and Prominent Squamous Metaplasia in Sebaceoma-A Rare Feature. A Clinicopathologic Study of 10 Cases.

    PubMed

    Flux, Katharina; Kutzner, Heinz; Rütten, Arno; Plaza, Jose A; Gasparov, Slavko; Michal, Michal; Guenova, Emmanuella; Kazakov, Dmitry V

    2016-09-01

    The authors describe 10 cases of sebaceoma that manifested prominent infundibulocystic structures in all cases and, additionally, conspicuous squamous metaplasia in 6 neoplasms. All tumors occurred on the scalp or the face (2 cases lacked clinical information) and presented as a solitary lesion, measuring from 5 to 20 mm. The patients' age ranged from 22 to 89 years. The main component of all tumors was small, uniform basaloid cells (immature sebocytes) intermixed with mature sebocytes clearly arranged in nodules, classifying the lesions as a sebaceoma. In all neoplasms, the tumor cells showed organoid growth patterns of sebaceoma, including rippled, sinusoidal/labyrinthine, and carcinoid-like, occurring alone or in combination. Additionally, numerous infundibulocystic structures were readily noticed and were either distributed multifocally or unilocular within the tumors. In some cases, they were segregated from the main tumor bulk. The authors posit that these structures, which are different from both sebaceous ductal differentiation and squamous metaplasia, represent an authentic follicular differentiation. The infundibulocystic features (combined with squamous metaplasia), when prominent and in a limited biopsy specimen, may cause a confusion with trichoadenoma or even microcystic adnexal carcinoma. PMID:26760686

  13. Temperature of Solar Prominences Obtained with the Fast Imaging Solar Spectrograph on the 1.6 m New Solar Telescope at the Big Bear Solar Observatory

    NASA Astrophysics Data System (ADS)

    Park, Hyungmin; Chae, Jongchul; Song, Donguk; Maurya, Ram Ajor; Yang, Heesu; Park, Young-Deuk; Jang, Bi-Ho; Nah, Jakyoung; Cho, Kyung-Suk; Kim, Yeon-Han; Ahn, Kwangsu; Cao, Wenda; Goode, Philip R.

    2013-11-01

    We observed solar prominences with the Fast Imaging Solar Spectrograph (FISS) at the Big Bear Solar Observatory on 30 June 2010 and 15 August 2011. To determine the temperature of the prominence material, we applied a nonlinear least-squares fitting of the radiative transfer model. From the Doppler broadening of the Hα and Ca ii lines, we determined the temperature and nonthermal velocity separately. The ranges of temperature and nonthermal velocity were 4000 - 20 000 K and 4 - 11 km s-1. We also found that the temperature varied much from point to point within one prominence.

  14. Prominent Women Biologists

    ERIC Educational Resources Information Center

    Hoh, Yin Kiong; Boo, Hong Kwen

    2003-01-01

    The perception that scientists are intelligent white men who are socially inept, absent-minded nerds seems to prevail among students at all levels, from elementary school to college. While media may, by chance or choice, promote this image, it is unfortunately a realistic one. This stereotypical image of scientists as white men has, in part,…

  15. Biconditional Prominence Correlation

    ERIC Educational Resources Information Center

    Teeple, David Allan

    2009-01-01

    This dissertation presents one solution to a problem in phonological typology, which is to explain the apparent cross-linguistic absence of a pattern I call "Strong-Position Neutralization" (or SPN): neutralization of a contrast in a strong position while the same contrast is maintained in the corresponding weak position. This is predicted in a…

  16. A RISING COOL COLUMN AS A SIGNATURE OF HELICAL FLUX EMERGENCE AND FORMATION OF PROMINENCE AND CORONAL CAVITY

    SciTech Connect

    Okamoto, Takenori J.; Tsuneta, Saku; Berger, Thomas E.

    2010-08-10

    Continuous observations were performed of a quiescent prominence with the Solar Optical Telescope on board the Hinode satellite on 2006 December 23 and 24. A peculiar slowly rising column of {approx}10{sup 4} K plasma develops from the lower atmosphere during the observations. The apparent ascent speed of the column is 2 km s{sup -1}, while the fine structures of the column exhibit much faster motion of up to 20 km s{sup -1}. The column eventually becomes a faint low-lying prominence. An overlying coronal cavity associated with the appearance of the column seen in the X-ray and EUV moves upward at {approx}5 km s{sup -1}. We discuss the relationship between these episodes and suggest that they are due to the emergence of a helical flux rope that undergoes reconnection with lower coronal fields, possibly carrying material into the coronal cavity. Under the assumption of the emerging flux scenario, the lower velocity of 2 km s{sup -1} and the higher one of 20 km s{sup -1} in the column are attributed to the rising motion of the emerging flux and to the outflow driven by magnetic reconnection between the emerging flux and the pre-existing coronal field, respectively. The present paper gives a coherent explanation of the enigmatic phenomenon of the rising column with the emergence of the helical rope and its effect on the corona. We discuss the implications that the emergence of such a helical rope has on the dynamo process in the convection zone.

  17. Prominent steatosis with hypermetabolism of the cell line permissive for years of infection with hepatitis C virus.

    PubMed

    Sugiyama, Kazuo; Ebinuma, Hirotoshi; Nakamoto, Nobuhiro; Sakasegawa, Noriko; Murakami, Yuko; Chu, Po-Sung; Usui, Shingo; Ishibashi, Yuka; Wakayama, Yuko; Taniki, Nobuhito; Murata, Hiroko; Saito, Yoshimasa; Fukasawa, Masayoshi; Saito, Kyoko; Yamagishi, Yoshiyuki; Wakita, Takaji; Takaku, Hiroshi; Hibi, Toshifumi; Saito, Hidetsugu; Kanai, Takanori

    2014-01-01

    Most of experiments for HCV infection have been done using lytic infection systems, in which HCV-infected cells inevitably die. Here, to elucidate metabolic alteration in HCV-infected cells in a more stable condition, we established an HCV-persistently-infected cell line, designated as HPI cells. This cell line has displayed prominent steatosis and supported HCV infection for more than 2 years, which is the longest ever reported. It enabled us to analyze metabolism in the HCV-infected cells integrally combining metabolomics and expression arrays. It revealed that rate-limiting enzymes for biosynthesis of cholesterol and fatty acids were up-regulated with actual increase in cholesterol, desmosterol (cholesterol precursor) and pool of fatty acids. Notably, the pentose phosphate pathway was facilitated with marked up-regulation of glucose-6-phosphate dehydrogenase, a rete-limiting enzyme, with actual increase in NADPH. In its downstream, enzymes for purine synthesis were also up-regulated resulting in increase of purine. Contrary to common cancers, the TCA cycle was preferentially facilitated comparing to glycolysis pathway with a marked increase of most of amino acids. Interestingly, some genes controlled by nuclear factor (erythroid-derived 2)-like 2 (Nrf2), a master regulator of antioxidation and metabolism, were constitutively up-regulated in HPI cells. Knockdown of Nrf2 markedly reduced steatosis and HCV infection, indicating that Nrf2 and its target genes play important roles in metabolic alteration and HCV infection. In conclusion, HPI cell is a bona fide HCV-persistently-infected cell line supporting HCV infection for years. This cell line sustained prominent steatosis in a hypermetabolic status producing various metabolites. Therefore, HPI cell is a potent research tool not only for persistent HCV infection but also for liver metabolism, overcoming drawbacks of the lytic infection systems. PMID:24718268

  18. Simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament induced by a single shock wave

    SciTech Connect

    Shen, Yuandeng; Liu, Ying D.; Chen, P. F.; Ichimoto, Kiyoshi

    2014-11-10

    We present the first stereoscopic and Doppler observations of simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament launched by a single shock wave. Using Hα Doppler observations, we derive the three-dimensional oscillation velocities at different heights along the prominence axis. The results indicate that the prominence has a larger oscillation amplitude and damping time at higher altitude, but the periods at different heights are the same (i.e., 13.5 minutes). This suggests that the prominence oscillates like a linear vertical rigid body with one end anchored on the Sun. One of the filaments shows weak transverse oscillation after the passing of the shock, which is possibly due to the low altitude of the filament and the weakening (due to reflection) of the shock wave before the interaction. Large-amplitude longitudinal oscillation is observed in the other filament after the passing of the shock wave. The velocity amplitude and period are about 26.8 km s{sup –1} and 80.3 minutes, respectively. We propose that the orientation of a filament or prominence relative to the normal vector of the incoming shock should be an important factor for launching transverse or longitudinal filament oscillations. In addition, the restoring forces of the transverse prominence are most likely due to the coupling of gravity and magnetic tension of the supporting magnetic field, while that for the longitudinal filament oscillation is probably the resultant force of gravity and magnetic pressure.

  19. Ultrasound Imaging Improves Identification of Prominent Hardware in the Surgical Treatment of Distal Radius Fractures: A Cadaveric and Prospective Clinical Study.

    PubMed

    Watchmaker, Jacqueline D; Daley, Roger A; Watchmaker, Greg P; Grindel, Steven I

    2016-03-01

    Background Volarly applied locking plates are one of several current treatment options for displaced fractures of the distal radius. Presently, surgeons use intraoperative depth gauges and fluoroscopy to select and confirm proper screw length. The contour of the dorsal cortex beneath the extensor compartments along with fracture comminution may limit the accuracy of screw length selection. Question/Purpose To evaluate the accuracy of ultrasound (US) and fluoroscopy in the detection of dorsally prominent screws placed during volar plating of experimentally created distal radius fractures and extend this prospectively into the clinical setting. Patients and Methods Distal radius fractures were experimentally induced in fresh cadaveric arms. The fractures were then internally fixated with volar locking plates utilizing fluoroscopic imaging. US imaging of the dorsal surface of the radius was then performed followed by dorsal dissection and direct caliper measurements to quantitate screw tips as recessed, flush, or protruding from the dorsal cortex. A small, prospective clinical study was also conducted to validate the clinical usefulness of using US to provide additional information regarding screw tip prominence. Results Our study demonstrated that US was able to detect dorsally prominent screw tips not visible on fluoroscopy. Cadaveric dissection showed a higher statistical correlation between US imaging and actual prominence than between fluoroscopy and actual prominence. Conclusions US examination after volar plate fixation of comminuted distal radius fractures may detect dorsal screw tip prominence when screw lengths are selected to engage the dorsal cortex. Level of Evidence IV. PMID:26855834

  20. Phase transitions, prominent dielectric anomalies, and negative thermal expansion in three high thermally stable ammonium magnesium-formate frameworks.

    PubMed

    Shang, Ran; Xu, Guan-Cheng; Wang, Zhe-Ming; Gao, Song

    2014-01-20

    We present three Mg-formate frameworks, incorporating three different ammoniums: [NH4][Mg(HCOO)3] (1), [CH3CH2NH3][Mg(HCOO)3] (2) and [NH3(CH2)4NH3][Mg2(HCOO)6] (3). They display structural phase transitions accompanied by prominent dielectric anomalies and anisotropic and negative thermal expansion. The temperature-dependent structures, covering the whole temperature region in which the phase transitions occur, reveal detailed structural changes, and structure-property relationships are established. Compound 1 is a chiral Mg-formate framework with the NH4(+) cations located in the channels. Above 255 K, the NH4(+) cation vibrates quickly between two positions of shallow energy minima. Below 255 K, the cations undergo two steps of freezing of their vibrations, caused by the different inner profiles of the channels, producing non-compensated antipolarization. These lead to significant negative thermal expansion and a relaxor-like dielectric response. In perovskite 2, the orthorhombic phase below 374 K possesses ordered CH3CH2NH3(+) cations in the cubic cavities of the Mg-formate framework. Above 374 K, the structure becomes trigonal, with trigonally disordered cations, and above 426 K, another phase transition occurs and the cation changes to a two-fold disordered state. The two transitions are accompanied by prominent dielectric anomalies and negative and positive thermal expansion, contributing to the large regulation of the framework coupled the order-disorder transition of CH3CH2NH3(+). For niccolite 3, the gradually enhanced flipping movement of the middle ethylene of [NH3(CH2)4NH3](2+) in the elongated framework cavity finally leads to the phase transition with a critical temperature of 412 K, and the trigonally disordered cations and relevant framework change, providing the basis for the very strong dielectric dispersion, high dielectric constant (comparable to inorganic oxides), and large negative thermal expansion. The spontaneous polarizations