Sample records for xxiv polimery perrenatov

  1. Spectrum of sodiumlike selenium - Se XXIV

    NASA Technical Reports Server (NTRS)

    Brown, C. M.; Seely, J. F.; Feldman, U.; Richardson, M. C.; Behring, W. E.; Cohen, L.

    1986-01-01

    High-resolution spectra of Se XXIV have been obtained with a 3-m grazing-incidence spectrograph. Thin plastic foils coated with selenium were irradiated with four or eight beams of the OMEGA laser in a line-focus configuration. Spectrograms were obtained by viewing the plasma axially. Prominent in the spectra were the 3s-3p and 3p-3d transitions in the 150-240-A region and the transitions nl-(n + 1)l-prime with n = 3, 4 in the 24-80-A region. The energy levels and ionization limit derived from the measured wavelengths are also presented.

  2. On The Back Of A Grasshopper: The XXIV Corps And The Korean Occupation

    DTIC Science & Technology

    2016-05-26

    particularly by the suicidal elements of the armed forces who will take advantage of any weakness on the part of our forces.”53 The XXIV Corps could expect some...discussed earlier, write that the temptation to blame a single “man in the dock,” usually the commander, is normally misplaced. Rather the “modern

  3. Relativistic Radiative and Auger Rates for Fe XXIV

    NASA Technical Reports Server (NTRS)

    Bautista, M. A.; Mendoza, C.; Kallman, T. R.; Palmeri, P.; White, Nicholas E. (Technical Monitor)

    2002-01-01

    As part of a project to compute improved atomic data for the spectral modeling of iron K lines, we report extensive calculations and comparisons of radiative and Auger rates for transitions involving the K-vacancy states in Fe XXIV. By making use of several computational codes, a detailed study is carried out of orbital representation, configuration interaction, relativistic corrections, cancellation effects, and fine tuning. It is shown that a formal treatment of the Breit interaction is essential to render the important magnetic correlations that take part in the decay pathways of this ion. As a result, the accuracy of the present A-values is firmly ranked at better than 10% while that of the Auger rates at only 15%.

  4. XXIV International Conference on Integrable Systems and Quantum symmetries (ISQS-24)

    NASA Astrophysics Data System (ADS)

    Burdík, Čestmír; Navrátil, Ondřej; Posta, Severin

    2017-01-01

    The XXIV International Conference on Integrable Systems and Quantum Symmetries (ISQS-24), organized by the Department of Mathematics, Faculty of Nuclear Sciences and Physical Engineering, Czech Technical University Prague and the Bogoliubov Laboratory of Theoretical Physics of the Joint Institute for Nuclear Research, belongs to the successful series of conferences held at the Czech Technical University which began in 1992 and is devoted to problems of mathematical physics related to the theory of integrable systems, quantum groups and quantum symmetries. During the last 5 years, each of the conferences gathered around 110 scientists from all over the world. 43 papers of plenary lectures and contributions presented at ISQS-24 are published in the present issue of Journal of Physics: Conference Series.

  5. Ionization balance for iron XXV, XXIV and XXIII derived from solar flare X-ray spectra

    NASA Astrophysics Data System (ADS)

    Antonucci, E.; Dodero, M. A.; Gabriel, A. H.; Tanaka, K.; Dubau, J.

    1987-06-01

    An analysis has been carried out using over 300 spectra of solar flares from both the XRP instrument on SMM and the SOX instrument on Hinotori. The helium-like iron and associated dielectronic satellite spectra were used in order to derive a revised ionization balance for Fe XXIV/Fe XXV. This is found to lie between the theoretical curves based upon ECIP ionization rates, and those using Lotz formalism, with a tendency to be closer to the former. An extension of the analysis to include Fe XXIII is subject to a somewhat larger uncertainty in the interpretation. However it indicates a similar effect for this ion. Using all three ions, a revised ionization balance for iron is presented.

  6. Calculations for energies, transition rates, and lifetimes in Al-like Kr XXIV

    NASA Astrophysics Data System (ADS)

    Zhang, C. Y.; Si, R.; Liu, Y. W.; Yao, K.; Wang, K.; Guo, X. L.; Li, S.; Chen, C. Y.

    2018-05-01

    Using the second-order many-body perturbation theory (MBPT) method, a complete and accurate data set of excitation energies, lifetimes, wavelengths, and electric dipole (E1), magnetic dipole (M1), electric quadrupole (E2), and magnetic quadrupole (M2) line strengths, transition rates, and oscillator strengths for the lowest 880 levels arising from the 3l3 (0 ≤ l ≤ 2), 3l2 4l‧ (0 ≤ l ≤ 2, 0 ≤l‧ ≤ 3), 3s2 5 l (0 ≤ l ≤ 4), 3p2 5 l (0 ≤ l ≤ 1), and 3s3p5 l (0 ≤ l ≤ 4) configurations in Al-like Kr XXIV is provided. Comparisons are made with available experimental and theoretical results. Our calculated energies are expected to be accurate enough to facilitate identifications of observed lines involving the n = 4 , 5 levels. The complete data set is also useful for modeling and diagnosing fusion plasma.

  7. Atomic Data for the K-vacancy States of Fe XXIV

    NASA Technical Reports Server (NTRS)

    Bautista, M. A.; Mendoza, C.; Kallman, T. R.; Palmeri, P.

    2003-01-01

    As part of a project to compute improved atomic data for the spectral modeling of iron K lines, we report extensive calculations and comparisons of atomic data for K-vacancy states in Fe XXIV. The data sets include: (i) energy levels, line wavelengths, radiative and Auger rates; (ii) inner-shell electron impact excitation rates and (iii) fine structure inner-shell photoionization cross sections. The calculations of energy levels and radiative and Auger rates have involved a detailed study of orbital representations, core relaxation, configuration interaction, relativistic corrections, cancellation effects and semi-empirical corrections. It is shown that a formal treatment of the Breit interaction is essential to render the important magnetic correlations that take part in the decay pathways of this ion. As a result, the accuracy of the present A-values is firmly ranked at better than 10% while that of the Auger rates at only 15%. The calculations of collisional excitation and photoionization cross sections take into account the effects of radiation and spectator Auger dampings. In the former, these effects cause significant attenuation of resonances leading to a good agreement with a simpler method where resonances are excluded. In the latter, resonances converging to the K threshold display symmetric profiles of constant width that causes edge smearing.

  8. Atomic Data for the K-Vacancy States of Fe XXIV

    NASA Technical Reports Server (NTRS)

    Bautista, M. A.; Mendoza, C.; Kallman, T. R.; Palmeri, P.

    2002-01-01

    As part of a project to compute improved atomic data for the spectral modeling of iron K lines, we report extensive calculations and comparisons of atomic data for K-vacancy states in Fe XXIV. The data sets include: (i) energy levels, line wavelengths, radiative and Auger rates; (ii) inner-shell electron impact excitation rates and (iii) fine structure inner-shell photoionization cross sections. The calculations of energy levels and radiative and Auger rates have involved a detailed study of orbital representations, core relaxation, configuration interaction, relativistic corrections, cancellation effects and semi-empirical corrections. It is shown that a formal treatment of the Breit interaction is essential to render the important magnetic correlations that take part in the decay pathways of this ion. As a result, the accuracy of the present A-values is firmly ranked at better than 10% while that of the Auger rates at only 15%. The calculations of collisional excitation and photoionization cross sections take into account the effects of radiation and spectator Auger dampings. In the former, these effects cause significant attenuation of resonances leading to a good agreement with a simpler method where resonances are excluded. In the latter, resonances converging to the K threshold display symmetric profiles of constant width that causes edge smearing.

  9. Measurement of wavelengths and lamb shifts for inner-shell transitions in Fe XVIII-XXIV. [from solar flare X-ray spectra

    NASA Technical Reports Server (NTRS)

    Seely, J. F.; Feldman, U.; Safronova, U. I.

    1986-01-01

    The wavelengths of inner-shell 1s-2p transitions in the ions Fe XVIII-XXIV have been measured in solar flare spectra recorded by the Naval Research Laboratory crystal spectrometer (SOLFLEX) on the Air Force P78-1 spacecraft. The measurements are compared with previous measurements and with recently calculated wavelengths. It is found that the measured wavelengths are systematically larger than the wavelengths calculated using the Z-expansion method by up to 0.65 mA. For the more highly charged ions, these differences can be attributed to the QED contributions to the transition energies that are not included in the Z-expansion calculations.

  10. CALCULATIONS WITH SPECTROSCOPIC ACCURACY: ENERGIES AND TRANSITION RATES IN THE NITROGEN ISOELECTRONIC SEQUENCE FROM Ar XII TO Zn XXIV

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Wang, K.; Dang, W.; Si, R.

    2016-03-15

    Combined relativistic configuration interaction and many-body perturbation calculations are performed for the 359 fine-structure levels of the 2s{sup 2} 2p{sup 3}, 2 s2p{sup 4}, 2p{sup 5}, 2s{sup 2} 2p{sup 2} 3l, 2 s2p{sup 3} 3l, 2p{sup 4} 3l, and 2s{sup 2} 2p{sup 2} 4l configurations in N-like ions from Ar xii to Zn xxiv. Complete and consistent data sets of energies, wavelengths, radiative rates, oscillator strengths, and line strengths for all possible electric dipole, magnetic dipole, electric quadrupole, and magnetic quadrupole transitions among the 359 levels are given for each ion. The present work significantly increases the amount of accuratemore » data for ions in the nitrogen-like sequence, and the accuracy of the energy levels is high enough to enable the identification and interpretation of observed spectra involving the n = 3, 4 levels, for which experimental values are largely scarce. Meanwhile, the results should be of great help for modeling and diagnosing astrophysical and fusion plasmas.« less

  11. Calculation of levels, transition rates, and lifetimes for the arsenic isoelectronic sequence Sn XVIII-Ba XXIV, W XLII

    NASA Astrophysics Data System (ADS)

    Wang, K.; Chen, Z. B.; Chen, C. Y.; Yan, J.; Dang, W.; Zhao, X. H.; Yang, X.

    2017-09-01

    Multi-configuration Dirac-Fock (MCDF) calculations of energy levels, wavelengths, oscillator strengths, lifetimes, and electric dipole (E1), magnetic dipole (M1), electric quadrupole (E2), magnetic quadrupole (M2) transition rates are reported for the arsenic isoelectronic sequence Sn XVIII-Ba XXIV, W XLII. Results are presented among the 86 levels of the 4s2 4p3, 4 s 4p4, 4p5, 4s2 4p2 4 d, and 4 s 4p3 4 d configurations in each ion. The relativistic atomic structure package GRASP2K is adopted for the calculations, in which the contributions from the correlations within the n ≤ 7 complexes, Breit interaction (BI) and quantum electrodynamics (QED) effects are taking into account. The many-body perturbation theory (MBPT) method is also employed as an independent calculation for comparison purposes, taking W XLII as an example. Calculated results are compared with data from other calculations and the observed values from the Atomic Spectra Database (ASD) of the National Institute of Standards and Technology (NIST). Good agreements are obtained. i.e, the accuracy of our energy levels is assessed to be better than 0.6%. These accurate theoretical data should be useful for diagnostics of hot plasmas in fusion devices.

  12. Application of relativistic distorted-wave method to electron-impact excitation of highly charged Fe XXIV ion embedded in weakly coupled plasmas

    NASA Astrophysics Data System (ADS)

    Chen, Zhanbin

    2018-05-01

    The process of excitation of highly charged Fe XXIV ion embedded in weakly coupled plasmas by electron impact is studied, together with the subsequent radiative decay. For the target structure, the calculation is performed using the multiconfiguration Dirac-Hartree-Fock method incorporating the Debye-Hückel potential for the electron-nucleus interaction. Fine-structure levels of the 1s22p and 1s2s2p configurations and the transition properties among these levels are presented over a wide range of screening parameters. For the collision dynamics, the distorted-wave method in the relativistic frame is adopted to include the effect of plasma background, in which the interparticle interactions in the system are described by screened interactions of the Debye-Hückel type. The continuum wave function of the projectile electron is obtained by solving the modified Dirac equations. The influence of plasma strength on the cross section, the linear polarization, and the angular distribution of x-ray photon emission are investigated in detail. Comparison of the present results with experimental data and other theoretical predictions, when available, is made.

  13. Naval Ocean Research and Development Activity Journal Index for 1976 thru 1984,

    DTIC Science & Technology

    1985-03-01

    and Antibiotics. Venezuela Basin. Deep-Sea Research, v. 31, Botanica Marina, v. XXIV, p. 399-404. p. 403-414. Thompson, J. Dana (1978). Ocean Deserts...v. 29, n. 102, p. 286-295. Phytoplankton Extracellular Products. Botanica marina, v~. XXXVI, p. 375-381. Radl, C.J. and J.P. Welsh (1983). Inventory...Experiments tion and Antibiotics. Botanica Marina, v. XXIV, in the Indian River Estuary, Florida. Journal of p. 399-404. ?. Marine Research, v. 36, p, 569-593

  14. XXIV Corps Action Report

    DTIC Science & Technology

    1945-06-01

    looses, Whoa tea ligt of sutiiürinad exeogs eqaipiaeet booane as tab Mr had, eftov -tz.. sare i&estttuteä to obtain it». Eov~ rar, because of ehangeä...shelter, food and medical service wore thvs ?va^l- ^*Tft für an* reason caäualfiiea were of necessity Sid -73 - UNCLASSIFIED BSXCH XX...their duties included posting proclamations, locating civilian food and medical supplies, establishing collec- tion centers, and evacuating

  15. 15 CFR Supplement No. 8 to Part 742 - Self-Classification Report for Encryption Items

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... forensics (v) Cryptographic accelerator (vi) Data backup and recovery (vii) Database (viii) Disk/drive... (MAN) (xxii) Modem (xxiii) Network convergence or infrastructure n.e.s. (xxiv) Network forensics (xxv...

  16. 15 CFR Supplement No. 8 to Part 742 - Self-Classification Report for Encryption Items

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... forensics (v) Cryptographic accelerator (vi) Data backup and recovery (vii) Database (viii) Disk/drive... (MAN) (xxii) Modem (xxiii) Network convergence or infrastructure n.e.s. (xxiv) Network forensics (xxv...

  17. 15 CFR Supplement No. 8 to Part 742 - Self-Classification Report for Encryption Items

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... forensics (v) Cryptographic accelerator (vi) Data backup and recovery (vii) Database (viii) Disk/drive... (MAN) (xxii) Modem (xxiii) Network convergence or infrastructure n.e.s. (xxiv) Network forensics (xxv...

  18. 15 CFR Supplement No. 8 to Part 742 - Self-Classification Report for Encryption Items

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... forensics (v) Cryptographic accelerator (vi) Data backup and recovery (vii) Database (viii) Disk/drive... (MAN) (xxii) Modem (xxiii) Network convergence or infrastructure n.e.s. (xxiv) Network forensics (xxv...

  19. 47. Photocopied October 1976, from b.f.Tower, Illistrations of the Croton ...

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

    47. Photocopied October 1976, from b.f.Tower, Illistrations of the Croton Aqueduct, New York, Wiley and Putnam, 1843. ISOMETRICAL VIEW OF THE DISTRIBUTING RESERVIOR, PLATE XXIV, PAGE 119. - Old Croton Aqueduct, New York County, NY

  20. 8 CFR 241.2 - Warrant of removal.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ...: (i) Director, Detention and Removal Operations; (ii) Deputy Assistant Director, Field Operations... Directors; (xxi) Deputy Port Directors; (xxii) Assistant Port Directors; (xxiii) Director, Field Operations; (xxiv) Deputy Director, Field Operations; (xxv) Assistant Director, Field Operations; and (xxvi) Other...

  1. 78 FR 22659 - Revisions to the Export Administration Regulations: Initial Implementation of Export Control Reform

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-04-16

    ... Designed'' Definition B. Other Definitions XXIV. Part 774--The Commerce Control List A. Product Group... Changes H. Country Groups XII. Part 742--Control Policy A. National Security (NS) Review Policy B...-all controls on parts, components, accessories, and attachments specifically designed or modified for...

  2. Hurricane Havens Handbook for the North Atlantic Ocean. Change 5. Naval Stations Mobile, Pascagoula, and Ingleside as Hurricane Havens.

    DTIC Science & Technology

    1993-08-01

    XXIV-2 0 CHANGE 5 . 3.3 ENVIRONMENTAL EFFECTS 3.3.1 WIND AND TOPOGRAPHY The relatively low- lving topograDhv surrounding Mobile Bay affords little...for Corpus Christi, Texas. The report contains computer- gridded charts with storm surge heights computed for several locations and situations, including

  3. 3 CFR 13515 - Executive Order 13515 of October 14, 2009. Increasing Participation of Asian Americans and...

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... to science and technology, culture and the arts, and the professions, including business, law... members who: (i) have a history of involvement with the AAPI communities; (ii) are from the fields of...; (xxiii) the Office of Science and Technology Policy; and (xxiv) other executive branch departments...

  4. 49 CFR 229.135 - Event recorders.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ...) Locomotive position in consist (lead or trail); (xxiii) Tractive effort; (xxiv) Cruise control on/off, if so...; (xviii) Brakes apply summary train line; (xix) Brakes released summary train line; (xx) Cruise control on... determining, that a brake application or release resulted from manipulation of brake controls at the position...

  5. 49 CFR 229.135 - Event recorders.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ...) Locomotive position in consist (lead or trail); (xxiii) Tractive effort; (xxiv) Cruise control on/off, if so...; (xviii) Brakes apply summary train line; (xix) Brakes released summary train line; (xx) Cruise control on... determining, that a brake application or release resulted from manipulation of brake controls at the position...

  6. 49 CFR 229.135 - Event recorders.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ...) Locomotive position in consist (lead or trail); (xxiii) Tractive effort; (xxiv) Cruise control on/off, if so...; (xviii) Brakes apply summary train line; (xix) Brakes released summary train line; (xx) Cruise control on... determining, that a brake application or release resulted from manipulation of brake controls at the position...

  7. 49 CFR 229.135 - Event recorders.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ...) Locomotive position in consist (lead or trail); (xxiii) Tractive effort; (xxiv) Cruise control on/off, if so...; (xviii) Brakes apply summary train line; (xix) Brakes released summary train line; (xx) Cruise control on... determining, that a brake application or release resulted from manipulation of brake controls at the position...

  8. 40 CFR 52.465 - Original identification of plan section.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... Castle County Portion of the Delaware State Implementation Plan, covering changes to the air pollution... Control of Air Pollution submitted on September 22, 1981 by the Secretary, Department of Natural Resources... Table I(a) to Regulation Number XXIV of the Delaware Regulations Governing the Control of Air Pollution...

  9. 28 CFR 0.109 - Implementation of the Treaty of Friendship and General Relations Between the United States and...

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... Friendship and General Relations Between the United States and Spain. 0.109 Section 0.109 Judicial... Service § 0.109 Implementation of the Treaty of Friendship and General Relations Between the United States... States within the meaning of Article XXIV of the Treaty of Friendship and General Relations Between the...

  10. 28 CFR 0.109 - Implementation of the Treaty of Friendship and General Relations Between the United States and...

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... Friendship and General Relations Between the United States and Spain. 0.109 Section 0.109 Judicial... Service § 0.109 Implementation of the Treaty of Friendship and General Relations Between the United States... States within the meaning of Article XXIV of the Treaty of Friendship and General Relations Between the...

  11. 28 CFR 0.109 - Implementation of the Treaty of Friendship and General Relations Between the United States and...

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... Friendship and General Relations Between the United States and Spain. 0.109 Section 0.109 Judicial... Service § 0.109 Implementation of the Treaty of Friendship and General Relations Between the United States... States within the meaning of Article XXIV of the Treaty of Friendship and General Relations Between the...

  12. 28 CFR 0.109 - Implementation of the Treaty of Friendship and General Relations Between the United States and...

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... Friendship and General Relations Between the United States and Spain. 0.109 Section 0.109 Judicial... Service § 0.109 Implementation of the Treaty of Friendship and General Relations Between the United States... States within the meaning of Article XXIV of the Treaty of Friendship and General Relations Between the...

  13. 28 CFR 0.109 - Implementation of the Treaty of Friendship and General Relations Between the United States and...

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... Friendship and General Relations Between the United States and Spain. 0.109 Section 0.109 Judicial... Service § 0.109 Implementation of the Treaty of Friendship and General Relations Between the United States... States within the meaning of Article XXIV of the Treaty of Friendship and General Relations Between the...

  14. Historic Landscape Inventory for Marietta National Cemetery

    DTIC Science & Technology

    2017-11-14

    development context, a description of current conditions, and an analysis of changes over time to the cultural landscape. All landscape features were...Factors ..................................................................................................... xxiv 1 Methodology ...yards 0.9144 meters ERDC/CERL TR-17-41 1 1 Methodology 1.1 Background The U.S. Congress codified the National Historic Preservation Act of

  15. Strategic Mobility Alternatives for the 1980s. Volume 2. Analysis and Conclusions

    DTIC Science & Technology

    1977-03-01

    with renewed emphasis on the Nxi-mod; "II rl ++|llllll’’’P.7= UNCLASSIFIED -xxiv- o Continued, even accelerated, acquisition of the spares neces- sary...H. Birch, J. Houston, L. L. Moorhous, J. Pederson , and H. B. Turin. UNCLASSIID UNCLAS8WEED S~- iii- CONTENTS PREFACE iii SURM ARY

  16. 77 FR 31691 - Approval and Promulgation of Implementation Plans; State of Hawaii; Regional Haze Federal...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-05-29

    ... Subject to BART 3. BART Determination for Kanoelehua Hill a. BART for NO X and Particulate Matter (PM) b.... The initials PM mean or refer to particulate matter. xxiv. The initials PM2.5 mean or refer to particulate matter with an aerodynamic diameter of less than 2.5 micrometers (fine particulate matter). xxv...

  17. VizieR Online Data Catalog: WIYN open cluster study. LX. RV survey of NGC 6819 (Milliman+, 2014)

    NASA Astrophysics Data System (ADS)

    Milliman, K. E.; Mathieu, R. D.; Geller, A. M.; Gosnell, N. M.; Meibom, S.; Platais, I.

    2014-10-01

    The WOCS radial velocity target sample for NGC 6819 has 3895 stars that span 1° on the sky centered at RA=19h41m17.5s, DE=+40°11'47'' (J2000). The details of our radial velocity survey of NGC 6819 including the observing procedure, data reduction, and membership classification are discussed in depth in Hole et al. 2009 (cat. J/AJ/138/159; Paper XXIV) and Geller et al. 2008 (cat. J/AJ/135/2264; Paper XXXII). Observations of NGC 6819 with the Hydra Multi-Object Spectrograph (MOS) on the WIYN 3.5m telescope began in 1998 June and are still ongoing. We have almost 14000 spectra for over 2600 stars. These observations are augmented with 733 radial velocity measurements for 170 stars taken at the Harvard-Smithsonian Center for Astrophysics (CfA) facilities between 1988 May and 1995 by R. D. Mathieu and D. W Latham (Hole et al. 2009, cat. J/AJ/138/159; Paper XXIV). (4 data files).

  18. Critical Rare Earths, National Security, and U.S.-China Interactions: A Portfolio Approach to Dysprosium Policy Design

    DTIC Science & Technology

    2015-01-01

    by the graduate fellow’s faculty committee. C O R P O R A T I O N Dissertation Critical Rare Earths, National Security, and U.S.-China Interactions A...Portfolio Approach to Dysprosium Policy Design David L. An Dissertation Critical Rare Earths, National Security, and U.S.-China Interactions A...Permanent Magnet ................................................ xxiv Dysprosium, the Most Critical Rare Earth

  19. The Manufacture, Properties, and Testing of Napalm Soaps

    DTIC Science & Technology

    1943-11-17

    prrcltio’n. Tests at 1000C. a.nd 100 p.s,,i. %Inhibitor Induction Addod Pcriod, mins. N one 0 20 Eydroquinone 1 5 duPont #19 1 150 Lecithin 1 SF0 1 45...acetone tends to hydrolyze the soap, liberating more free acid which in turn is removed by the solvent. Table XXIV shows results obtained with a

  20. Multiple-Purpose Project, Osage River Basin, Osage River, Missouri. Harry S. Truman Dam & Reservoir Operation and Maintenance Manual. Appendix VII. Volume 1. Construction Foundation Report.

    DTIC Science & Technology

    1984-01-01

    RIVER MISSOURI Report from September 1966 HARRY S. TROMAN DAM & RESERVOIR November 1979 OPERATION AND MAINTENANCE MANUAL 6 PERFORMING DRG. REPORT N4040E...Two of this report ) VII- I- xxiv ............................. .... ... .... ... . .2. . . OPERATION AND MAINTENANCE MANUAL HARRY S. TRUMAN DAM AND...RESERVOIR OSAGE RIVER, MISSOURI APPENDIX VII CONSTRUCTION FOUNDATION REPORT CHAPTER 1 INTRODUCTION 1-01. Location and Description of Project: Harry S

  1. DEPARTURE OF HIGH-TEMPERATURE IRON LINES FROM THE EQUILIBRIUM STATE IN FLARING SOLAR PLASMAS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Kawate, T.; Keenan, F. P.; Jess, D. B., E-mail: t.kawate@qub.ac.uk

    2016-07-20

    The aim of this study is to clarify if the assumption of ionization equilibrium and a Maxwellian electron energy distribution is valid in flaring solar plasmas. We analyze the 2014 December 20 X1.8 flare, in which the Fe xxi 187 Å, Fe xxii 253 Å, Fe xxiii 263 Å, and Fe xxiv 255 Å emission lines were simultaneously observed by the EUV Imaging Spectrometer on board the Hinode satellite. Intensity ratios among these high-temperature Fe lines are compared and departures from isothermal conditions and ionization equilibrium examined. Temperatures derived from intensity ratios involving these four lines show significant discrepancies atmore » the flare footpoints in the impulsive phase, and at the looptop in the gradual phase. Among these, the temperature derived from the Fe xxii/Fe xxiv intensity ratio is the lowest, which cannot be explained if we assume a Maxwellian electron distribution and ionization equilibrium, even in the case of a multithermal structure. This result suggests that the assumption of ionization equilibrium and/or a Maxwellian electron energy distribution can be violated in evaporating solar plasma around 10 MK.« less

  2. The Psychoanalytic Study of the Child, Volume XXIV.

    ERIC Educational Resources Information Center

    Eissler, Ruth S.; And Others

    Articles on psychoanalytic theory concern libidinal object constancy and mental representation, the unrememberable and unforgettable (repression), and the motive, meaning, and causality of anthropomorphism. Discussions of normal and pathological development include the following: levels of verbal communication in the schizophrenic child, a review…

  3. PRISM. Volume 2, Number 3, June 2011

    DTIC Science & Technology

    2011-06-01

    Institute (SIPRI) Background Paper (Stockholm: SIPRI, April 2009), 3, available at <http://books.sipri.org/files/misc/ SIPRIBP0904a.pdf>. 41 Martin ...Conflict (Washington, DC: CNA, 2010), 28. 46 Nenad Dimitrijevic and Petra Kovacs, “Managing Hatred and Distrust: Changes from the Bottom and the Top...Dimitrijevic and Petra Kovacs (Hungary: Open Society Institute, 2004), xxiv. 47 Simonsen, “Addressing Ethnic Divisions in Post-Conflict Institution-Building

  4. Democratization of the Arab Middle East: Possibility or Pipedream?

    DTIC Science & Technology

    2006-01-04

    As long as States have sufficient income they may have little reason to reform. Based on Luciani’s argument, Heather Deegan , a comparative Politics...and Problems of Democracy by Heather Deegan , (Boulder, CO: Rienner Publishing, 1994), pg viii. 2 George W. Bush, Foreword to the National Security...Middle East Policy 12 (Summer 2005): 28. 29 Ibid., 29. 30 Giacomo Luciani, The Arab State, (London 1990), pg xxiv. 31 Heather Deegan , The Middle East

  5. Exploration and Production of Hydrocarbon Resources in Coastal Alabama and Mississippi. Executive Summary.

    DTIC Science & Technology

    1984-11-01

    r .-. u S FINAL GENERIC ENVIROMENTAL IMPACT SlAiLMENT .XPLORAYION AND PRODUCTION OF HYDROCARBON RESOU CES IN COASTAL AIABAMA AND MISSISSIPPI The...a service could potentially affect cultural resources in the area of development. Prior to issuing any project permit, conflicts on potential impacts...34 Air Emission. 6-34 Noise 6-34 Solid and Hazardous Waste 6-34 Socioe -conomic Characteristics 6-34 Navigation 6-34 xxiv TABLE OF CONTENTS (Continued

  6. Spruce aphid (Elatobium abietinum Walker) (Hemiptera: Aphididae) [Chapter XXIV

    Treesearch

    Ann M. Lynch

    2014-01-01

    Elatobium abietinum Walker is a spruce-feeding aphid that in Europe is referred to as the green spruce aphid (Day et al., 1998a) (Fig. 1). However, in North America E. abietinum is known simply as the spruce aphid, while the common name "green spruce aphid" refers to a different species, Cinara fornacula Hottes (Hemiptera: Aphididae) (http://www.entsoc.org/...

  7. USSR and Eastern Europe Scientific Abstracts, Electronics and Electrical Engineering. Number 31

    DTIC Science & Technology

    1977-06-09

    RABOT VYCHISLITEL’NOGO TSENTRA MOSKOVSKOGO UNIVERSITETA in Russian 1975 pp 183-192 BEREZINA, N. I. and CHECHKIN , A . V . [Abstract] This paper deals...ZADACHAKH ELEKTRODINAMIKI) XXIV; SBORNIK RABOT VYCHISLITEL’NOGO TSENTRA MOSKOVSKOGO UNIVERSITETA in Russian 1975 pp 161-170 CHECHKIN , A . V ...flux in such a device described in terms of current I]_(ü),z) and kinetic potential VI(<ü,Z)= 2VQ V 1^> Z) as the variables. The law of power

  8. E-2 Systems Approach to Training: Development, Implementation, Evaluation, and Revision.

    DTIC Science & Technology

    1979-08-01

    1 1 2.0 xxII 2 2 3.3 XXIII 5 1.5 2 3.3 XXIV 1 2 1.5 2.- XXV 4 1 39 NAVTRAEQUIPCEN 78-C-0045-1 TABLE 2. (CONTINUED) lOIIhLI CARRIL CLASSROOM 1 SI-8 - 2...i i cvc r ed i -i a e ext reP me ly tnt e r,, t I n ______ b_ h. n te re s tinr% __________c. bo r ing _________d. extreme-ly bu )ring o. .IA 1

  9. Modeling X-Ray Photoionized Plasmas: Ion Storage Ring Measurements of Low Temperature Dielectronic Recombination Rate Coefficients for L-Shell Iron

    NASA Technical Reports Server (NTRS)

    Savin, D. W.; Badnell, N. R.; Bartsch, T.; Brandau, C.; Chen, M. H.; Grieser, M.; Gwinner, G.; Hoffknecht, A.; Kahn, S. M.; Linkemann, J.

    2000-01-01

    Iron L-shell ions (Fe XVII to Fe XXIV) play an important role in determining the line emission and thermal and ionization structures of photoionized gases. Existing uncertainties in the theoretical low temperature dielectronic recombination (DR) rate coefficients for these ions significantly affects our ability to model and interpret observations of photoionized plasmas. To help address this issue, we have initiated a laboratory program to produce reliable low temperature DR rates. Here, we present some of our recent results and discuss some of their astrophysical implications.

  10. Planck 2015 results. XXIV. Cosmology from Sunyaev-Zeldovich cluster counts

    NASA Astrophysics Data System (ADS)

    Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Bartolo, N.; Battaner, E.; Battye, R.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J.-F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.-R.; Chiang, H. C.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Désert, F.-X.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Weller, J.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.

    2016-09-01

    We present cluster counts and corresponding cosmological constraints from the Planck full mission data set. Our catalogue consists of 439 clusters detected via their Sunyaev-Zeldovich (SZ) signal down to a signal-to-noise ratio of 6, and is more than a factor of 2 larger than the 2013 Planck cluster cosmology sample. The counts are consistent with those from 2013 and yield compatible constraints under the same modelling assumptions. Taking advantage of the larger catalogue, we extend our analysis to the two-dimensional distribution in redshift and signal-to-noise. We use mass estimates from two recent studies of gravitational lensing of background galaxies by Planck clusters to provide priors on the hydrostatic bias parameter, (1-b). In addition, we use lensing of cosmic microwave background (CMB) temperature fluctuations by Planck clusters as an independent constraint on this parameter. These various calibrations imply constraints on the present-day amplitude of matter fluctuations in varying degrees of tension with those from the Planck analysis of primary fluctuations in the CMB; for the lowest estimated values of (1-b) the tension is mild, only a little over one standard deviation, while it remains substantial (3.7σ) for the largest estimated value. We also examine constraints on extensions to the base flat ΛCDM model by combining the cluster and CMB constraints. The combination appears to favour non-minimal neutrino masses, but this possibility does little to relieve the overall tension because it simultaneously lowers the implied value of the Hubble parameter, thereby exacerbating the discrepancy with most current astrophysical estimates. Improving the precision of cluster mass calibrations from the current 10%-level to 1% would significantly strengthen these combined analyses and provide a stringent test of the base ΛCDM model.

  11. Planck 2015 results: XXIV. Cosmology from Sunyaev-Zeldovich cluster counts

    DOE PAGES

    Ade, P. A. R.; Aghanim, N.; Arnaud, M.; ...

    2016-09-20

    In this work, we present cluster counts and corresponding cosmological constraints from the Planck full mission data set. Our catalogue consists of 439 clusters detected via their Sunyaev-Zeldovich (SZ) signal down to a signal-to-noise ratio of 6, and is more than a factor of 2 larger than the 2013 Planck cluster cosmology sample. The counts are consistent with those from 2013 and yield compatible constraints under the same modelling assumptions. Taking advantage of the larger catalogue, we extend our analysis to the two-dimensional distribution in redshift and signal-to-noise. We use mass estimates from two recent studies of gravitational lensing ofmore » background galaxies by Planck clusters to provide priors on the hydrostatic bias parameter, (1-b). In addition, we use lensing of cosmic microwave background (CMB) temperature fluctuations by Planck clusters as an independent constraint on this parameter. These various calibrations imply constraints on the present-day amplitude of matter fluctuations in varying degrees of tension with those from the Planck analysis of primary fluctuations in the CMB; for the lowest estimated values of (1-b) the tension is mild, only a little over one standard deviation, while it remains substantial (3.7σ) for the largest estimated value. We also examine constraints on extensions to the base flat ΛCDM model by combining the cluster and CMB constraints. The combination appears to favour non-minimal neutrino masses, but this possibility does little to relieve the overall tension because it simultaneously lowers the implied value of the Hubble parameter, thereby exacerbating the discrepancy with most current astrophysical estimates. In conclusion, improving the precision of cluster mass calibrations from the current 10%-level to 1% would significantly strengthen these combined analyses and provide a stringent test of the base ΛCDM model.« less

  12. Planck 2015 results: XXIV. Cosmology from Sunyaev-Zeldovich cluster counts

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Ade, P. A. R.; Aghanim, N.; Arnaud, M.

    In this work, we present cluster counts and corresponding cosmological constraints from the Planck full mission data set. Our catalogue consists of 439 clusters detected via their Sunyaev-Zeldovich (SZ) signal down to a signal-to-noise ratio of 6, and is more than a factor of 2 larger than the 2013 Planck cluster cosmology sample. The counts are consistent with those from 2013 and yield compatible constraints under the same modelling assumptions. Taking advantage of the larger catalogue, we extend our analysis to the two-dimensional distribution in redshift and signal-to-noise. We use mass estimates from two recent studies of gravitational lensing ofmore » background galaxies by Planck clusters to provide priors on the hydrostatic bias parameter, (1-b). In addition, we use lensing of cosmic microwave background (CMB) temperature fluctuations by Planck clusters as an independent constraint on this parameter. These various calibrations imply constraints on the present-day amplitude of matter fluctuations in varying degrees of tension with those from the Planck analysis of primary fluctuations in the CMB; for the lowest estimated values of (1-b) the tension is mild, only a little over one standard deviation, while it remains substantial (3.7σ) for the largest estimated value. We also examine constraints on extensions to the base flat ΛCDM model by combining the cluster and CMB constraints. The combination appears to favour non-minimal neutrino masses, but this possibility does little to relieve the overall tension because it simultaneously lowers the implied value of the Hubble parameter, thereby exacerbating the discrepancy with most current astrophysical estimates. In conclusion, improving the precision of cluster mass calibrations from the current 10%-level to 1% would significantly strengthen these combined analyses and provide a stringent test of the base ΛCDM model.« less

  13. Measurements of molybdenum radiation in the Alcator C-Mod tokamak using a multilayer mirror soft x-ray polychromator

    NASA Astrophysics Data System (ADS)

    May, M. J.; Finkenthal, M.; Regan, S. P.; Moos, H. W.; Terry, J. L.; Graf, M. A.; Fournier, K.; Goldstein, W. L.

    1995-01-01

    A photometrically calibrated polychromator utilizing layered synthetic microstructure coated flats (also known as multilayer mirrors, MLMs) as dispersive elements is operating on the Alcator C-Mod tokamak to measure the molybdenum emissions in the XUV. Molybdenum, the first wall material in C-Mod, is the dominant high Z impurity in the plasma. Three spectral regions are measured by three separate MLM-detector channels. The characteristic charge states in the region between 30-40 Å are Mo xv to Mo xx, between 65-90 Å are Mo xxiv to Mo xxvi, and between 110-130 Å are Mo xxxi and Mo xxxii. The instrument's spectral resolution varies from 0.4 Å at λ=30 Å to 7 Å at λ=130 Å. The temporal resolution is typically 1.0 ms, but sampling rates of less than 1 ms are possible. The instrument was photometrically calibrated at The Johns Hopkins University using a Manson soft x-ray light source. Power loss estimates from Mo xxiv to Mo xxvi, Mo xxxi, and Mo xxxii have been obtained during ohmic and ICRF plasmas using the mist transport code to model the molybdenum charge state distributions in the plasma. The Mo concentrations have also been determined. Mo contributes ˜0.1 to the Zeff of 1.3 during ohmic plasmas. This contribution increases during ICRF heating to ˜0.5 of the Zeff of 2. The polychromator functions as a time-resolved soft x-ray emission power loss monitor.

  14. Feasibility Study for a Structurally Efficient, Multi-Modal Shelter Concept Utilizing Advanced Technology Production Techniques

    DTIC Science & Technology

    1974-02-01

    II I~ x p:1 ns ion P roc cuurc Longitudin:-11 Section, Container Mod·c Configuration r Ex p :m s i on Pro c c d u r e Longitudinal Section...No . I II. I I I. IV. v. VI. VII. VIII. IX. X . XI. XII. XIII. XIV. XV . XVI. XVII . XVIII . XIX. XX. XXI. XXII . XXI II. XXIV...mat e rial s and examples from these categories . Glass Fibers Glass Mi c r os pheres As bestos Carbon Graphite Ce llulose Cotton Jute Rayo n

  15. Spectrum lines of highly ionized zinc, germanium, selenium, zirconium, molybdenum, and silver injected into Princeton Large Torus and Tokamak Fusion Test Reactor tokamak discharges

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Hinnov, E.; Boody, F.; Cohen, S.

    1986-10-01

    Measured wavelengths of a number of highly ionized atoms are reported. These include the 3s/sup 2/3p--3s3p/sup 2/ and 3s/sup 2/3p--3s/sup 2/3d transitions in the aluminum isoelectronic sequence of Zn XVIII, Ge XX, Se XXII, Zr XXVIII, Mo XXX, and Ag XXXV; several transitions in the n = 2 shell of Zn XXII, Zn XXIII, and Zn XXIV; and the resonance and intercombination lines of Ag XXXVI--Ag XXXVII and of Ge XXIX--Ge XXX.

  16. The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs

    NASA Astrophysics Data System (ADS)

    Wittenmyer, Robert A.; Butler, R. P.; Tinney, C. G.; Horner, Jonathan; Carter, B. D.; Wright, D. J.; Jones, H. R. A.; Bailey, J.; O'Toole, Simon J.

    2016-03-01

    We present updated simulations of the detectability of Jupiter analogs by the 17-year Anglo-Australian Planet Search. The occurrence rate of Jupiter-like planets that have remained near their formation locations beyond the ice line is a critical datum necessary to constrain the details of planet formation. It is also vital in our quest to fully understand how common (or rare) planetary systems like our own are in the Galaxy. From a sample of 202 solar-type stars, and correcting for imperfect detectability on a star-by-star basis, we derive a frequency of {6.2}-1.6+2.8% for giant planets in orbits from 3 to 7 au. When a consistent definition of “Jupiter analog” is used, our results are in agreement with those from other legacy radial-velocity surveys.

  17. Oral histories in meteoritics and planetary science—XXIV: William K. Hartmann

    NASA Astrophysics Data System (ADS)

    Sears, Derek W. G.

    2014-06-01

    In this interview, William Hartmann (Bill, Fig. 1) describes how he was inspired as a teenager by a map of the Moon in an encyclopedia and by the paintings by Chesley Bonestell. Through the amateur journal "Strolling Astronomer," he shared his interests with other teenagers who became lifelong colleagues. At college, he participated in Project Moonwatch, observing early artificial satellites. In graduate school, under Gerard Kuiper, Bill discovered Mare Orientale and other large concentric lunar basin structures. In the 1960s and 1970s, he used crater densities to study surface ages and erosive/depositional effects, predicted the approximately 3.6 Gyr ages of the lunar maria before the Apollo samples, discovered the intense pre-mare lunar bombardment, deduced the youthful Martian volcanism as part of the Mariner 9 team, and proposed (with Don Davis) the giant impact model for lunar origin. In 1972, he helped found (what is now) the Planetary Science Institute. From the late 1970s to early 1990s, Bill worked mostly with Dale Cruikshank and Dave Tholen at Mauna Kea Observatory, helping to break down the Victorian paradigm that separated comets and asteroids, and determining the approximately 4% albedo of comet nuclei. Most recently, Bill has worked with the imaging teams for several additional Mars missions. He has written three college textbooks and, since the 1970s, after painting illustrations for his textbooks, has devoted part of his time to painting, having had several exhibitions. He has also published two novels. Bill Hartmann won the 2010 Barringer Award for impact studies and the first Carl Sagan Award for outreach in 1997.

  18. Velocity Characteristics of Evaporated Plasma using Hinode/EIS

    NASA Technical Reports Server (NTRS)

    Milligan, Ryan O.; Dennis, Brian R.

    2009-01-01

    This paper presents a detailed study of chromospheric evaporation using the EUV Imaging Spectrometer (EIS) onboard Hinode in conjunction with HXR observat,ions from RHESSI. The advanced capabilities of EIS were used to measure Doppler shifts in 15 emission lines covering the temperature range T=0.05-16 MK during the impulsive phase of a C-class flare on 2007 December 14. Blueshifts indicative of the evaporated material were observed in six emission lines from Fe XIV-XXIV (2-16 MK). Upflow velocity was found to scale with temperature as v(sub up) (kilometers per second) approximately equal to 5-17 T (MK). Although the hottest emission lines, Fe XXIII and Fe XXIV, exhibited upflows of greater than 200 kilometers per second, their line profiles were found to be dominated by a stationary component in stark contrast to the predictions of the standard flare model. Emission from O VI-Fe XIII lines (0.5-1.5 MK) was found to be redshifted by v(sub down) (kilometers per second) approximately equal to 60-17 T (MK) and was interpreted as the downward-moving 'plug' characteristic of explosive evaporation. These downflows occur at temperatures significantly higher than previously expected. Both upflows and downflows were spatially and temporally correlated with HXR emission observed by RHESSI that provided the properties of the electron beam deemed to be the driver of the evaporation. The energy contained in the electron beam was found to be greater than or equal to 10(sup 11) ergs per square centimeter per second consistent with the value required to drive explosive chromospheric evaporation from hydrodynamic simulations.

  19. Cross sections and rate coefficients for excitation of Δn = 1 transitions in Li-like ions with 6 < Z < 42.

    NASA Astrophysics Data System (ADS)

    Safronova, U. I.; Safronova, M. S.; Kato, T.

    Excitation cross sections and rate coefficients by electron impact were calculated for the 1s22s - 1s2s2p, 1s22s - 1s2s2 and 1s22s - 1s2p2 transitions of the Li-like ions (C IV, N V, O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Ti XX, Fe XXIV, Ni XXVI, Zn XXVIII, Ge XXX, Se XXXII, Kr XXXIIV and Mo XXXX) by a Coulomb-Born approximation with exchange and including relativistic effects and configuration interactions. Level energies, mixing coefficients and transition wavelengths and probabilities were also computed.

  20. [Clinical research XXIV. From clinical judgment to ethics in research on humans].

    PubMed

    Pérez-Rodríguez, Marcela; Palacios-Cruz, Lino; Rivas-Ruiz, Rodolfo; Talavera, Juan O

    2014-01-01

    Bioethics in research is an essential part of the structured review process of an article and it is based on three fundamental principles: respect for persons, beneficence and justice. In addition to not providing valid knowledge, a research with inadequate design, execution and statistical analysis is not ethical either, since these methodological deficiencies will produce information that will not be useful and, therefore, the risks that the participants were exposed to will have been in vain. Beyond scientific validity, there are other aspects that outline if an investigation is ethical, such as the clinical and social value of a study, a fair selection of participants, favorable risk-benefit balance, an independent review, the informed consent and respect for participants and potential participants. Throughout the article here presented, the documents that profile the behavior of investigators to protect the participants, such as the Declaration of Helsinki, the national regulations that rule us and the differences between research without risk, with minimal risk and with greater than minimal risk are discussed. That like in daily life, behavior in research involving human participants must be self-regulated, ie, people with knowledge of the existence of the law discover that the man is outside the realm of nature where work is done under the necessity of natural causality, and falls within the scope of the will; only if the man is free to decide their actions may be a law regulating their action.

  1. Psychology of computer use: XXIV. Computer-related stress among technical college students.

    PubMed

    Ballance, C T; Rogers, S U

    1991-10-01

    Hudiburg's Computer Technology Hassles Scale, along with a measure of global stress and a scale on attitudes toward computers, were administered to 186 students in a two-year technical college. Hudiburg's work with the hassles scale as a measure of "technostress" was affirmed. Moderate, but statistically significant, correlations among the three scales are reported. No relationship between the hassles scale and achievement as measured by GPA was detected.

  2. Tabulation of comet observations.

    NASA Astrophysics Data System (ADS)

    1993-01-01

    Concerning comets: 1973 XII Kohoutek, 1975 IX Kobayashi-Berger-Milon, 1976 VI West, 1976 XI P/d'Arrest, 1977 XIV Kohler, 1979 X Bradfield, 1980 X P/Stephan-Oterma, 1980 XV Bradfield, 1981 II Panther, 1982 VI Austin, 1983 V Sugano-Saigusa-Fujikawa, 1983 VII IRAS-Araki-Alcock, 1983 XIII P/Kopff, 1984 XIII Austin, 1984 XXIII Levy-Rudenko, 1985 XIII P/Giacobini-Zinner, 1985 XVII Hartley-Good, 1985 XIX Thiele, 1986 I P/Boethin, 1986 III P/Halley, 1986 XVIII Terasako, 1987 II Sorrells, 1987 III Nishikawa-Takamizawa-Tago, 1987 X P/Grigg-Skjellerup, 1987 XXIII Rudenko, 1987 XXIX Bradfield, 1987 XXXII McNaught, 1987 XXXIII P/Borrelly, 1988 IV Furuyama, 1988 V Liller, 1988 XIV P/Tempel 2, 1988 XV Machholz, 1988 XX Yanaka, 1988 XXIV Yanaka, 1989 X P/Brorsen-Metcalf, 1989 XV P/Schwassmann-Wachmann 1, 1989 XIX Okazaki-Levy-Rudenko, 1989 XXI Helin-Roman-Alu, 1989 XXII Aarseth-Brewington, 1990 III Černis-Kiuchi-Nakamura, 1990 VI Skorichenko-George, 1990 VIII P/Schwassmann-Wachmann 3, 1990 IX P/Peters-Hartley, 1990 X P/Wild 4, 1990 XIV P/Honda Mrkos-Pajdušáková, 1990 XVII Tsuchiya-Kiuchi, 1990 XXI P/Encke, 1990 XXVI Arai, 1991 XI P/Levy, 1991 XV P/Hartley 2, 1991 XVI P/Wirtanen, 1991 XVII P/Arend-Rigaux, 1991 XXI P/Faye, 1991 XXIII P/Shoemaker 1, 1991 XXIV Shoemaker-Levy, 1991l Helin-Lawrence, 1991ο P/Chernykh, 1991r Helin-Alu, 1991a1 Shoemaker-Levy, 1991g1 Zanotta-Brewington, 1991h1 Mueller, 1912d Tanaka-Machholz, 1992f P/Shoemaker-Levy 8, 1992k Machholz, 1992l P/Giclas, 1992p P/Brewington, 1992q Helin-Lawrence, 1992s P/Ciffréo, 1992t P/Swift-Tuttle, 1992u P/Väisälä, 1992x P/Schaumasse, 1992y Shoemaker, 1992a1 Ohshita, 1993a Mueller, P/Smirnova-Chernykh.

  3. Diterpenoids from the flowers of Rhododendron molle.

    PubMed

    Zhou, Shuai-Zhen; Yao, Sheng; Tang, Chunping; Ke, Changqiang; Li, Lu; Lin, Ge; Ye, Yang

    2014-05-23

    A new seco-kalmane-type diterpenoid, seco-rhodomollone (1), five new grayanane-type diterpenoids, rhodomollein XXI (2), 6-O-acetylrhodomollein XXI (3), 6,14-di-O-acetylrhodomollein XXI (4), rhodomollein XXII (5), and 2-O-methylrhodomollein XI (6), and two new kalmane-type diterpenoids, rhodomolleins XXIII (7) and XXIV (8), together with seven known compounds, were isolated from the flowers of Rhododendron molle collected in Guangxi Province, China. The absolute configurations of 1 and 3 were defined by single-crystal X-ray diffraction experiments. Compound 1 possesses an unprecedented 1,5-seco-kalmane skeleton presumably derived by cleavage of the C-1-C-5 bond of the kalmane skeleton. Compounds 2-4 represent the first examples from a natural source of grayanane-type diterpenoids with a chlorine substituent.

  4. VizieR Online Data Catalog: ExoMol line lists. XXIV. SiH (Yurchenko+, 2018)

    NASA Astrophysics Data System (ADS)

    Yurchenko, S. N.; Sinden, F.; Lodi, L.; Hill, C.; Gorman, M. N.; Tennyson, J.

    2017-11-01

    The data for each isotopologue are in two parts. The first, s_*.dat contain lists of rovibronic states. Each state is labelled with the total angular momentum, state degeneracy, life time, Zeeman Lande-g factor, total (+/-) and e/f parities, vibrational quantum number, projection of the electronic, spin and total angular momenta. Each state has a unique number, which is the number of the row in which it appears in the file. This number is the means by which the state is related to the second part of the data system, the transitions files. The transition files t_*.dat contain four columns: the reference number in the energy file of the upper state; that of the lower state; the Einstein A coefficient of the transition; the transition wavenumber. (8 data files).

  5. Planck early results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo

    NASA Astrophysics Data System (ADS)

    Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Bernard, J.-P.; Bersanelli, M.; Bhatia, R.; Blagrave, K.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cardoso, J.-F.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L.-Y.; Chiang, C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J.-M.; Désert, F.-X.; Dickinson, C.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Joncas, G.; Jones, A.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Leroy, C.; Linden-Vørnle, M.; Lockman, F. J.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marshall, D. J.; Martin, P.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Pajot, F.; Paladini, R.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pinheiro Gonçalves, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Starck, J.-L.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J.-P.; Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.

    2011-12-01

    This paper presents the first results from a comparison of Planck dust maps at 353, 545 and 857GHz, along with IRAS data at 3000 (100 μm) and 5000GHz (60 μm), with Green Bank Telescope 21-cm observations of Hi in 14 fields covering more than 800 deg2 at high Galactic latitude. The main goal of this study is to estimate the far-infrared to sub-millimeter (submm) emissivity of dust in the diffuse local interstellar medium (ISM) and in the intermediate-velocity (IVC) and high-velocity clouds (HVC) of the Galactic halo. Galactic dust emission for fields with average Hi column density lower than 2 × 1020 cm-2 is well correlated with 21-cm emission because in such diffuse areas the hydrogen is predominantly in the neutral atomic phase. The residual emission in these fields, once the Hi-correlated emission is removed, is consistent with the expected statistical properties of the cosmic infrared background fluctuations. The brighter fields in our sample, with an average Hi column density greater than 2 × 1020 cm-2, show significant excess dust emission compared to the Hi column density. Regions of excess lie in organized structures that suggest the presence of hydrogen in molecular form, though they are not always correlated with CO emission. In the higher Hi column density fields the excess emission at 857 GHz is about 40% of that coming from the Hi, but over all the high latitude fields surveyed the molecular mass faction is about 10%. Dust emission from IVCs is detected with high significance by this correlation analysis. Its spectral properties are consistent with, compared to the local ISM values, significantly hotter dust (T ~ 20K), lower submm dust opacity normalized per H-atom, and a relative abundance of very small grains to large grains about four times higher. These results are compatible with expectations for clouds that are part of the Galactic fountain in which there is dust shattering and fragmentation. Correlated dust emission in HVCs is not detected; the average of the 99.9% confidence upper limits to the emissivity is 0.15 times the local ISM value at 857 and 3000GHz, in accordance with gas phase evidence for lower metallicity and depletion in these clouds. Unexpected anti-correlated variations of the dust temperature and emission cross-section per H atom are identified in the local ISM and IVCs, a trend that continues into molecular environments. This suggests that dust growth through aggregation, seen in molecular clouds, is active much earlier in the cloud condensation and star formation processes. Corresponding author: M.-A. Miville-Deschênes, e-mail: mamd@ias.u-psud.fr

  6. The beta Pictoris circumstellar disk. XXIV. Clues to the origin of the stable gas

    NASA Astrophysics Data System (ADS)

    Lagrange, A.-M.; Beust, H.; Mouillet, D.; Deleuil, M.; Feldman, P. D.; Ferlet, R.; Hobbs, L.; Lecavelier Des Etangs, A.; Lissauer, J. J.; McGrath, M. A.; McPhate, J. B.; Spyromilio, J.; Tobin, W.; Vidal-Madjar, A.

    1998-02-01

    GHRS high resolution spectra of {beta \\:Pictoris} were obtained to study the stable gas around this star. Several elements are detected and their abundances measured. Upper limits to the abundances of others are also measured. The data permit improved chemical analysis of the stable gas around {beta \\:Pictoris}, and yield new and more accurate estimates of the radiation pressure acting on various elements. We first analyze the data in the framework of a closed-box model. The electron density is evaluated (Neion {S}imeq10(6) cm(-3) ), which in turn implies constraints on the ionization stages of the various elements. The refractory elements in the stable gas have then standard abundances. In contrast, in this model, the lighter elements sulfur and carbon, observed in their neutral form, seem to be depleted. However several arguments, especially the strong radiation pressure, argue against a closed-box hypothesis. We therefore develop hydrodynamical simulations, taking into account the radiation pressure, to reproduce the stable features under three different hypotheses for the origin of the stable gas: stellar ejection, comet evaporation and grain evaporation. They show that a permanent production of gas is needed in order to sustain a stable absorption. In order to reproduce the observed zero velocity of the absorption features a mechanism is also needed to slow down the radial flow of matter. We show that this could be achieved by a colliding ring of neutral hydrogen farther than 0.5AU from the star. Applied to the Fe Ii\\ lines, the simulations constrain the temperature (Tion {S}imeq1500-2000K) and the velocity dispersion (ion {S}imeq2kms(-1) ) in the gaseous medium. When applied to Ca Ii\\ and to other UV lines, they test the chemical composition of the parent source of gas, which is found to have standard abundances in refractory elements. The gas production rate is ion {S}imeq 10(-16}M_{sun) yr(-1) . This description is the first consistent explanation for these long-lived stable absorptions observed for a large number of lines arising from a variety of energy levels in different chemical elements. It raises the question of the origin of the parent material, together with its composition and dynamics. This realizes a link between this gaseous component and the whole circumstellar system. Based on observations collected with the Hubble Space Telescope

  7. FLARE FOOTPOINT REGIONS AND A SURGE OBSERVED BY HINODE/EIS, RHESSI, AND SDO/AIA

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Doschek, G. A.; Warren, H. P.; Dennis, B. R.

    2015-11-01

    The Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft observed flare footpoint regions coincident with a surge for an M3.7 flare observed on 2011 September 25 at N12 E33 in active region 11302. The flare was observed in spectral lines of O vi, Fe x, Fe xii, Fe xiv, Fe xv, Fe xvi, Fe xvii, Fe xxiii, and Fe xxiv. The EIS observations were made coincident with hard X-ray bursts observed by RHESSI. Overlays of the RHESSI images on the EIS raster images at different wavelengths show a spatial coincidence of features in the RHESSI images with the EIS upflowmore » and downflow regions, as well as loop-top or near-loop-top regions. A complex array of phenomena were observed, including multiple evaporation regions and the surge, which was also observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly telescopes. The slit of the EIS spectrometer covered several flare footpoint regions from which evaporative upflows in Fe xxiii and Fe xxiv lines were observed with Doppler speeds greater than 500 km s{sup −1}. For ions such as Fe xv both evaporative outflows (∼200 km s{sup −1}) and downflows (∼30–50 km s{sup −1}) were observed. Nonthermal motions from 120 to 300 km s{sup −1} were measured in flare lines. In the surge, Doppler speeds are found from about 0 to over 250 km s{sup −1} in lines from ions such as Fe xiv. The nonthermal motions could be due to multiple sources slightly Doppler-shifted from each other or turbulence in the evaporating plasma. We estimate the energetics of the hard X-ray burst and obtain a total flare energy in accelerated electrons of ≥7 × 10{sup 28} erg. This is a lower limit because only an upper limit can be determined for the low-energy cutoff to the electron spectrum. We find that detailed modeling of this event would require a multithreaded model owing to its complexity.« less

  8. Survey of Students and Non-Students about Continuing Education Market Place. Volume XXIV, Number 16.

    ERIC Educational Resources Information Center

    Lucas, John A.; And Others

    To evaluate the outreach and marketing efforts for its non-credit offerings, William Rainey Harper College in Illinois conducted a study of recent continuing education students in spring 1996. First, a random sample of 200 former students who had enrolled in continuing education courses in the past 5 years was surveyed, receiving 57 completed…

  9. ExoMol line lists XXIV: a new hot line list for silicon monohydride, SiH

    NASA Astrophysics Data System (ADS)

    Yurchenko, Sergei N.; Sinden, Frances; Lodi, Lorenzo; Hill, Christian; Gorman, Maire N.; Tennyson, Jonathan

    2018-02-01

    SiH has long been observed in the spectrum of our Sun and other cool stars. Computed line lists for the main isotopologues of silicon monohydride, 28SiH, 29SiH, 30SiH and 28SiD are presented. These line lists consider rotation-vibration transitions within the ground X 2Π electronic state as well as transitions to the low-lying A 2Δ and a 4Σ- states. Ab initio potential energy (PECs) and dipole moment curves along with spin-orbit and electronic angular momentum couplings between them are calculated using the multireference configuration interaction level of theory with the MOLPRO package. The PEC for the ground X 2Π state is refined to available experimental data with a typical accuracy of around 0.01 cm-1 or better. The 28SiH line list includes 11 785 rovibronic states and 1724 841 transitions with associated Einstein-A coefficients for angular momentum J up to 82.5 and covering wavenumbers up to 31 340 cm-1 (λ < 0.319 μm). Spectra are simulated using the new line list and comparisons made with various experimental spectra. These line lists are applicable up to temperatures of 5000 K, making them relevant to astrophysical objects such as exoplanetary atmospheres and cool stars and opening up the possibility of detection in the interstellar medium. These line lists, called SiGHTLY, are available at the ExoMol (www.exomol.com) and CDS data base websites.

  10. Fe L-shell Excitation Cross Section Measurements on EBIT-I

    NASA Astrophysics Data System (ADS)

    Chen, Hui; Beiersdorfer, P.; Brown, G.; Boyce, K.; Kelley, R.; Kilbourne, C.; Porter, F.; Gu, M. F.; Kahn, S.

    2006-09-01

    We report the measurement of electron impact excitation cross sections for the strong iron L-shell 3-2 lines of Fe XVII to Fe XXIV at the LLNL EBIT-I electron beam ion trap using a crystal spectrometer and NASA-Goddard Space Flight Center's 6x6 pixel array microcalorimeter. The cross sections were determined by direct normalization to the well-established cross sections for radiative electron capture. Our results include the excitation cross section for over 50 lines at multiple electron energies. Although we have found that for 3C line in Fe XVII the measured cross sections differ significantly from theory, in most cases the measurements and theory agree within 20%. This work was performed under the auspices of the U.S. DOE by LLNL under contract No. W-7405-Eng-48 and supported by NASA APRA grants to LLNL, GSFC, and Stanford University.

  11. DOE Office of Scientific and Technical Information (OSTI.GOV)

    Bhatia, A.K.; Seely, J.F.; Feldman, U.

    Oscillator strengths, radiative decay rates, and electron collision strengths have been calculated for the N-like ions Ar XII, Ti XVI, Fe XX, Zn XXIV, and Kr XXX. Included in the calculation are the 72 levels of the configurations 2s{sup 2}2p{sup 3}, 2s2p{sup 4}, 2p{sup 5}, 2s{sup 2}2p{sup 2}3s, 2s{sup 2}2p{sup 2}3p, and 2s{sup 2}2p{sup 2}3d. The level populations are calculated for the electron densities 10{sup 13}, 10{sup 14}, and 10{sup 15} cm{sup {minus}3}, and the spectral line intensities of the transitions from these levels are presented. The calculated intensities are in good agreement with the relative intensities observed in themore » spectra from the PLT tokamak.« less

  12. Quantum-Like Model for Decision Making Process in Two Players Game. A Non-Kolmogorovian Model

    NASA Astrophysics Data System (ADS)

    Asano, Masanari; Ohya, Masanori; Khrennikov, Andrei

    2011-03-01

    In experiments of games, players frequently make choices which are regarded as irrational in game theory. In papers of Khrennikov (Information Dynamics in Cognitive, Psychological and Anomalous Phenomena. Fundamental Theories of Physics, Kluwer Academic, Norwell, 2004; Fuzzy Sets Syst. 155:4-17, 2005; Biosystems 84:225-241, 2006; Found. Phys. 35(10):1655-1693, 2005; in QP-PQ Quantum Probability and White Noise Analysis, vol. XXIV, pp. 105-117, 2009), it was pointed out that statistics collected in such the experiments have "quantum-like" properties, which can not be explained in classical probability theory. In this paper, we design a simple quantum-like model describing a decision-making process in a two-players game and try to explain a mechanism of the irrational behavior of players. Finally we discuss a mathematical frame of non-Kolmogorovian system in terms of liftings (Accardi and Ohya, in Appl. Math. Optim. 39:33-59, 1999).

  13. High resolution X-ray spectra of solar flares. V - Interpretation of inner-shell transitions in Fe XX-Fe XXIII

    NASA Technical Reports Server (NTRS)

    Doschek, G. A.; Feldman, U.; Cowan, R. D.

    1981-01-01

    The paper examines high-resolution solar flare iron line spectra recorded between 1.82 and 1.97 A by a spectrometer flown by the Naval Research Laboratory on an Air Force spacecraft launched on 1979 February 24. The emission line spectrum is due to inner-shell transitions in the ions Fe XX-Fe XXV. Using theoretical spectra and calculations of line intensities obtained by methods discussed by Merts, Cowan, and Magee (1976), electron temperatures as a function of time for two large class X flares are derived. These temperatures are deduced from intensities of lines of Fe XXII, Fe XXIII, and Fe XXIV. The determination of the differential emission measure between about 12-million and 20-million K using these temperatures is considered. The possibility of determining electron densities in flare and tokamak plasmas using the inner-shell spectra of Fe XXI and Fe XX is discussed.

  14. Non-thermal Motions in and above Flare Loop Tops Measured by the Extreme-ultraviolet Imaging Spectrometer on Hinode

    NASA Astrophysics Data System (ADS)

    Doschek, G. A.; Warren, H. P.

    2013-12-01

    The plasma volume above the soft X-ray emitting loop tops is of particular interest for studying the formation of flare loops. We present observations of non-thermal motions (turbulence) determined from spectral line profiles Fe XXIII and Fe XXIV ions. We compare the non-thermal motions at temperatures near 10 MK with the motions along the same lines-of-sight determined from lines of coronal ions such as Fe XII, Fe XIV, and Fe XV formed at 1-2 MK. We discuss the results in terms of predictions of the effects of magnetic reconnection and non-thermal motion results obtained in flares from earlier X-ray Yohkoh observations of line profiles of Fe XXV and Ca XIX. Fe XXV is formed at significantly higher temperatures than any strong flare EUV spectral line observed by EIS or by imaging telescopes such as AIA or TRACE. This work is supported by a NASA Hinode grant.

  15. Cross sections and rate coefficients for inner-shell excitation of Li-like ions with 6 < Z < 42

    NASA Astrophysics Data System (ADS)

    Safronova, U. I.; Safronova, M. S.; Kato, T.

    1996-07-01

    Excitation cross sections and rate coefficients by electron impact were calculated for the 1s22s-1s2s2p, 1s22s-1s2s2 and 1s22s-1s2p2 transitions of the Li-like ions (C IV, N V, O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Ti XX, Fe XXIV, Ni XXVI, Zn XXVIII, Ge XXX, Se XXXII, Kr XXXIV and Mo XXXX) in the Coulomb-Born approximation with exchange including relativistic effects and configuration interaction. Level energies, mixing coefficients and transition wavelengths and probabilities were also computed. Calculations performed by the 1/Z perturbation theory and Coulomb-Born approximation are compared with the R-matrix method and the distorted-wave approximation were Z is the nuclear charge. Formulae obtained for the angular factors of n-electron atomic system allow one to generalize this method to an arbitrary system of highly charged ions.

  16. AUTOMOTIVE DIESEL MAINTENANCE 2. UNIT XXIV, MICHIGAN/CLARK TRANSMISSION--OIL FLOW THROUGH THE CONTROL COVER ASSEMBLY.

    ERIC Educational Resources Information Center

    Human Engineering Inst., Cleveland, OH.

    THIS MODULE OF A 25-MODULE COURSE IS DESIGNED TO DEVELOP AN UNDERSTANDING OF THE SERVICING PROCEDURES FOR THE CONTROL SYSTEM OF A SPECIFIC TRANSMISSION USED ON DIESEL POWERED EQUIPMENT. TOPICS ARE EXAMINING THE CONTROL COVER ASSEMBLY, REGULATING VALVE AND SAFETY VALVE, AND INSPECTING THE SYSTEM. THE MODULE CONSISTS OF A SELF-INSTRUCTIONAL…

  17. The VMC Survey - XXIV. Signatures of tidally stripped stellar populations from the inner Small Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Subramanian, Smitha; Rubele, Stefano; Sun, Ning-Chen; Girardi, Léo; de Grijs, Richard; van Loon, Jacco Th.; Cioni, Maria-Rosa L.; Piatti, Andrés E.; Bekki, Kenji; Emerson, Jim; Ivanov, Valentin D.; Kerber, Leandro; Marconi, Marcella; Ripepi, Vincenzo; Tatton, Benjamin L.

    2017-05-01

    We study the luminosity function of intermediate-age red clump stars using deep, near-infrared photometric data covering ˜20 deg2 located throughout the central part of the Small Magellanic Cloud (SMC), comprising the main body and the galaxy's eastern wing, based on observations obtained with the VISTA Survey of the Magellanic Clouds (VMC). We identified regions that show a foreground population (˜11.8 ± 2.0 kpc in front of the main body) in the form of a distance bimodality in the red clump distribution. The most likely explanation for the origin of this feature is tidal stripping from the SMC rather than the extended stellar haloes of the Magellanic Clouds and/or tidally stripped stars from the Large Magellanic Cloud. The homogeneous and continuous VMC data trace this feature in the direction of the Magellanic Bridge and, particularly, identify (for the first time) the inner region (˜2-2.5 kpc from the centre) from where the signatures of interactions start becoming evident. This result provides observational evidence of the formation of the Magellanic Bridge from tidally stripped material from the SMC.

  18. Ion Storage Ring Measurements of Low Temperature Dielectronic Recombination Rate Coefficients for Modeling X-Ray Photoionized Cosmic Plasmas

    NASA Technical Reports Server (NTRS)

    Savin, D. W.; Gwinner, G.; Schwalm, D.; Wolf, A.; Mueller, A.; Schippers, S.

    2002-01-01

    Low temperature dielectronic recombination (DR) is the dominant recombination mechanism for most ions in X-ray photoionized cosmic plasmas. Reliably modeling and interpreting spectra from these plasmas requires accurate low temperature DR rate Coefficients. Of particular importance are the DR rate coefficients for the iron L-shell ions (Fe XVII-Fe XXIV). These ions are predicted to play an important role in determining the thermal structure and line emission of X-ray photoionized plasmas, which form in the media surrounding accretion powered sources such as X-ray binaries (XRBs), active galactic nuclei (AGN), and cataclysmic variables (Savin et al., 2000). The need for reliable DR data of iron L-shell ions has become particularly urgent after the launches of Chandra and XMM-Newton. These satellites are now providing high-resolution X-ray spectra from a wide range of X-ray photoionized sources. Interpreting the spectra from these sources requires reliable DR rate coefficients. However, at the temperatures relevant, for X-ray photoionized plasmas, existing theoretical DR rate coefficients can differ from one another by factors of two to orders of magnitudes.

  19. X-ray spectrum of Capella and its relation to coronal structure and ultraviolet emission

    NASA Technical Reports Server (NTRS)

    Mewe, R.; Gronenschild, E. H. B. M.; Heise, J.; Brinkman, A. C.; Dijkstra, J. H.; Westergaard, N. J.; Schnopper, H. W.; Seward, F. D.; Chlebowski, T.; Kuin, N. P. M.

    1982-01-01

    The binary system Capella has been observed on 1979 March 15 and on 1980 March 15-17, with the objective grating spectrometer on board the Einstein Observatory. The spectrum measured with the 1000 1/mm grating covers the range 5-30 A with a resolution less than 1 A. The spectra show evidence for a bimodal temperature distribution of emission measure in an optically thin plasma with one component about 5,000,000 K and the other one about 10,000,000 K. Spectral features can be identified with line emissions from O VIII, Fe XVII, Fe XVIII, Fe XXIV, and Ne X ions. Good spectral fits have been obtained assuming standard cosmic abundances. The data are interpreted in terms of emission from hot static coronal loops rather similar to the magnetic arch structures found on the sun. It is shown that the conditions for such a model can exist on Capella. Typical values of loop base pressure and half-length are derived for both temperature components and discussed in relation to UV observations.

  20. OBSERVATIONS OF THERMAL FLARE PLASMA WITH THE EUV VARIABILITY EXPERIMENT

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Warren, Harry P.; Doschek, George A.; Mariska, John T.

    2013-06-20

    One of the defining characteristics of a solar flare is the impulsive formation of very high temperature plasma. The properties of the thermal emission are not well understood, however, and the analysis of solar flare observations is often predicated on the assumption that the flare plasma is isothermal. The EUV Variability Experiment (EVE) on the Solar Dynamics Observatory provides spectrally resolved observations of emission lines that span a wide range of temperatures (e.g., Fe XV-Fe XXIV) and allow for thermal flare plasma to be studied in detail. In this paper we describe a method for computing the differential emission measuremore » distribution in a flare using EVE observations and apply it to several representative events. We find that in all phases of the flare the differential emission measure distribution is broad. Comparisons of EVE spectra with calculations based on parameters derived from the Geostationary Operational Environmental Satellites soft X-ray fluxes indicate that the isothermal approximation is generally a poor representation of the thermal structure of a flare.« less

  1. Nor-Ursodeoxycholic Acid as a Novel Therapeutic Approach for Cholestatic and Metabolic Liver Diseases.

    PubMed

    Halilbasic, Emina; Steinacher, Daniel; Trauner, Michael

    2017-01-01

    Norursodeoxycholic acid (norUDCA) is a side-chain-shortened derivative of ursodeoxycholic acid with relative resistance to amidation, which enables its cholehepatic shunting. Based on its specific pharmacologic properties, norUDCA is a promising drug for a range of cholestatic liver and bile duct disorders. Recently, norUDCA has been successfully tested clinically in patients with primary sclerosing cholangitis (PSC) as first application in patients. Moreover, hepatic enrichment of norUDCA facilitates direct therapeutic effects on both parenchymal and non-parenchymal liver cells, thereby counteracting cholestasis, steatosis, hepatic inflammation and fibrosis, inhibiting hepatocellular proliferation, and promoting autophagy. This may open its therapeutic use to other non-cholestatic and metabolic liver diseases. This review article is a summary of a lecture given at the XXIV International Bile Acid Meeting (Falk Symposium 203) on "Bile Acids in Health and Disease" held in Düsseldorf, on June 17-18, 2016 and summarizes the recent progress of norUDCA as novel therapeutic approach in cholestatic and metabolic liver disorders with a specific focus on PSC. © 2017 S. Karger AG, Basel.

  2. Follow-Up Study of Former Materials/Logistics Management Students at Harper College, 1990-1995. Volume XXIV, Number 14.

    ERIC Educational Resources Information Center

    Lucas, John A.; Magad, Eugene

    In fall 1995, William Rainey Harper College in Illinois conducted a study of former students in the Materials/Logistics Management (MLM) program to determine their evaluation of their educational experiences in the program. The sample consisted of 298 former MLM students from 1990 to 1995, including 119 students who had earned 48 credit hours but…

  3. The VLT-FLAMES Tarantula Survey . XXIV. Stellar properties of the O-type giants and supergiants in 30 Doradus

    NASA Astrophysics Data System (ADS)

    Ramírez-Agudelo, O. H.; Sana, H.; de Koter, A.; Tramper, F.; Grin, N. J.; Schneider, F. R. N.; Langer, N.; Puls, J.; Markova, N.; Bestenlehner, J. M.; Castro, N.; Crowther, P. A.; Evans, C. J.; García, M.; Gräfener, G.; Herrero, A.; van Kempen, B.; Lennon, D. J.; Maíz Apellániz, J.; Najarro, F.; Sabín-Sanjulián, C.; Simón-Díaz, S.; Taylor, W. D.; Vink, J. S.

    2017-04-01

    Context. The Tarantula region in the Large Magellanic Cloud (LMC) contains the richest population of spatially resolved massive O-type stars known so far. This unmatched sample offers an opportunity to test models describing their main-sequence evolution and mass-loss properties. Aims: Using ground-based optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS), we aim to determine stellar, photospheric and wind properties of 72 presumably single O-type giants, bright giants and supergiants and to confront them with predictions of stellar evolution and of line-driven mass-loss theories. Methods: We apply an automated method for quantitative spectroscopic analysis of O stars combining the non-LTE stellar atmosphere model fastwind with the genetic fitting algorithm pikaia to determine the following stellar properties: effective temperature, surface gravity, mass-loss rate, helium abundance, and projected rotational velocity. The latter has been constrained without taking into account the contribution from macro-turbulent motions to the line broadening. Results: We present empirical effective temperature versus spectral subtype calibrations at LMC-metallicity for giants and supergiants. The calibration for giants shows a +1kK offset compared to similar Galactic calibrations; a shift of the same magnitude has been reported for dwarfs. The supergiant calibrations, though only based on a handful of stars, do not seem to indicate such an offset. The presence of a strong upturn at spectral type O3 and earlier can also not be confirmed by our data. In the spectroscopic and classical Hertzsprung-Russell diagrams, our sample O stars are found to occupy the region predicted to be the core hydrogen-burning phase by state-of-the-art models. For stars initially more massive than approximately 60 M⊙, the giant phase already appears relatively early on in the evolution; the supergiant phase develops later. Bright giants, however, are not systematically positioned between giants and supergiants at Minit ≳ 25 M⊙. At masses below 60 M⊙, the dwarf phase clearly precedes the giant and supergiant phases; however this behavior seems to break down at Minit ≲ 18 M⊙. Here, stars classified as late O III and II stars occupy the region where O9.5-9.7 V stars are expected, but where few such late O V stars are actually seen. Though we can not exclude that these stars represent a physically distinct group, this behavior may reflect an intricacy in the luminosity classification at late O spectral subtype. Indeed, on the basis of a secondary classification criterion, the relative strength of Si iv to He I absorption lines, these stars would have been assigned a luminosity class IV or V. Except for five stars, the helium abundance of our sample stars is in agreement with the initial LMC composition. This outcome is independent of their projected spin rates. The aforementioned five stars present moderate projected rotational velocities (I.e., νesini < 200kms-1) and hence do not agree with current predictions of rotational mixing in main-sequence stars. They may potentially reveal other physics not included in the models such as binary-interaction effects. Adopting theoretical results for the wind velocity law, we find modified wind momenta for LMC stars that are 0.3 dex higher than earlier results. For stars brighter than 105 L⊙, that is, in the regime of strong stellar winds, the measured (unclumped) mass-loss rates could be considered to be in agreement with line-driven wind predictions if the clump volume filling factors were fV 1/8 to 1/6. Based on observations collected at the European Southern Observatory under program ID 182.D-0222.Tables C.1-C.5 are also available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/600/A81

  4. Probing the Inflow/Out-flow and Accretion Disk of Cyg X-1 in the High State with HETG/Chandra

    NASA Technical Reports Server (NTRS)

    Feng, Y. X.; Tennant, A. F.; Zhang, S. N.

    2003-01-01

    Cyg X- 1 was observed in the high state at the conjunction orbital phase (0) with HETG/Chandra. Strong and asymmetric absorption lines of highly ionized species were detected, such as Fe XXV, Fe XXIV, Fe XXIII, Si XIV, S XVI, Ne X, and etc. In the high state the profile of the absorption lines are composed of an extended red wing and a less extended blue wing. The red wings of higher ionized species are more extended than that of lower ionized species. The detection of these lines provides a way to probe the properties of the flow around the companion and the black hole in Cyg X-1 during the high state. A broad emission feature around 6.5 keV was significantly detected from the both spectra of HETG/Chandra and PCA/RXTE. This feature appears to be symmetric and can be fitted with a Gaussian function rather than the Laor disk line model of fluorescent Fe K$ \\alpha$ line from an accretion disk. The implications of these results on the structure of the accretion flow of Cyg X-1 in the high state are discussed.

  5. Probing the Inflow/Outflow and Accretion Disk of Cygnus X-1 in the High State with the Chandra High Energy Transmission Grating

    NASA Technical Reports Server (NTRS)

    Feng, Y. X.; Tennant, A. F.; Zhang, S. N.

    2003-01-01

    Cygnus X-1 was observed in the high state at the conjunction orbital phase (0) with Chandra High Energy Transmission Grating (HETG). Strong and asymmetric absorption lines of highly ionized species were detected, such as Fe xxv, Fe xxiv, Fe xxiii, Si xiv, S xvi, Ne x, etc. In the high state the profile of the absorption lines is composed of an extended red wing and a less extended blue wing. The red wings of higher ionized species are more extended than those of lower ionized species. The detection of these lines provides a way to probe the properties of the flow around the companion and the black hole in Cyg X-1 during the high state. A broad emission feature around 6.5 keV was significantly detected from the spectra of both the Chandra/HETG and the RXTE/Proportional Counter Array. This feature appears to be symmetric and can be fitted with a Gaussian function rather than the Laor disk line model of the fluorescent Fe K(alpha) line from an accretion disk. The implications of these results on the structure of the accretion flow of Cyg X-1 in the high state are discussed.

  6. Trends in qualifying biomarkers in drug safety. Consensus of the 2011 meeting of the spanish society of clinical pharmacology.

    PubMed

    Agúndez, José A G; Del Barrio, Jaime; Padró, Teresa; Stephens, Camilla; Farré, Magí; Andrade, Raúl J; Badimon, Lina; García-Martín, Elena; Vilahur, Gemma; Lucena, M Isabel

    2012-01-01

    In this paper we discuss the consensus view on the use of qualifying biomarkers in drug safety, raised within the frame of the XXIV meeting of the Spanish Society of Clinical Pharmacology held in Málaga (Spain) in October, 2011. The widespread use of biomarkers as surrogate endpoints is a goal that scientists have long been pursuing. Thirty years ago, when molecular pharmacogenomics evolved, we anticipated that these genetic biomarkers would soon obviate the routine use of drug therapies in a way that patients should adapt to the therapy rather than the opposite. This expected revolution in routine clinical practice never took place as quickly nor with the intensity as initially expected. The concerted action of operating multicenter networks holds great promise for future studies to identify biomarkers related to drug toxicity and to provide better insight into the underlying pathogenesis. Today some pharmacogenomic advances are already widely accepted, but pharmacogenomics still needs further development to elaborate more precise algorithms and many barriers to implementing individualized medicine exist. We briefly discuss our view about these barriers and we provide suggestions and areas of focus to advance in the field.

  7. Laser gain on 3p-3d and 3s-3p transitions and X-ray line ratios for the nitrogen isoelectronic sequence

    NASA Technical Reports Server (NTRS)

    Feldman, U.; Seely, J. F.; Bhatia, A. K.

    1989-01-01

    Results are presented on calculations of the 72 levels belonging to the 2s(2)2p(3), 2s2p(4), 2p(5), 2s(2)2p(2)3s, 2s(2)2p(2)3p, and 2s(2)2p(2)3d configurations of the N I isoelectronic sequence for the ions Ar XII, Ti XVI, Fe XX, Zn XXIV, and Kr XXX, for electron densities up to 10 to the 24th/cu cm. It was found that large population inversions and gain occur between levels in the 2s(2)2p(2)3p configuration and levels in the 2s(2)2p(2)3d configuration that cannot decay to the ground configuration by an electric dipole transition. For increasing electron densities, the intensities of the X-ray transitions from the 2s(2)2p(2)3p configuration to the ground configuration decrease relative to the transitions from the 2s(2)2p(2)3s and 2s(2)2p(2)3d configurations to the ground configuration. The density dependence of these X-ray line ratios is presented.

  8. Follow-Up Study of Students Who Enrolled in Small Business Non-Credit Courses at Harper College. Volume XXIV, Number 8.

    ERIC Educational Resources Information Center

    Lucas, John A.; Soto, Linda

    As part of a review of its Small Business Management courses and seminars, William Rainey Harper College in Illinois conducted a study of students currently enrolled in spring 1995 and students who had enrolled from fall 1993 to fall 1994 to determine the students' characteristics, the effectiveness of marketing efforts, and students' perceptions…

  9. Plasma dynamics above solar flare soft x-ray loop tops

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Doschek, G. A.; Warren, H. P.; McKenzie, D. E.

    2014-06-10

    We measure non-thermal motions in flare loop tops and above the loop tops using profiles of highly ionized spectral lines of Fe XXIV and Fe XXIII formed at multimillion-degree temperatures. Non-thermal motions that may be due to turbulence or multiple flow regions along the line of sight are extracted from the line profiles. The non-thermal motions are measured for four flares seen at or close to the solar limb. The profile data are obtained using the Extreme-ultraviolet Imaging Spectrometer on the Hinode spacecraft. The multimillion-degree non-thermal motions are between 20 and 60 km s{sup –1} and appear to increase withmore » height above the loop tops. Motions determined from coronal lines (i.e., lines formed at about 1.5 MK) tend to be smaller. The multimillion-degree temperatures in the loop tops and above range from about 11 MK to 15 MK and also tend to increase with height above the bright X-ray-emitting loop tops. The non-thermal motions measured along the line of sight, as well as their apparent increase with height, are supported by Solar Dynamics Observatory Atmospheric Imaging Assembly measurements of turbulent velocities in the plane of the sky.« less

  10. Sea Level Station Metadata for Tsunami Detection, Warning and Research

    NASA Astrophysics Data System (ADS)

    Stroker, K. J.; Marra, J.; Kari, U. S.; Weinstein, S. A.; Kong, L.

    2007-12-01

    -priority metadata requirements identified at a water level workshop held at the XXIV IUGG Meeting in Perugia will be addressed: consistent, validated, and well defined numbers (e.g. amplitude); exact location of sea level stations; a complete record of sea level data stored in the archive; identifying high-priority sea level stations; and consistent definitions. NOAA's National Geophysical Data Center (NGDC) and co-located World Data Center for Solid Earth Geophysics (including tsunamis) would hold the archive of the sea level station data and distribute the standard metadata. Currently, NGDC is also archiving and distributing the DART buoy deep-ocean water level data and metadata in standards based formats. Kari, Uday S., John J. Marra, Stuart A. Weinstein, 2006 A Tsunami Focused Data Sharing Framework For Integration of Databases that Describe Water Level Station Specifications. AGU Fall Meeting, 2006. San Francisco, California. Marra, John, J., Uday S. Kari, and Stuart A. Weinstein (in press). A Tsunami Detection and Warning-focused Sea Level Station Metadata Web Service. IUGG XXIV, July 2-13, 2007. Perugia, Italy.

  11. NASA/DOD Aerospace Knowledge Diffusion Research Project. XXIV - A general approach to measuring the value of aerospace information products and services

    NASA Technical Reports Server (NTRS)

    Brinberg, Herbert R.; Pinelli, Thomas E.

    1993-01-01

    This paper discusses the various approaches to measuring the value of information, first defining the meanings of information, economics of information, and value. It concludes that no general model of measuring the value of information is possible and that the usual approaches, such as cost/benefit equations, have very limited applications. It also concludes that in specific contexts with given goals for newly developed products and services or newly acquired information, there is a basis for its objective valuation. The axioms and inputs for such a model are described and directions for further verification and analysis are proposed.

  12. Creating the Future through Research. Proceedings of the National Agricultural Education Research Meeting (Las Vegas, Nevada, December 10, 1997). Volume XXIV.

    ERIC Educational Resources Information Center

    Connors, James J., Ed.; Murphy, Tim H., Ed.

    The following are among the 51 papers and 7 poster sessions included: "Agriculture in the Classroom" (Hillison); "Effects of an Elementary Agri-Science Program on Student Perceptions of and Performance in Agriculture and Science" (Howell); "Current Status of Preservice Teacher Education Programs in Agriculture" (Swortzel); "Problems and Challenges…

  13. An Fe XXIV Absorption Line in the Persistent Spectrum of the Dipping Low-mass X-Ray Binary 1A 1744-361

    NASA Astrophysics Data System (ADS)

    Gavriil, Fotis P.; Strohmayer, Tod E.; Bhattacharyya, Sudip

    2012-07-01

    We report on Chandra X-ray Observatory (Chandra) High Energy Transmission Grating spectra of the dipping low-mass X-ray binary 1A 1744-361 during its 2008 July outburst. We find that its persistent emission is well modeled by a blackbody (kT ~ 1.0 keV) plus power law (Γ ~ 1.7) with an absorption edge. In the residuals of the combined spectrum, we find a significant absorption line at 6.961 ± 0.002 keV, consistent with the Fe XXVI (hydrogen-like Fe) 2-1 transition. We place an upper limit on the velocity of a redshifted flow of v < 221 km s-1. We find an equivalent width for the line of 27+2 - 3 eV, from which we determine a column density of (7 ± 1) × 1017 cm-2 via a curve-of-growth analysis. Using XSTAR simulations, we place a lower limit on the ionization parameter of >103.6 erg cm s-1. We discuss what implications the feature has on the system and its geometry. We also present Rossi X-ray Timing Explorer data accumulated during this latest outburst and, via an updated color-color diagram, clearly show that 1A 1744-361 is an "atoll" source.

  14. An Fe XXIV Absorption Line in the Persistent Spectrum of the Dipping Low-Mass X-Ray Binary 1A 1744-361

    NASA Technical Reports Server (NTRS)

    Gavriil, Fotis P.; Strohmayer, Tod E.; Bhattacharyya, Sudip

    2012-01-01

    We report on Chandra X-ray Observatory (Chandra) High Energy Transmission Grating spectra of the dipping low-mass X-ray binary 1A 1744-361 during its 2008 July outburst. We find that its persistent emission is well modeled by a blackbody (kT approx. 1.0 keV) plus power law (Gamma approx. 1.7) with an absorption edge. In the residuals of the combined spectrum, we find a significant absorption line at 6.961 +/- 0.002 keV, consistent with the Fe xxvi (hydrogen-like Fe) 2-1 transition.We place an upper limit on the velocity of a redshifted flow of nu < 221 km/s. We find an equivalent width for the line of 27+2/-3 eV, from which we determine a column density of (7 +/- 1)×10(exp 17) /sq. cm via a curve-of-growth analysis. Using XSTAR simulations, we place a lower limit on the ionization parameter of >103.6 erg cm/s. We discuss what implications the feature has on the system and its geometry. We also present Rossi X-ray Timing Explorer data accumulated during this latest outburst and, via an updated color-color diagram, clearly show that 1A 1744-361 is an "atoll" source

  15. The Fe K Line Region Of η Carinae Around The X-ray Minima

    NASA Astrophysics Data System (ADS)

    Leyder, Jean-Christophe; Corcoran, M. F.; Henley, D. B.; Hamaguchi, K.; Ishibashi, K.; Pittard, J.

    2011-09-01

    We studied the Fe K line region of η Carinae with high-resolution X-ray Chandra grating spectra, using observations covering key phases around the last two X-ray minima (i.e. in 2003.5 and 2009). The line centroids are slightly redshifted, as opposed to the blueshifted lines observed at lower X-ray energies. This is the first observational evidence that the plasma producing the iron line emission is dynamically distinct from the plasma responsible for K-shell emission at lower energies, and is in agreement with the general colliding wind shock model. Gaussian modeling of the Fe XXV K-shell triplet blend shows apparent variations in centroid velocity, which are difficult to interpret as orbital motion of the companion star. Significant variability in the doppler broadening of the Fe K fluorescence emission line at 6.4 keV suggests that the formation of this line occurs in the wind of η Carinae at some particular phases. Of particular interest is the presence of a red wing in the profile of the Fe XXV triplet. This emission probably arises from iron in ionization states below Fe XXIV. Different mechanisms that might explain this emission will be discussed, e.g. an extremely bright, relatively cool, and heavily absorbed equilibrium plasma; emission from unshocked photoionized wind material; or assuming a fraction of the thermal plasma is not in ionization equilibrium.

  16. A Massive X-ray Outflow From The Quasar PDS 456

    NASA Technical Reports Server (NTRS)

    Reeves, J. N.; O'Brien, P. T.; Ward, M. J.

    2003-01-01

    We report on XMM-Newton spectroscopic observations of the luminous, radio-quiet quasar PDS 456. The hard X-ray spectrum of PDS 456 shows a deep absorption trough (constituting 50% of the continuum) at energies above 7 keV in the quasar rest frame, which can be attributed to a series of blue-shifted K-shell absorption edges due to highly ionized iron. The higher resolution soft X-ray grating RGS spectrum exhibits a broad absorption line feature near 1 keV, which can be modeled by a blend of L-shell transitions from highly ionized iron (Fe XVII - XXIV). An extreme outflow velocity of approx. 50000 km/s is required to model the K and L shell iron absorption present in the XMM-Newton data. Overall, a large column density (N(sub H) = 5 x 10(exp 23)/sq cm) of highly ionized gas (log xi = 2.5) is required in PDS 456. A large mass outflow rate of approx. 10 solar mass/year (assuming a conservative outflow covering factor of 0.1 steradian) is derived, which is of the same order as the overall mass accretion rate in PDS 456. This represents a substantial fraction (approx. 10%) of the quasar energy budget, whilst the large column and outflow velocity place PDS 456 towards the extreme end of the broad absorption line quasar population.

  17. Critical early roles for col27a1a and col27a1b in zebrafish notochord morphogenesis, vertebral mineralization and post-embryonic axial growth.

    PubMed

    Christiansen, Helena E; Lang, Michael R; Pace, James M; Parichy, David M

    2009-12-29

    Fibrillar collagens are well known for their links to human diseases, with which all have been associated except for the two most recently identified fibrillar collagens, type XXIV collagen and type XXVII collagen. To assess functions and potential disease phenotypes of type XXVII collagen, we examined its roles in zebrafish embryonic and post-embryonic development. We identified two type XXVII collagen genes in zebrafish, col27a1a and col27a1b. Both col27a1a and col27a1b were expressed in notochord and cartilage in the embryo and early larva. To determine sites of type XXVII collagen function, col27a1a and col27a1b were knocked down using morpholino antisense oligonucleotides. Knockdown of col27a1a singly or in conjunction with col27a1b resulted in curvature of the notochord at early stages and formation of scoliotic curves as well as dysmorphic vertebrae at later stages. These defects were accompanied by abnormal distributions of cells and protein localization in the notochord, as visualized by transmission electron microscopy, as well as delayed vertebral mineralization as detected histologically. Together, our findings indicate a key role for type XXVII collagen in notochord morphogenesis and axial skeletogenesis and suggest a possible human disease phenotype.

  18. The EVE Doppler Sensitivity and Flare Observations

    NASA Technical Reports Server (NTRS)

    Hudson, H. S.; Woods, T. N.; Chamberlin, P. C.; Didkovsky, L.; Del Zanna, G.

    2011-01-01

    The Extreme-ultraviolet Variability Experiment (EVE) obtains continuous EUV spectra of the Sun viewed as a star. Its primary objective is the characterization of solar spectral irradiance, but its sensitivity and stability make it extremely interesting for observations of variability on time scales down to the limit imposed by its basic 10 s sample interval. In this paper we characterize the Doppler sensitivity of the EVE data. We find that the 30.4 nm line of He II has a random Doppler error below 0.001 nm (1 pm, better than 10 km/s as a redshift), with ample stability to detect the orbital motion of its satellite, the Solar Dynamics Observatory (SDO). Solar flares also displace the spectrum, both because of Doppler shifts and because of EVE's optical layout, which (as with a slitless spectrograph) confuses position and wavelength. As a flare develops, the centroid of the line displays variations that reflect Doppler shifts and therefore flare dynamics. For the impulsive phase of the flare SOL2010-06-12, we find the line centroid to have a redshift of 16.8 +/- 5.9 km/s relative to that of the flare gradual phase (statistical errors only). We find also that high-temperature lines, such as Fe XXIV 19.2 nm, have well-determined Doppler components for major flares, with decreasing apparent blueshifts as expected from chromospheric evaporation flows.

  19. Histone deacetylase 8 regulates cortactin deacetylation and contraction in smooth muscle tissues

    PubMed Central

    Li, Jia; Chen, Shu; Cleary, Rachel A.; Wang, Ruping; Gannon, Olivia J.; Seto, Edward

    2014-01-01

    Histone deacetylases (HDACs) are a family of enzymes that mediate nucleosomal histone deacetylation and gene expression. Some members of the HDAC family have also been implicated in nonhistone protein deacetylation, which modulates cell-cycle control, differentiation, and cell migration. However, the role of HDACs in smooth muscle contraction is largely unknown. Here, HDAC8 was localized both in the cytoplasm and the nucleus of mouse and human smooth muscle cells. Knockdown of HDAC8 by lentivirus-encoding HDAC8 shRNA inhibited force development in response to acetylcholine. Treatment of smooth muscle tissues with HDAC8 inhibitor XXIV (OSU-HDAC-44) induced relaxation of precontracted smooth muscle tissues. In addition, cortactin is an actin-regulatory protein that undergoes deacetylation during migration of NIH 3T3 cells. In this study, acetylcholine stimulation induced cortactin deacetylation in mouse and human smooth muscle tissues, as evidenced by immunoblot analysis using antibody against acetylated lysine. Knockdown of HDAC8 by RNAi or treatment with the inhibitor attenuated cortactin deacetylation and actin polymerization without affecting myosin activation. Furthermore, expression of a charge-neutralizing cortactin mutant inhibited contraction and actin dynamics during contractile activation. These results suggest a novel mechanism for the regulation of smooth muscle contraction. In response to contractile stimulation, HDAC8 may mediate cortactin deacetylation, which subsequently promotes actin filament polymerization and smooth muscle contraction. PMID:24920679

  20. Five new triterpene saponins, polygalasaponins XXVIII-XXXII from the root of Polygala japonica Houtt.

    PubMed

    Zhang, D; Miyase, T; Kuroyanagi, M; Umehara, K; Ueno, A

    1996-04-01

    Five new oleanane-type saponins, polygalasaponins XXVIII-XXXII, along with one known saponin, polygalasaponin XXIV, and one known acylated sucrose, tenuifoliside C, were isolated from the root of Polygala japonica. The structures of these new compounds were elucidated as 3-O-beta-D-glucopyranosyl pesenegenin 28-O-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamnopyranosyl (1-->2)-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-beta-D-galactopyranosyl (1-->5)-beta-D-apiofuranosyl (1-->4)-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamno-pyranosyl (1-->2)-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-beta-D-galactopyranosyl (1-->4)-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamnopyranosyl (1-->2)-[4-O-p-methoxycinnamoyl]-[beta-D-glucopyranosyl (1-->3)]-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-alpha-L-arabinopyranosyl (1-->3)-beta-D-xylopyranosyl (1-->4)-[beta-D-apiofuranosyl (1-->3)]-alpha-L-rhamnopyranosyl (1-->2)-[4-O-3,4,5-trimethoxycinnamoyl]-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl persenegenin 28-O-alpha-L-arabinopyranosyl (1-->3)-beta-D-xylopyranosyl (1-->4)-[beta-D-apiofuranosyl (1-->3)-alpha-L-rhamnopyranosyl (1-->2)-[4-O-p-methoxycinnamoyl]-[alpha-L-rhamnopyranosyl (1-->3)-beta-D-fucopyranosyl ester, respectively, on the basis of spectroscopic and chemical evidence.

  1. AUTOMOTIVE DIESEL MAINTENANCE 1. UNIT XXIV, I--MAINTAINING THE FUEL SYSTEM PART III--CATERPILLAR DIESEL ENGINE, II--UNDERSTANDING THE VOLTAGE REGULATOR/ALTERNATOR.

    ERIC Educational Resources Information Center

    Minnesota State Dept. of Education, St. Paul. Div. of Vocational and Technical Education.

    THIS MODULE OF A 30-MODULE COURSE IS DESIGNED TO DEVELOP AN UNDERSTANDING OF THE OPERATION AND MAINTENANCE OF THE DIESEL ENGINE FUEL AND BATTERY CHARGING SYSTEM. TOPICS ARE (1) INJECTION TIMING CONTROLS, (2) GOVERNOR, (3) FUEL SYSTEM MAINTENANCE TIPS, (4) THE CHARGING SYSTEM, (5) REGULATING THE GENERATOR/ALTERNATOR, AND (6) CHARGING SYSTEM SERVICE…

  2. Orthopyroxenes as Recorders of Diogenite Petrogenesis: Nature and Causes of Intragrain Chemical Variability

    NASA Astrophysics Data System (ADS)

    Papike, J. J.; Spilde, M. N.

    1993-07-01

    .g., (100) augite lamellae in an OPX host], and (3) relatively random variability (e.g., exsolution of spinel). Figure 1 (an OPX from Garland) provides evidence for smooth core-to-rim diffusion profiles. Iron and Mn increase while Mg and Cr decrease from core to rim. Also, Al remains relatively constant, Si decreases, and Ti shows an increase, near the grain edge, on the core-to-rim traverse. These chemical systematics were likely caused by a reaction between the cumulate OPX grain and trapped melt. The trapped melt was apparently enriched in Fe and Mn and depleted in Cr relative to OPX. In conclusion, postcrystallization resetting of cumulate grain chemical systematics must be carefully assessed before the data can be "inverted" to estimates of parental melt compositions. Acknowledgment: This research was supported by NASA grant NAGW-3347 and the Institute of Meteoritics. References: [1] Shearer C. K. et al. (1993) LPS XXIV, 1289-1290. [2] Lambert D. D. and Simmons E. C. (1987) Am. J. Sci., 287, 1-32. [3] Takeda H. et. al. (1979) Proc. 3rd Symp. Antarc. Met., 82-108. [4] Papike J. J. et. al. (1993) LPS XXIV, 1109-1110. Fig. 1 appears here in the hard copy.

  3. EUVE observations of Algol: Detection of a continuum and implications for the coronal (Fe/H) abundance

    NASA Technical Reports Server (NTRS)

    Stern, Robert A.; Lemen, James R.; Schmitt, Jurgen H. M. M.; Pye, John P.

    1995-01-01

    We report results from the first extreme ultraviolet spectrum of the prototypical eclipsing binary Algol (beta Per), obtained with the spectrometers on the Extreme Ultraviolet Explorer (EUVE). The Algol spectrum in the 80-350 A range is dominated by emission lines of Fe XVI-XXIV, and the He II 304 A line. The Fe emission is characteristic of high-temperature plasma at temperatures up to at least log T approximately 7.3 K. We have successfully modeled the observed quiescent spectrum using a continuous emission measure distribution with the bulk of the emitting material at log T greater than 6.5. We are able to adequately fit both the coronal lines and continuum data with a cosmic abundance plasma, but only if Algol's quiescent corona is dominated by material at log T greater than 7.5, which is physically ruled out by prior X-ray observations of the quiescent Algol spectrum. Since the coronal (Fe/H) abundance is the principal determinant of the line-to-continuum ratio in the EUV, allowing the abundance to be a free parameter results in models with a range of best-fit abundances approximately = 15%-40% of solar photospheric (Fe/H). Since Algol's photospheric (Fe/H) appears to be near-solar, the anomalous EUV line-to-continuum ratio could either be the result of element segregation in the coronal formation process, or other, less likely mechanisms that may enhance the continuum with respect to the lines.

  4. Representation and transformation of Langley's map of the infrared solar spectrum

    NASA Astrophysics Data System (ADS)

    Loettgers, Andrea

    In 1900, after 18 years of research, the American astrophysicist Samuel Pierpont Langley published the final report of his investigations in the infrared region of the solar spectrum. (See Samuel P. Langley: Annals of the Astrophysical Observatory of the Smithsonian Institution, Vol. 1, Washington: Goverment Printing Office, 1900.) In this report one finds three different types of maps of the infrared region, extending from 1.1 mu-m to 5.3 mu-m and showing the positions of 750 absorption lines: a bolograph, a line spectrum and a normal spectrum. (The bolograph, the line spectrum and the normal spectrum are accessible as pl. XX and XXIV at http://adsbit.harvard.edu/books/saoann/.) Looking at these three distinct forms of representation raises the questions: Why did Langley decide to use three representations for the visualization of his results? How are these distinct representations connected? An analysis of the first question will provide further insight into the ``connection between instruments, practices, and the visual'', into the recording, evaluation and processing of the data and, furthermore, into the historical and disciplinary contexts. The prevailing trend toward the automation of measuring and registration processes, and the associated claim of `mechanical objectivity', together with standards concerning precision and completeness set by Henry Rowland's photographic measurements in the visible part of the spectrum, turn out to be the strongest elements in the development of the different forms of representation and their respective transformations.

  5. Orthopyroxenes as Recorders of Diogenite Petrogenesis: Al-Cr-Ti Systematics

    NASA Astrophysics Data System (ADS)

    Fowler, G. W.; Papike, J. J.; Spilde, M. N.; Shearer, C. K.

    1993-07-01

    A77256, which accounts for its data plotting below the main trend. It should be noted that the main trend and the ALH A77256 trend have less scatter near the bottom of the data arrays than near the top. In fact, lines drawn through the bottom of the arrays project through the origin. Some of the reason for the scatter, other than subsolidus annealing effects [3], may be the result of different Ti^3+/Ti^4+ ratios in OPX resulting from variable fO2 environments. A possible charge balance equation, for other then quadrilateral components is: ^VITi^3++2^VITi^4++^VICr^3++^VIAl^3+=^IVAl (Na is so low it can be ignored). The cores of most OPX grains probably still retain their igneous signatures; therefore, the high Al, Cr, Ti end of the main trend likely reflects melt compositions enriched in these elements. Acknowledgment. This research was supported by NASA Grant NAGW- 3347 and the Institute of Meteoritics. References. [1] Papike J. J. et. al. (1993) LPS XXIV, 1109-1110. [2] Shearer C. K. et al. (1993) LPS XXIV, 1289-1290. [3] Papike J. J. and Spilde M. N. (1993) This volume. Fig. 1, which appears here in the hard copy, shows Al vs. Ti atoms per formula unit. Fig. 2, which appears here in the hard copy, shows Ti + Cr vs. Al in atoms per formula unit.

  6. Stable Nickel Isotopes in Fusion Crusts from Iron Meteorites and from Metallic Particles in a Black Wabar Impact Glass

    NASA Astrophysics Data System (ADS)

    Xue, S.; Herzog, G. F.; Hall, G. S.

    1993-07-01

    from the incoming meteorite (see [4]). Horz et al. [6] found variable Fe/Ni ratios (from 0.1 to 222) in black melt glasses associated with the Wabar impact. The Fe/Ni ratio in our metal sample is 2, which is considerably lower than that in the bulk meteorite (~12.4). Several lines of evidence suggest that vapor fractionation is to be expected in samples that have Fe/Ni ratios greater than those in the bulk impactor [2-6]. Thus it is not surprising that our first results for Wabar impactites show no Ni isotopic fractionation. Isotopic analyses of Wabar impactites with high Fe/Ni ratios should be made to test the importance of vapor fractionation. References: [1] Herzog G. F. et al. (1992) LPSC XXIII, 527-528. [2] Xue S. et al. (1993) LPSC XXIV, 1547-1548. [3] Davis A. et al. (1993) LPSC XXIV, 373- 374. [4] Mittlefehldt D. W. et al. (1992) Meteoritics, 27, 361-370. [5] Clayton R. N. et al. (1986) EPSL, 79, 235-240. [6] Horz F. et al. (1989) Proc. LPSC 19th, 697-710. Table 1, which appears in the hard copy, shows delta (permil) and average isotope fractionation PHI (%/amu) for Ni isotopes in iron meteorites and black Wabar impact glass.

  7. Chemistry of vinylidene complexes. XXIV. A new μ-vinylidene complex containing RePt core, and platinum-bound carbonyl ligand. Spectroscopic, structural and electrochemical study

    NASA Astrophysics Data System (ADS)

    Verpekin, Victor V.; Vasiliev, Alexander D.; Kondrasenko, Alexander A.; Burmakina, Galina V.; Chudin, Oleg S.; Pavlenko, Nina I.; Zimonin, Dmitry V.; Rubaylo, Anatoly I.

    2018-07-01

    The novel heterobinuclear μ-vinylidene complex [Cp(CO)2Re(μ-C=CHPh)Pt(PPh3)(CO)] (1) was isolated from the reaction mixture of [Cp(CO)2Re(μ-C=CHPh)Fe(CO)4] and Pt(PPh3)4 for the first time. Alternative high-yield synthetic approaches to 1 were developed including the reactions of [Cp(CO)2Re(μ-C=CHPh)Pt(PPh3)2] (2) with Co2(CO)8 and Rh(acac)(CO)2. The complex was characterized by IR and 1H, 13C and 31P NMR spectroscopy, a molecular structure of 1 was determined by X-ray diffraction analysis. The electrochemical behavior of the new complex was studied by cyclic voltammetry at platinum or glassed carbon electrodes and by dc polarography at a dropping mercury electrode.

  8. Chandra X-ray spectroscopy of focused wind in the Cygnus X-1 system: II. The non-dip spectrum in the low/hard state – modulations with orbital phase

    DOE PAGES

    Miskovicova, Ivica; Hell, Natalie; Hanke, Manfred; ...

    2016-05-25

    Accretion onto the black hole in the system HDE 226868/Cygnus X-1 is powered by the strong line-driven stellar wind of the O-type donor star. We study the X-ray properties of the stellar wind in the hard state of Cyg X-1, as determined using data from the Chandra High Energy Transmission Gratings. Large density and temperature inhomogeneities are present in the wind, with a fraction of the wind consisting of clumps of matter with higher density and lower temperature embedded in a photoionized gas. Absorption dips observed in the light curve are believed to be caused by these clumps. This workmore » concentrates on the non-dip spectra as a function of orbital phase. The spectra show lines of H-like and He-like ions of S, Si, Na, Mg, Al, and highly ionized Fe (Fe xvii–Fe xxiv). We measure velocity shifts, column densities, and thermal broadening of the line series. The excellent quality of these five observations allows us to investigate the orbital phase-dependence of these parameters. We show that the absorber is located close to the black hole. Doppler shifted lines point at a complex wind structure in this region, while emission lines seen in some observations are from a denser medium than the absorber. Here, the observed line profiles are phase-dependent. Their shapes vary from pure, symmetric absorption at the superior conjunction to P Cygni profiles at the inferior conjunction of the black hole.« less

  9. Formulation and evaluation of antihyperglycemic leaf extracts of Zizyphus spina-christi (L.) Willd.

    PubMed

    Nesseem, D I; Michel, C G; Sleem, A A; El-Alfy, T S

    2009-02-01

    This study deals with the formulation of antihyperglycemic leaf extracts of Zizyphus spina-christi (L.) Willd. A bioactivity guided fractionation of different leaf extracts [defatted ethanol 70% (a), butanol (b), ethanol 70% (c), ethyl acetate (d) and petroleum ether (e) extracts] revealed that extract (c) possessed the highest antihyperglycemic activity followed by (b) and (a). HPLC was adopted for standardization of the extract (c) based on evaluation of the major saponin christinin-A which was used as marker. The detection limit was 9.45 mg/ml for Christinin-A. Extracts (a), (b) and (c) were separately formulated in soft (S) and hard (H) gelatin capsules. Two different formulations (F1 and F2) were tried using different excipients suitable for oral drug delivery. Formula 1, used for soft gelatin capsules [(F1) Sa, Sb, Sc] Formula 2, used for hard gelatin capsules [(F2) - Ha, Hb, Hc]. The recovery rates of the samples of saponin were in the range 99.43-101.86% at 200, 800 microg/ml and 1200 microg/ml. Saponin release rates from different formulae were carried out using dissolution tester USP XXIV. The highest release was obtained from formulation Sc. The release of the extracts followed diffusion mechanism. The selected formula Sc exhibited highest anti-diabetic activity (P < 0.01) on acute and long-term administration and highest saponin release. This formula (Sc) contained poly-oxyethylene (20) cetyl ether (BC-20TX), PEG 400, PEG 6000, purified water, meglyol 810, ascorbic acid and 200 mg of extract (c).

  10. The quiescent and flaring EUV spectrum of Algol and its relationship to other active coronae. EUV spectroscopy of bright hyades coronae: 71 Tauri and Theta 1 Tauri

    NASA Technical Reports Server (NTRS)

    Stern, Robert A.

    1994-01-01

    This program involves analysis and interpretation of EUVE spectrometer observations of the active stars Algol (beta Per) and 71 Tauri. The EUVE satellite spectrometers observed the prototype eclipsing binary Algol over nearly 1.5 orbital periods. Effective exposure times were 100 ksec and 89 ksec in the short wave (70-180 A) and medium wave (140-370 A) channels. High temperature (up to 20 MK) Fe XVI-XXIV emission lines are clearly detected in the overall spectrum. In addition, a quiescent continuum is present which increases towards shorter wavelengths. Using synthesized spectra of optically thin line and continuum emission folded through the instrumental response, we have examined constraints on the (Fe/H) coronal abundance in Algol. We find that the coronal Fe is underabundant by factors that approximately equal 2-4 relative to solar photospheric values, unless an unreasonably large quantity of coronal plasma at T greater than 30 MK is present in the quiescent spectrum. The latter possibility is, however, inconsistent with available X-ray data. Lightcurves of the high temperature EUV lines compared to line emission at He II 304 A show considerable differences, with much deeper minima present in the He II line during both primary and secondary eclipses. Toward the end of the observation a moderate flare lasting approximately 6 hours was detected in the high temperature Fe emission lines. The 71 Tau observation, for about the same exposure time, revealed only a handful of weak emission lines; however, the strongest lines were also those of Fe XXIII/XX, suggesting a hot coronal plasma. No obvious flaring or other variation was present in the 71 Tau Deep Survey lightcurve.

  11. Observations of quasi-periodic phenomena associated with a large blowout solar jet

    NASA Astrophysics Data System (ADS)

    Morton, R. J.; Srivastava, A. K.; Erdélyi, R.

    2012-06-01

    Aims: A variety of periodic phenomena have been observed in conjunction with large solar jets. We aim to find further evidence for (quasi-)periodic behaviour in solar jets and determine what the periodic behaviour can tell us about the excitation mechanism and formation process of the large solar jet. Methods: Using the 304 Å (He-II), 171 Å (Fe IX), 193 Å (Fe XII/XXIV) and 131 Å (Fe VIII/XXI) filters onboard the Solar Dynamic Observatory (SDO) Atmospheric Imaging Assembly (AIA), we investigate the intensity oscillations associated with a solar jet. Results: Evidence is provided for multiple magnetic reconnection events occurring between a pre-twisted, closed field and open field lines. Components of the jet are seen in multiple SDO/AIA filters covering a wide range of temperatures, suggesting the jet can be classified as a blowout jet. Two bright, elongated features are observed to be co-spatial with the large jet, appearing at the jet's footpoints. Investigation of these features reveal they are defined by multiple plasma ejections. The ejecta display (quasi-)periodic behaviour on timescales of 50 s and have rise velocities of 40-150 km s-1 along the open field lines. Due to the suggestion that the large jet is reconnection-driven and the observed properties of the ejecta, we further propose that these ejecta events are similar to type-II spicules. The bright features also display (quasi)-periodic intensity perturbations on the timescale of 300 s. Possible explanations for the existence of the (quasi-)periodic perturbations in terms of jet dynamics and the response of the transition region are discussed. Movies are available in electronic form at http://www.aanda.org

  12. Slipping magnetic reconnection during an X-class solar flare observed by SDO/AIA

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Dudík, J.; Del Zanna, G.; Mason, H. E.

    2014-04-01

    We present SDO/AIA observations of an eruptive X-class flare of 2012 July 12, and compare its evolution with the predictions of a three-dimensional (3D) numerical simulation. We focus on the dynamics of flare loops that are seen to undergo slipping reconnection during the flare. In the Atmospheric Imaging Assembly (AIA) 131 Å observations, lower parts of 10 MK flare loops exhibit an apparent motion with velocities of several tens of km s{sup –1} along the developing flare ribbons. In the early stages of the flare, flare ribbons consist of compact, localized bright transition-region emission from the footpoints of the flaremore » loops. A differential emission measure analysis shows that the flare loops have temperatures up to the formation of Fe XXIV. A series of very long, S-shaped loops erupt, leading to a coronal mass ejection observed by STEREO. The observed dynamics are compared with the evolution of magnetic structures in the 'standard solar flare model in 3D.' This model matches the observations well, reproducing the apparently slipping flare loops, S-shaped erupting loops, and the evolution of flare ribbons. All of these processes are explained via 3D reconnection mechanisms resulting from the expansion of a torus-unstable flux rope. The AIA observations and the numerical model are complemented by radio observations showing a noise storm in the metric range. Dm-drifting pulsation structures occurring during the eruption indicate plasmoid ejection and enhancement of the reconnection rate. The bursty nature of radio emission shows that the slipping reconnection is still intermittent, although it is observed to persist for more than an hour.« less

  13. Carbon and Nitrogen Chemistry of Lodranites: Relationship to Acapulco?

    NASA Astrophysics Data System (ADS)

    Grady, M. M.; Franchi, I. A.; Pillinger, C. T.

    1993-07-01

    , if present. Analysis of whole-rock Lodran yielded 17.0 ppm nitrogen, with delta^15N ca. +4 per mil. A prominent release of nitrogen occurred between 650 degrees C and 900 degrees C, 50% of the total, with delta^15N varying between ca. +3 per mil and +9 per mil. Lodran is very different from Acapulco in both its carbon and nitrogen chemistry. There is little evidence for the presence of graphite in the former meteorite and it does not appear to contain the component of isotopically light nitrogen that is so abundant in Acapulco. However, Lodran does manifest a nitrogen- bearing component with intermediate isotopic composition, the location of which, in the metal or silicate portion of the meteorite is, as yet, unknown. Since Lodran has apparently experienced an elevated temperature regime compared with Acapulco, it might be possible that nitrogen has been remobilized and mixed in the former meteorite, leading to erasure of the characteristic isotopically light signature. Lodran has a higher whole-rock nitrogen abundance than Acapulco, thus it is unlikely that the presence of heavier nitrogen in Lodran is simply a result of fractionation of a reservoir during open system heating. References: [1] McCoy T. J. et al. (1993) LPS XXIV, 945-946. [2] Clayton R. N. et al. (1992) LPS XXIII, 231-232. [3] Bogard D. D. et al. (1993) LPS XXIV, 141-142. [4] Sturgeon G. and Marti K. (1990) LPS XXI, 1220-1221. [5] Becker R. H. (1991) LPS XXII, 69- 70. [6] Grady M. M. and Pillinger C. T. (1986) GCA, 50, 255-263, [7] Palme H. et al. (1981) GCA, 45, 727-752. [8] Kim Y. et al. (1992) LPS XXIII, 691-692.

  14. Modeling Solar Atmospheric Phenomena with AtomDB and PyAtomDB

    NASA Astrophysics Data System (ADS)

    Dupont, Marcus; Foster, Adam

    2018-01-01

    Taking advantage of the modeling tools made available by PyAtomDB (Foster 2015), we evaluated the impact of changing atomic data on solar phenomena, in particular their effects on models of coronal mass ejections (CME). Intitially, we perform modifications to the canonical SunNEI code (Murphy et al. 2011) in order to include non-equilibrium ionization (NEI) processes that occur in the CME modeled in SunNEI. The methods used involve the consideration of radiaitive cooling as well as ion balance calculations. These calculations were subsequently implemented within the SunNEI simulation. The insertion of aforementioned processes and parameter customizaton produced quite similar results of the original except for the case of iron. These differences were traced to inconsistencies in the recombination rates for Argon-like iron ions between the CHIANTI and AtomDB databases, even though they in theory use the same data. The key finding was that theoretical models are greatly impacted by the relative atomic database update cycles.Following the SunNEI comparison, we then use the AtomDB database to model the time depedencies of intensity flux spikes produced by a coronal shock wave (Ma et al. 2011). We produced a theretical representation for an ionizing plasma that interpolated over the intensity in four Astronomical Imaging Assembly (AIA) filters. Specifically, the 171 A (Fe IX) ,193 A (Fe XII, FeXXIV),211 A (Fe XIV),and 335 A (Fe XVI) wavelengths in order to assess the comparative spectral emissions between AtomDB and the observed data. The results of the theoretical model, in principle, shine light on both the equilibrium conditions before the shock and the non-equilibrium response to the shock front, as well as discrepancies introduced by changing the atomic data.

  15. The infauna of three widely distributed sponge species (Hexactinellida and Demospongiae) from the deep Ekström Shelf in the Weddell Sea, Antarctica

    NASA Astrophysics Data System (ADS)

    Kersken, Daniel; Göcke, Christian; Brandt, Angelika; Lejzerowicz, Franck; Schwabe, Enrico; Anna Seefeldt, Meike; Veit-Köhler, Gritta; Janussen, Dorte

    2014-10-01

    Due to their high abundance and large body size sponges have a central position in Antarctic zoobenthos, where they form the most extensive sponge grounds of the world. Though research on Antarctic benthos communities is quite established, research on sponge-associated infauna communities is scarce. We analyzed associated infauna of fifteen individuals of the sponge species Mycale (Oxymycale) acerata Kirkpatrick, 1907 (Demospongiae: Mycalina), Rossella antarctica Carter, 1872 and R. racovitzae Topsent, 1901 (both Hexactinellida: Lyssacinosida). Samples were collected from the deep Ekström Shelf at 602 m in the South-Eastern Weddell Sea, Antarctica, during the ANT XXIV-2 (SYSTCO I) expedition of RV Polarstern. The number of species, α- and β-diversity and the significantly different species composition of infauna communities related to sponge species were calculated, the latter via cluster analysis. The sponge-associated infauna consisted of five phyla: Foraminifera, Nematoda, Polychaeta, Mollusca and Arthropoda. In total 11,463 infaunal specimens were extracted and we found at least 76 associated species. Highest values of α-diversity were calculated for a sample of R. antarctica with a Shannon-Index of 1.84 and Simpson-Index of 0.72 respectively. Our results of the cluster-analysis show significant differences between infauna communities and a unique species composition for single sponge species. Polychaetes of the genus Syllis Lamarck, 1818 were numerous in M. acerata and genera like Pionosyllis Malmgren, 1867 and Cirratulus Lamarck, 1801 were numerous in R. antarctica. Individuals of the amphipod species Seba cf. dubia Schellenberg, 1926 were often found in R. antarctica and R. racovitzae while Colomastix fissilingua Schellenberg, 1926 was frequent in samples of M. acerata. Molluscs were present in M. acerata and R. antarctica but absent in R. racovitzae.

  16. Crustal structure of the Boreas Basin formed at ultraslow spreading Knipovich Ridge - Northern North Atlantic

    NASA Astrophysics Data System (ADS)

    Hermann, T.; Jokat, W.

    2012-04-01

    The Boreas Basin is located in Norwegian Greenland Sea bordered by the Greenland Fracture Zone in the south and the Hovgard Ridge in the north, respectively. In the east it adjoins the ultraslow mid-ocean Knipovich Ridge. Previous seismic reflection studies in the Boreas Basin have shown that the basement topography has a roughness, which is typical for ultraslow spreading ridges. This observation supports assumptions that the basin was formed at ultraslow spreading rates during its entire geological history. However, the detailed crustal structure remained unresolved. In summer 2009 new seismic refraction data were acquired in the Boreas Basin during the expedition ARK-XXIV/3 with the research vessel Polarstern. The deep seismic sounding line has a length of 340 km. Forward modelling of the data of 18 ocean bottom seismometers deployed along the NW-SE trending profile reveal an unusual 3.2 km thin oceanic crust. The crustal model is further constrained by S-wave and 2D gravity modelling. The P-wave velocity model shows a layered oceanic crust without oceanic layer 3 and with velocities less than 6.3 km/s except beneath a nearly 2000 m high seamount. Beneath the seamount velocities of up to 6.7 km/s were observed. The mantle velocities range between 7.5 km/s in the uppermost mantle and 8.0 km/s in almost 15 km depth. A serpentinisation of approximately 13% in the uppermost mantle decreasing downwards can explain the low mantle velocities. In summary, the transect confirms earlier models that the entire Boreas Basin was formed at ultraslow spreading rates. Indications for this are the basement roughness and the overall thin oceanic crust. Both observations are typical for ultraslow spreading systems.

  17. Global topics and novel approaches in the study of air pollution, climate change and forest ecosystems.

    PubMed

    Sicard, Pierre; Augustaitis, Algirdas; Belyazid, Salim; Calfapietra, Carlo; de Marco, Alessandra; Fenn, Mark; Bytnerowicz, Andrzej; Grulke, Nancy; He, Shang; Matyssek, Rainer; Serengil, Yusuf; Wieser, Gerhard; Paoletti, Elena

    2016-06-01

    stomatal O3 flux parameterizations for risk assessment, especially, in under-investigated regions; (xxii) Defining biologically based O3 standards for protection thresholds and critical levels; (xxiii) Use of free-air exposure facilities; (xxiv) Assessing O3 impacts on forest ecosystem services. Copyright © 2016 Elsevier Ltd. All rights reserved.

  18. Testing the Prediction of Iron Alteration Minerals on Low Albedo Asteroids

    NASA Technical Reports Server (NTRS)

    Jarvis, K. S.; Vilas, Faith; Howell, E.; Kelley, M.; Cochran, A.

    1999-01-01

    Absorption features centered near 0.60 - 0.65 and 0.80 - 0.90 micron were identified in the spectra of three low-albedo main-belt (165, 368, 877) and two low-albedo outer-belt (225, 334) asteroids (Vilas et al., Icarus, v. 109,274,1994). The absorption features were attributed to charge transfer transitions in iron alteration minerals such as goethite, hematite, and jarosite, all products of aqueous alteration. Concurrently, Jarvis et al. (LPSC XXIV, 715, 1993) presented additional spectra of low-albedo asteroids that had absorption features centered near 0.60 - 0.65 micron without the longer wavelength feature. Since these two features in iron oxides originate from the same ground state, and the longer wavelength feature requires less energy to exist, the single shorter wavelength feature cannot be caused by the iron alteration minerals. In addition, spectra of minerals such as hematite and goethite show a rapid increase in reflectance beginning near 0.5 micron absent in the low-albedo asteroid spectra. The absence of this rise has been attributed to its suppresion from opaques in the surface material. Spectra on more than one night were available for only one of these five asteroids, 225 Henrietta, and showed good repeatability of the 0.65-micron feature. We have acquired additional spectra of all five asteroids in order to test the repeatability of the 0.65-micron feature, and the presence and repeatability of the features centered near 0.8 - 0.9 micron. We specifically will test the possibility that longer wavelength features could be caused by incomplete removal of telluric water. Asteroid 877 Walkure is a member of the Nysa-Hertha family, and will be compared to spectra of other members of that family. Data were acquired in 1996 and 1999 on the 2.1-m telescope with a facility cassegrain spectrograph, McDonald Observatory, Univ. Of Texas, and the 1.5-m telescope with facility cassegrain spectrograph at CTIO. This research is supported by the NASA Planetary

  19. Simultaneous ASCA and EUVE Observations of Capella

    NASA Astrophysics Data System (ADS)

    Brickhouse, N. S.; Dupree, A. K.; Edgar, R. J.; Drake, S. A.; White, N. E.; Liedahl, D. A.; Singh, K. P.

    1997-05-01

    We present simultaneous observations taken in Mar 1996 of the bright stellar coronal source Capella (HD 34029) with the ASCA and EUVE satellites. Previous EUVE observations of Fe emission lines (Fe VIII --- XXIV, excluding XVII) revealed a narrow emission measure feature at 6 x 10(6) K, which has proven to be remarkably stable over several years (flux from Fe XVIII and XIX has not varied by more than 30%), while lines formed at higher temperatures have shown intensity variations up to factors of 4. Furthermore, extremely high signal-to-noise spectra obtained by summing all EUVE measurements show that the Fe/H abundance ratio is consistent with solar photospheric. (See Dupree et al. 1993, ApJ, 418, L41; Brickhouse, Raymond, & Smith 1995, ApJSupp, 97, 551; Brickhouse 1996, IAU Coll. 152, Astrophysics in the Extreme Ultraviolet, Bowyer & Malina, eds (Kluwer), 141.) Meanwhile, the ASCA data of Capella have proven notoriously difficult to analyze. The performance verification (PV) phase data suggested a somewhat subsolar Fe abundance, but models were in poor agreement with the data (chi (2red) ~ 6). (See Drake 1996, Conf. on Cosmic Abundances, U. Maryland). Since the emission lines observed by EUVE are formed at the same emitting temperatures as the X-ray spectrum (Capella is ``soft'' such that very little flux is observed above 2 keV), the emission measure distribution derived from EUVE lines should provide a direct prediction of the X-ray spectrum, with only the relative abundances of species other than Fe as free parameters. Like the PV data, the new ASCA spectrum is not well fit by any of the standard models. Applying the constraints imposed by EUVE does not make a major improvement in the fit --- multi-thermal, variable abundance models such as Raymond-Smith and MEKAL do not provide any acceptable fit (chi (2red) > 5). We discuss our efforts to understand the X-ray spectrum, including studies of the uncertainties in the atomic data and of the underlying assumptions

  20. Petrology and Geochemistry of LEW 88663 and PAT 91501: High Petrologic L Chondrites

    NASA Astrophysics Data System (ADS)

    Mittlefehldt, D. W.; Lindstrom, M. M.; Field, S. W.

    1993-07-01

    composition of PAT 91501 in order to investigate this further. Orthopyroxenes in LEW 88663 have a lower Wo content, and clinopyroxenes have a higher Wo content, than those in PAT 91501, and have equilibrated to lower temperatures, perhaps ~1000 degrees C [5]. References: [1] Wasson and Kallemeyn (1988) Phil. Trans. R. Soc. Lond., A325, 535. [2] Davis et al. (1993) LPS XXIV, 375. [3] Taylor et al. (1979) GCA, 43, 323. [4] Fodor and Keil (1975) Meteoritics, 10, 325. [5] Lindsley (1983) Am. Mineral., 68, 477. [6] Jurewicz et al. (1993) LPS XXIV, 739.

  1. Tabulation of comet observations.

    NASA Astrophysics Data System (ADS)

    1991-07-01

    Concerning comets: 1957 III Arend-Roland, 1957 V Mrkos, 1958 III Burnham, 1959 III Bester-Hoffmeister, 1959 VI Alcock, 1959 VIII P/Giacobini-Zinner, 1960 I P/Wild 1, 1960 II Burnham, 1960 III P/Schaumasse, 1960 VIII P/Finlay, 1961 V Wilson-Hubbard, 1961 VIII Seki, 1962 III Seki-Lines, 1962 VIII Humason, 1963 I Ikeya, 1963 III Alcock, 1963 V Pereyra, 1964 VI Tomita-Gerber-Honda, 1964 VIII Ikeya, 1964 IX Everhart, 1979 X Bradfield, 1980 X P/Stephan-Oterma, 1980 XII Meier, 1980 XIII P/Tuttle, 1981 II Panther, 1982 I Bowell, 1982 IV P/Grigg-Skjellerup, 1982 VII P/d'Arrest, 1986 III P/Halley, 1987 IV Shoemaker, 1987 XII P/Hartley 3, 1987 XIX P/Schwassmann-Wachmann 2, 1987 XXIX Bradfield, 1987 XXX Levy, 1987 XXXII McNaught, 1987 XXXIII P/Borrelly, 1987 XXXVI P/Parker-Hartley, 1987 XXXVII P/Helin- Roman-Alu 1, 1988 III Shoemaker-Holt, 1988 V Liller, 1988 VIII P/Ge-Wang, 1988 XI P/Shoemaker-Holt 2, 1988 XIV P/Tempel 2, 1988 XV Machholz, 1988 XX Yanaka, 1988 XXI Shoemaker, 1988 XXIV Yanaka, 1989 III Shoemaker, 1989 V Shoemaker-Holt-Rodriquez, 1989 VIII P/Pons-Winnecke, 1989 X P/Brorsen-Metcalf, 1989 XI P/Gunn, 1989 XIII P/Lovas 1, 1989 XVIII McKenzie-Russell, 1989 XIX Okazaki-Levy-Rudenko, 1989 XX P/Clark, 1989 XXI Helin-Ronan-Alu, 1989 XXII Aarseth-Brewington, 1989h P/Van Biesbroeck, 1989t P/Wild 2, 1989u P/Kearns-Kwee, 1989c1 Austin, 1989e1 Skorichenko-George, 1990a P/Wild 4, 1990b Černis-Kiuchi-Nakamura, 1990c Levy, 1990e P/Wolf-Harrington, 1990f P/Honda-Mrkos-Pajdušáková, 1990g McNaught-Hughes, 1990i Tsuchiya-Kiuchi, 1990n P/Taylor, 1990ο P/Shoemaker-Levy 1, 1991a P/Metcalf-Brewington, 1991b Arai, 1991c P/Swift-Gehrels, 1991d Shoemaker-Levy, 1991e P/Shoemaker-Levy 3, 1991h P/Takamizawa, 1991j P/Hartley 1, 1991k P/Mrkos, 1991l Helin-Lawrence, 1991n P/Faye, 1991q P/Levy, 1991t P/Hartley 2, P/Encke, P/Schwassmann-Wachmann 1.

  2. DOE Office of Scientific and Technical Information (OSTI.GOV)

    Conn, A. R.; Parker, Q. A.; Zucker, D. B.

    In 'A Bayesian Approach to Locating the Red Giant Branch Tip Magnitude (Part I)', a new technique was introduced for obtaining distances using the tip of the red giant branch (TRGB) standard candle. Here we describe a useful complement to the technique with the potential to further reduce the uncertainty in our distance measurements by incorporating a matched-filter weighting scheme into the model likelihood calculations. In this scheme, stars are weighted according to their probability of being true object members. We then re-test our modified algorithm using random-realization artificial data to verify the validity of the generated posterior probability distributionsmore » (PPDs) and proceed to apply the algorithm to the satellite system of M31, culminating in a three-dimensional view of the system. Further to the distributions thus obtained, we apply a satellite-specific prior on the satellite distances to weight the resulting distance posterior distributions, based on the halo density profile. Thus in a single publication, using a single method, a comprehensive coverage of the distances to the companion galaxies of M31 is presented, encompassing the dwarf spheroidals Andromedas I-III, V, IX-XXVII, and XXX along with NGC 147, NGC 185, M33, and M31 itself. Of these, the distances to Andromedas XXIV-XXVII and Andromeda XXX have never before been derived using the TRGB. Object distances are determined from high-resolution tip magnitude posterior distributions generated using the Markov Chain Monte Carlo technique and associated sampling of these distributions to take into account uncertainties in foreground extinction and the absolute magnitude of the TRGB as well as photometric errors. The distance PPDs obtained for each object both with and without the aforementioned prior are made available to the reader in tabular form. The large object coverage takes advantage of the unprecedented size and photometric depth of the Pan-Andromeda Archaeological Survey. Finally

  3. Analyses of genetic diversity of bacterial blight pathogen, Xanthomonas oryzae pv. oryzae using IS1112 in Bangladesh.

    PubMed

    Islam, Md Rashidul; Alam, Md Samiul; Khan, Ashik Iqbal; Hossain, Ismail; Adam, Lorne R; Daayf, Fouad

    2016-01-01

    Bacterial blight (BB) is caused by Xanthomonas oryzae pv. oryzae (Xoo), a most destructive disease of rice, mostly in Asia, including Bangladesh. Altogether 96 isolates of Xoo were collected from 19 rice-growing districts of Bangladesh in both the rain-fed and irrigated seasons of 2014 to assess their pathotypic and genetic variation. Pathotypic analyses were carried out on a set of 12 Near Isogenic Lines (NILs) of rice containing a single resistance gene and two check varieties IR24 and TN1 by the leaf clipping inoculation method. A total of 24 pathotypes were identified based on their virulence patterns on the NILs tested. Among these, pathotypes VII, XII and XIV, considered as major, containing a maximum number of isolates (9.38% each), are frequently distributed in seven northern to mid-eastern districts of Bangladesh. The most virulent pathotype I was recorded in the Habiganj and Brahmanbaria districts. The molecular analysis of variability among the isolates was carried out through PCR analysis using multi-locus primers Jel1 and Jel2 (based on the repetitive element IS1112 in the Xoo genome). Using the genotypic data, a dendrogram was constructed with 17 clusters along with 17 molecular haplotypes at the 65% similarity index. Cluster I was composed of 46 isolates considered as major, whereas clusters X, XI, XII and XVII were represented by a single isolate. A phenogram was constructed based on virulence to interpret the relationship between the pathotypes and the molecular haplotypes. At the 50% similarity level, among 10 clusters, cluster I, considered as major, consisted of a maximum of 10 pathotypes out of 24. In case of haplotypes, a maximum of 7 haplotypes were obtained from pathotype XII, whereas pathotypes IX, X, XV, XXII and XXIV were represented by a single haplotype. However, the present study revealed that different isolates belonging to the same pathotypes belonged to different haplotypes. Conversely, genetically similar haplotypes were also

  4. The WIYN Open Cluster Study: A 15-Year Report

    NASA Astrophysics Data System (ADS)

    Mathieu, Robert D.; WOCS Collaboration

    2013-06-01

    The WIYN 3.5m telescope combines large aperture, wide field of view and superb image quality. The WIYN consortium includes investigators in numerous areas of open cluster research. The combination spawned the WIYN Open Cluster Study (WOCS) over a decade ago, with the goals of producing 1) comprehensive photometric, astrometric and spectroscopic data for new fundamental open clusters and 2) addressing key astrophysical problems with these data. The set of core WOCS open clusters spans age and metallicity. Low reddening, solar proximity and richness were also desirable features in selecting core open clusters. More than 50 WIYN Open Cluster Study papers have been published in refereed journals. Highlights include: deep and wide-field photometry of NGC 188, NGC 2168 (M35), and NGC 6819 (WOCS I, II, XI and LII); deep and wide-field proper-motion studies of the old open clusters NGC 188, NGC 2682 (M67) and NGC 6791 (WOCS XVII, XXXIII and XLVI); comprehensive radial-velocity surveys of NGC 188, NGC 2168 and NGC 6819 (WOCS XXXII, XXIV, and XXXVIII); metallicity and lithium abundances in NGC 2168 (WOCS V); comprehensive definition of the hard-binary populations of NGC 188 and NGC 2168 (WOCS XXII and XLVIII); rotation period distributions in NGC 1039 (M34) and NGC 2168 (WOCS XXXV, XLIII, and XLV); study of chromospheric activity in NGC 2682 (WOCS XVIII); photometric variability surveys in NGC 188 and NGC 2682 (IX and XV); new Bayesian techniques for determination of cluster parameters (WOCS XXIII); a new infrared age-diagnostic for open clusters (WOCS XL); theoretical studies of stellar rotation (WOCS XIII and XIV); sophisticated N-body simulations of NGC 188 (WOCS LI); and the discovery of a high binary frequency and white dwarf companions among NGC 188 blue stragglers. While the WIYN 3.5m telescope remains at its heart, today the WIYN Open Cluster Study collaboration extends beyond both the WIYN observatory and consortium, and continues as a vital and productive

  5. The rebirth of Supernova 1987A : a study of the ejecta-ring collision

    NASA Astrophysics Data System (ADS)

    Gröningsson, Per

    high-ionization line profiles (Fe X-XIV) initially show larger spectral widths, which indicates that at least a fraction of the emission comes from non-radiative shocks.

  6. Tabulation of comet observations.

    NASA Astrophysics Data System (ADS)

    1993-10-01

    Concerning comets: 1955 III Mrkos, 1955 IV Bakharev-Macfarlane-Krienke, 1955 V Honda, 1956 III Mrkos, 1956 IV P/Olbers, 1957 III Arend-Roland, 1957 V Mrkos, 1958 III Burnham, 1959 VIII P/Giacobini-Zinner, 1960 II Burnham, 1973 XII Kohoutek, 1974 III Bradfield, 1975 IX Kobayashi-Berger-Milon, 1975 X Suzuki-Saigusa-Mori, 1975 XI Bradfield, 1975 XII Mori-Sato-Fujikawa, 1976 IV Bradfield, 1976 VI West, 1979 VII Bradfield, 1980 X P/Stephan-Oerma, 1980 XII Meier, 1980 XIII P/Tuttle, 1981 II Panther, 1981 IV P/Borrelly, 1981 XIX P/Swift-Gehrels, 1982 I Bowell, 1982 IV P/Grigg-Skjellerup, 1982 VI Austin, 1982 VII P/d'Arrest, 1982 VIII P/Churyumov-Gerasimenko, 1983 V Sugano-Saigusa-Fujikawa, 1983 VII IRAS-Araki-Alcock, 1983 X P/Tempel 2, 1983 XI P/Tempel 1, 1983 XIII P/Kopff, 1983 XIV P/IRAS, 1983 XV Shoemaker, 1984 III P/Hartley-IRAS, 1984 IV P/Crommelin, 1984 XI P/Faye, 1984 XIII Austin, 1984 XIV P/Wild 2, 1984 XVI P/Shoemaker 1, 1984 XXIII Levy-Rudenko, 1985 I P/Tsuchinshan 1, 1985 XIII P/Giacobini-Zinner, 1985 XV P/Giclas, 1985 XVI P/Ciffréo, 1985 XVII Hartley-Good, 1985 XVIII P/Shoemaker 3, 1985 XIX Thiele, 1986 I P/Boethin, 1986 III P/Halley, 1986 VIII P/Machholz, 1986 XVII Levy, 1986 XVIII Terasako, 1987 II Sorrells, 1987 VII Wilson, 1987 XIX P/Schwassmann-Wachmann 2, 1987 XXI Levy, 1987 XXIII Rudenko, 1987 XXIV P/Brooks 2, 1987 XXVII P/Kohoutek, 1987 XXIX Bradfield, 1988 IV Furuyama, 1988 XIV P/Tempel 2, 1989 III Shoemaker, 1989 XV P/Schwassmann-Wachmann 1, 1989 XIX Okazaki-Levy-Rudenko, 1990 V Austin, 1990 XVII Tsuchiya-Kiuchi, 1990 XX Levy, 1990 XXI P/Encke, 1990 XXVI Arai, 1991 I P/Metcalf-Brewington, 1991 XV P/Hartley 2, 1991 XVII P/Arend-Rigaux, 1991a1 Shoemaker-Levy, 1991g1 Zanotta-Brewington, 1992c P/Howell, 1992d Tanaka-Machholz, 1992e P/Singer Brewster, 1992f P/Shoemaker-Levy 8, 1992h Spacewatch, 1992j P/Ashbrook-Jackson, 1992t P/Swift-Tuttle, 1992u P/Väisälä 1, 1992w P/Slaughter-Burnham, 1992x P/Schaumasse, 1992y Shoemaker, 1993a Mueller, 1993d Mueller

  7. The Two-Phase, Two-Velocity Ionized Absorber in the Seyfert 1 Galaxy NGC 5548

    NASA Astrophysics Data System (ADS)

    Andrade-Velázquez, Mercedes; Krongold, Yair; Elvis, Martin; Nicastro, Fabrizio; Brickhouse, Nancy; Binette, Luc; Mathur, Smita; Jiménez-Bailón, Elena

    2010-03-01

    We present an analysis of X-ray high-quality grating spectra of the Seyfert 1 galaxy NGC 5548 using archival Chandra-High Energy Transmission Grating Spectrometer and Low Energy Transmission Grating Spectrometer observations for a total exposure time of 800 ks. The continuum emission (between 0.2 keV and 8 keV) is well represented by a power law (Γ = 1.6) plus a blackbody component (kT = 0.1 keV). We find that the well-known X-ray warm absorber (WA) in this source consists of two different outflow velocity systems. One absorbing system has a velocity of -1110 ± 150 km s-1 and the other of -490 ± 150 km s-1. Recognizing the presence of these kinematically distinct components allows each system to be fitted independently, each with two absorption components with different ionization levels. The high-velocity system consists of two components, one with a temperature of 2.7 ± 0.6 × 106 K, log U = 1.23, and another with a temperature of 5.8 ± 1.0 × 105 K, log U = 0.67. The high-velocity, high-ionization component produces absorption by charge states Fe XXI-XXIV, while the high-velocity, low-ionization component produces absorption by Ne IX-X, Fe XVII-XX, and O VII-VIII. The low-velocity system also required two absorbing components, one with a temperature of 5.8 ± 0.8 × 105 K, log U = 0.67, producing absorption by Ne IX-X, Fe XVII-XX, and O VII-VIII, and the other with a lower temperature of 3.5 ± 0.35 × 104 K and a lower ionization of log U = -0.49, producing absorption by O VI-VII and the Fe VII-XII M-shell Unresolved Transitions Array. Once these components are considered, the data do not require any further absorbers. In particular, a model consisting of a continuous radial range of ionization structures (as suggested by a previous analysis) is not required. The two absorbing components in each velocity system are in pressure equilibrium with each other. This suggests that each velocity system consists of a multi-phase medium. This is the first time that

  8. Determination of Groundwater Velocity and Dispersion Parameters by Borehole Wall Multielectrode Geoelectrics

    NASA Astrophysics Data System (ADS)

    Kessels, W.; Wuttke, M. W.

    2007-05-01

    measurements and vertical four point electrode interpretations. The transport equation for NaCl-tracered water is the basic rule to determine the groundwater transport velocity. Numerical calculations to simulate the measurement are carried out with the program FEFLOW. Due to the density contrast, the tracer undergoes vertical movement. Kessels, W., Zoth, G.(1998): Doppelmantel - Packer mit geoelektrischer Meßtechnik zur Bestimmung der Abstandsgeschwindigkeit des Grundwassers, Patent Az:19855048.0, GGA-Institut, Germany, Hannover. KESSELS, W., RIFAI, H., THORENZ, C., ZOTH, G.(2002): Multi Electrode Geoelectric on the Borehole Wall- Determination of groundwater velocity and dispersion parameters, AGU spring meeting, Washington KESSELS, W., ZOTH, G., WONIK, T., FULDA, C. (1999): THE USE OF SALT CARTRIDGES FOR FLUID LOGGING. XXIV GENERAL ASSEMBLY OF E.G.S. THE HAGUE, THE NETHERLANDS PANTELEIT,B., KESSELS, W., BINOT, F (2006): MUD TRACER TEST DURING SOFT ROCK DRILLING; W.R.R., VOL. 42, W11415, DOI:10.1029/2005WR004487

  9. Light Noble Gas Abundances in the Solar Wind Trapped by Chondritic Metal

    NASA Astrophysics Data System (ADS)

    Murer, Ch.; Bauer, H.; Wieler, R.

    1995-09-01

    by less than about 15% from those reported for present day SW and for solar gases in Acfer111 metal [4]. Remarkable is the good agreement of Ne/Ar deduced from meteorites with the SWC ratio, since the derivation of the latter value involved an about 40% correction for solar ^36Ar released from lunar soil and retrapped into the aluminium foils. References: [1] Wieler R. et al. (1993) LPS XXIV, 1519. [2] Wieler R. and Baur H. (1995) Astrophys. J., in press. [3] Murer Ch. et al. (1994) Meteoritics, 29, 506. [4] Pedroni A. and Begemann F. (1994) Meteoritics, 29, 632. [5] Murer Ch. (1995) Ph.D. thesis, ETH Zurich, #10964. [6] Cerutti H. (1974) Ph.D. thesis, Univ. Bern.

  10. Biogeochemical cycling of zinc and its isotopes in the Southern Ocean

    NASA Astrophysics Data System (ADS)

    Zhao, Y.; Vance, D.; Abouchami, W.; de Baar, H. J. W.

    2014-01-01

    We report Zn concentration and isotope data for seawater samples from the Atlantic sector of the Southern Ocean, collected during the IPY/GEOTRACES ANT-XXIV/III cruise along the Greenwich Zero Meridian. Data are reported for the full depth range of the water column at three stations, as well as a transect of surface samples, using a new analytical approach that is presented in detail here. Zn concentrations increase with depth, though due to proximity to upwelling sites, surface concentrations are not as low as in some parts of the ocean such as further northward into the Sub-Antarctic Zone. For two depth profiles south of the Polar Front Zone, the physical stratification of the upper water column is reflected in sudden near-surface changes in Zn concentration with depth. In contrast, beneath 100-300 m Zn concentrations barely change with depth. Zn isotopic data beneath 1000 m, for the Southern Ocean data presented here as well as published data from the North Atlantic and North Pacific, are strikingly homogeneous, with an average δ66Zn = +0.53 ± 0.14‰ (2SD, 2SE = 0.03, n = 21). The surface Southern Ocean is more variable, with δ66Zn ranging from 0.07‰ to 0.80‰. Between the two is a thin horizon at 40-80 m which, in the Southern Ocean as well as the North Atlantic and North Pacific, is characterised by distinctly light isotopic signatures, with δ66Zn about 0.3‰ lower than surface waters. Strong correlations between Si and Zn concentrations seen here and elsewhere, coupled to the lack of any systematic relationship between Si and Zn isotopes in the Southern Ocean, suggest that the removal of Zn associated with diatom opal involves little or no isotopic fractionation. Regeneration of this Zn also explains the homogeneous Zn isotopic composition of the global deep ocean so far sampled. However, the low Zn content of opal requires that deep ocean Zn does not directly come from the opal phase itself, but rather from associated organic material external to

  11. A Practical Guide for the Preparation of Specimens for X-ray Fluorescence and X-ray Diffraction Analysis (by V. E. Buhrke, R. Jenkins, and D. K. Smith)

    NASA Astrophysics Data System (ADS)

    Rudman, Reuben

    1999-06-01

    Wiley-VCH: New York, 1998. xxiv + 333 pp. ISBN 0-471-19458-1. $79.95. I would have subtitled this book "All You Ever Wanted To Know about ...Sample Preparation". Although its principal thrust is geared towards the analytical chemist in an X-ray diffraction (XRD) or X-ray fluorescence (XRF) service laboratory, this text will be of use primarily as a reference source in all milieus dealing with undergraduate research projects and advanced laboratory courses in physical and analytical chemistry. It contains dozens of suggestions for preparing randomly oriented small samples of nearly anything. For example, rocks and minerals, soft organics and hard ceramics, radioactive and liquid materials, metals and oils are all treated. As the availability of XRD and XRF equipment has increased, so has the use of these techniques in the teaching schedule. Many undergraduate laboratory and research projects utilizing these methods have been described in the literature and are found in laboratory textbooks. Very often, especially with the increasingly common use of automated computer-controlled instrumentation, sample preparation has become the key experimental technique required for successful data collection. However, it is not always easy to prepare the statistically random distribution of small particles (crystallites) that is required by these methods. A multitude of techniques have been developed over the past 70 years, but many of them have been handed down by word of mouth or are scattered throughout the literature. This book represents an attempt to systematically describe the theory and practice of sample preparation. This excellent guide to the intricacies of sample preparation begins with a description of statistical sampling methods and the principles of grinding techniques. After a discussion of XRF specimen preparation, which includes pressing pellets, fusion methods, crucible selection and handling very small samples, detailed descriptions for handling rocks

  12. Life sciences and space research XXIV(1) - Gravitational biology; Proceedings of Symposia 10 and 13 of the Topical Meeting of the Interdisciplinary Scientific Commission F (Meetings F1 and F2) of the COSPAR 28th Plenary Meeting, The Hague, Netherlands, June 25-July 6, 1990

    NASA Technical Reports Server (NTRS)

    Young, R. S. (Editor); Cogoli, A. (Editor); Planel, H. (Editor); Ubbels, G. A. (Editor); Sievers, A. (Editor); Oser, H. (Editor); Horneck, G. (Editor); Wagner, H. (Editor)

    1992-01-01

    Topics presented include an introduction to theories and models of biological response to gravity, gravity effects on biological systems, the function of calcium in plant graviperception, developmental biology on unmanned spacecraft, and the effect of microgravity on the development of plant protoplasts flown on Biocosmos 9. Also presented are the mechanism by which an asymmetric distribution of plant growth hormone is attained, the perception of gravity by plants, an animal research facility for Space Station Freedom, the long-term effects of microgravity and possible countermeasures, and an experimental system for determining the influence of microgravity on B lymphocyte activation and cell fusion.

  13. Use of Major- and Minor-Element Mapping to Measure Chemical Variability in Diogenite Pyroxenes

    NASA Astrophysics Data System (ADS)

    Spilde, M. N.; Papike, J. J.

    1993-07-01

    apparent concentration is close to the real (ZAF-corrected) concentration. A number of grains have been mapped in Roda, Garland, EET 83246 and LEW 88008. Except for Garland, OPX grains are relatively homogeneous. Some large Roda grains show very fine (100) augite lamellae along with small augite blebs and scattered spinel along relict grain boundaries. Orthopyroxenes in Garland exhibit rare zoning and thin augite lamellae. Both symmetrical and asymmetrical zoning are evident in elemental maps; an example of nearly symmetrical zoning is shown in the Fe and Mg quantitative maps in Fig. 1, which appears in the hard copy (note a companion abstract [3] that illustrates a microprobe traverse across this grain). In addition, some grains show evidence of partial relict rims, indicating that the grains are brecciated fragments of larger, zoned grains. These brecciated pieces may explain some, but not all, of the intragrain variability seen in Garland. Because Cr decreases toward the rim while Al remains relatively constant, those fragments from the grain core will have higher Cr/Al ratios than fragments from the rim. Acknowledgment: This research was supported by NASA Grant NAGW-3347 and the Institute of Meteoritics. References: [1] Hewins R. (1980) LPSC XI, 441-443. [2] Papike J. J. et al. (1993) LPSC XXIV, 1109-110. [3] Papike J. J. and Spilde M. N. (1993), this volume.

  14. Extraction of He and NE from Individual Lunar Ilmenite Grains by Pulse Heating

    NASA Astrophysics Data System (ADS)

    Nier, A. O.; Schlutter, D. J.

    1993-07-01

    observed in the total gas released by laser beam extractions performed on single grains from the same lunar ilmenite samples [3]. While there is considerable scatter in the data, the overall results are gratifying, and should become more definitive as more particles are investigated. The initial releases, almost certainly from the surfaces of the particles, come closer to the solar wind values [4] than generally reported for lunar grains. It will be interesting to see whether or not the differences observed are real and have a bearing on the general problem of the variation of the solar wind with time [5]. Acknowledgment: We are indebted to R. Wieler for the ilmenite grains used in the investigation. References: [1] Nier A. O. and Schlutter D. J. (1993) LPS XXIV, 1075-1076.[2] Wieler R. et al. (1986) GCA, 50, 1997-2017. [3] Olinger C. T. et al. (1990) Meteoritics, 25, 394. [4] Geiss J. et al. (1972) Apollo 16 Prelim. Sci. Rept., 14-1 to 14-10, NASA SP 315. [5] Becker R. H. and Pepin R. O. (1989) GCA, 53, 1135-1146.

  15. Nitrogen in Interplanetary Dust Particles

    NASA Astrophysics Data System (ADS)

    Keller, L. P.; Thomas, K. L.; Bradley, J. P.; McKay, D. S.

    1995-09-01

    SEM/EDX analysis of L2011R11 shows that it has a bulk C abundance of ~9 wt.% (nearly 3X the CI abundance), which indicates that, for this particle, the absolute N abundance is also enriched above CI levels. EELS is well-suited for this analysis because of its sensitivity for light element detection and quantification, and also for the additional data on bonding environment that can be deduced from the near-edge structure. References: [1] Stadermann F. J. et al. (1989) Meteoritics, 24, 327. [2] Stadermann F. J. et al. (1990) LPS XXI, 1190. [3] Messenger S. et al., this volume. [4] Clemett S. J. et al. (1993) Science, 262, 721. [5] Kerridge J. F. (1985) GCA, 49, 1707. [6] Fomenkova M. N. et al. (1994) GCA, 58, 4503. [7] Bradley J. P. et al. (1993) LPS XXIV, 173. [8] Anders E. and Grevesse N. (1989) GCA, 53, 197. FIGURE 1. Electron energy-loss data from carbonaceous material in L2011R11 (a pyroxene-rich, anhydrous IDP) showing detectable nitrogen associated with carbon. The lower spectrum is a 2nd difference spectrum of the raw data.

  16. Comparative analysis of several sediment transport formulations applied to dam-break flows over erodible beds

    NASA Astrophysics Data System (ADS)

    Cea, Luis; Bladé, Ernest; Corestein, Georgina; Fraga, Ignacio; Espinal, Marc; Puertas, Jerónimo

    2014-05-01

    studied. The first one is the benchmark case presented in Soares-Frazao et al. (2012), and consists in an instanteneous dam-break flow over a sand bed. The second one corresponds to the experimental studies performed at the Engineering Faculty of the UNAM (Fuentes-Mariles et al. (2010)) and consists in the erosion of a volcanic sand dike by an overtopping flow. In both cases experimental measurements of water depth and bed evolution are available to evaluate the performance of different sediment transport formulations. A sensitivity analysis to the physical properties of the bed material (grain density and size) is also presented for each formulation, in order to analyse to which degree the properties of the bed material need to be defined in the numerical model. References Bladé, E., Cea, L., Corestein, G., Escolano, E., Puertas, J., Vázquez-Cendón, M.E., Dolz, J., Coll, A. (2014). Iber: herramienta de simulación numérica del flujo en ríos. Revista Internacional de Métodos Numéricos para Cálculo y Diseño en Ingeniería, Vol.30(1), pp.1-10 Fuentes-Mariles, Ó. A., Cruz-Gerón, J. A., Rivera-Díaz, C., Luna-Cruz, F., and González-Prado, J. (2010). "Caracterización Experimental de Ruptura de Diques." XXIV Congreso Latinoamericano de Hidráulica Soares-Frazão et al. (2012). Dambreak flows over mobile beds: experiments and benchmark tests for numerical models. Journal of Hydraulic Research, Vol.50(4), pp.364-375

  17. The diagnosis and treatment of peripheral lymphedema: 2013 Consensus Document of the International Society of Lymphology.

    PubMed

    2013-03-01

    This International Society of Lymphology (ISL) Consensus Document is the current revision of the 1995 Document for the evaluation and management of peripheral lymphedema (1) for discussion at the XXIV International Congress of Lymphology. It is based upon modifications: [A] suggested and published following the 1997 XVI International Congress of Lymphology (ICL) in Madrid, Spain (2) discussed at the 1999 XVII ICL in Chennai, India (3) and considered/ confirmed at the 2000 (ISL) Executive Committee meeting in Hinterzarten, Germany (4); [B] derived from integration of discussions and written comments obtained during and following the 2001 XVIII ICL in Genoa, Italy as modified at the 2003 ISL Executive Committee meeting in Cordoba, Argentina (5); [C] suggested from comments, criticisms, and rebuttals as published in the December 2004 issue of Lymphology (6); [D] discussed in both the 2005 XX ICL in Salvador, Brazil and the 2007 XXI ICL in Shanghai, China and modified at the 2008 Executive Committee Meeting in Naples, Italy (7,8); and [E] modified from discussions and written comments from the 2009 XXII ICL in Sydney, Australia, the 2011 XXIII ICL in Malmo, Sweden and 2012 Executive Committee Meetings. The document attempts to amalgamate the broad spectrum of protocols advocated worldwide for the diagnosis and treatment of peripheral lymphedema into a coordinated proclamation representing a "Consensus" of the international community. The document is not meant to override individual clinical considerations for problematic patients nor to stifle progress. It is also not meant to be a legal formulation from which variations define medical malpractice. The Society understands that in some clinics the method of treatment derives from national standards while in others access to medical equipment and supplies is limited, and therefore the suggested treatments are impractical. Adaptability and inclusiveness does come at the price that members can rightly be critical of what

  18. The Chondrite Neagari: Petrography, Mineralogy, Chemical Compositions, and Cosmogenic Nuclides

    NASA Astrophysics Data System (ADS)

    Okada, A.; Komura, K.; Nagao, K.; Nishiizumi, K.; Miyamoto, Y.; Sakamoto, K.; Ebihara, M.; Shima, M.

    1995-09-01

    ) have been identified and their contents were determined by using a mock sample having known amounts of natural radioactivities. Among these nuclides, ^44mSc has the shortest half life (2.44 d) and has also been measured in the Mihonoseki meteorite [1]. Cosmogenic components were also observed for ^3He, ^21Ne, and ^38Ar by noble gas mass spectrometry. Cosmic-ray exposure ages calculated from cosmogenic ^21Ne and ^38Ar contents coupled with production rates by Eugster [2] and Schultz et al. [3], respectively, seem to be consistent (about 45 Ma), but the age from ^3He is significantly lower. Considering the loss of radiogenic ^4He, the Neagari meteorite must have experienced a high temperature event in space. Cosmogenic radionuclides ^10Be, ^26Al, and ^36Cl were also measured in an aliquot (77 mg) of the Neagari meteorite using an AMS facility at Lawrence Livermore National Laboratory. The concentrations of these nuclides in conjunction with the noble gas data as well as data of elemental abundances provide better knowledge of the exposure history of this meteorite. References: [1] Shima M. et al. (1993) LPS XXIV, 1297-1298. [2] Eugster O. (1988) GCA, 52, 1649-1662. [3] Schultz L. et al. (1991) GCA, 55, 59-66.

  19. Asteroid Spectroscopy: A Declaration of Independence

    NASA Astrophysics Data System (ADS)

    Bell, J. F.

    1995-09-01

    value. Carbonaceous: These asteroids were interpreted as "carbonaceous chondrites", due to a superficial resemblance in spectral shape and their lesser abundance than S-types. Later it was shown that the most common CCs, COs and CVs, actually fall into the classical S class (now broken off as a separate K class). But Cs and the related G, B, and F classes have been persistently interpreted as CM/CI analogs even though their only resolvable spectral feature is much shallower than that of the CM/CI meteontes. This difference has been rationalized with more "space weathering" processes. However, recently rare highly metamorphosed CCs have been shown to match the C-G-B-F asteroid without "weathering"[4], suggesting that CIs and CMs come from some small, undiscovered class of outer belt asteroids analagous to Qs in the inner belt. These examples demonstrate an evolution of our thinking from belief in a close relationship between the meteorite population and the asteroids (with any discordant results from the telescope explained away by ad hoc mechanisms), toward a model in which the gigantic meteorite data set is seen as highly biased and non-representative of the asteroid belt, and in many cases useless due to the multiple possible interpretations of the same data. It is time for a more balanced approach to asteroid science, in which meteoritics plays a supplementary role to direct studies of asteroids, rather that the dominant one it has to date. References: [1] Binzel et al. (1993) Science, 260, 186-191. [2] Gaffey M. J. et. al. (1994) Icarus, 106, 573-602. [3] Binzel R. P. et al. (1994) Science, 262, 1541-1543. [4] Hiroi T. et al. (1993) LPS XXIV, 659-660.

  20. Phosphate-Silicate Inclusions in Chaunskij: How Diverse are They?

    NASA Astrophysics Data System (ADS)

    Petaev, M. I.; Clarke, R. S., Jr.; Jarosewich, E.; Lipschutz, M. E.; Wang, M.-S.; Davis, A. M.; Steele, I. M.; Olsen, E. J.; Wood, J. A.

    1993-07-01

    intergrowths, with or without silica and opaque minerals. However, some inclusions do not match the mineralogies of "igneous" or "metamorphic" lithologies. They consist of cordierite only (inclusion #1-10); cordierite and silica (#1-18); silica, whitlockite, and troilite with minor Al-rich chromite and rare pyroxene (#4- 5A); plagioclase and whitlockite (#4-5D); and silica and whitlockite (#4-6E). Mineral compositions vary considerably both between and within all inclusions. No systematic differences between separate inclusions were found. Compositions of pyroxene and plagioclase match those of mesosideritic minerals. The chromite and ilmenite display systematic variations in MgO, MnO, Al(sub)2O(sub)3 and V(sub)2O(sub)3 contents, suggestive of a precursor material consisting of a series of basaltic rocks. The bulk chemical composition of the largest silicate inclusion, recalculated to the silicate fraction only, is very close to that of eucrites and mesosiderites except for a large enrichment in P and volatile chalcophiles. Major-element and REE chemistry and bulk mineralogy point to cumulate eucrites as the precursor of the silicate inclusions. This precursor was apparently slightly fractionated during the remelting event inferred by the structure of the "igneous" lithology. The "metamorphic" lithology apparently was formed due to reaction between silicates and phosphorus dissolved in the metal: Px + An + P + O --> Cord + Q + Whit. This reaction took place under ~700 degrees C and ~4 kbar [3] in the interior of the Chaunskij parent body. Compositions and textures of small inclusions suggest that the metamorphic reaction took place before the incorporation of the inclusions into the piece of metal making up the Chaunskij main mass. References: [1] Petaev M. I. et al. (1993) LPS XXIV, 1131-1132. [2] Clarke R. S. Jr. et al., this volume. [3] Petaev M. I. et al. (1992) Meteoritics, 27, 276-277.

  1. Cosmogenic Radionuclides in Recently Fallen Chondrites Mihonoseki and Tahara

    NASA Astrophysics Data System (ADS)

    Shima, M.; Honda, M.; Yabuki, S.; Takahashi, K.

    1993-07-01

    comparison, while for Mihonoseki only (3) was used. The difficulty was to prepare a suitable mock sample having the same density as chondrites 3.5. Especially for a large sample like Mihonoseki, even when we use about equal fractions of olivine sand and metallic iron, the weight of the mock was about 80%, and when we intend to obtain heavier than 90%, we have to use a larger portion of metallic iron, which causes some reductions in the efficiencies of 20-30%, depending on energies. Results: The contents of 14 gamma emitters were studied as shown in the Table (which appears in the hard copy). Errors quoted are only from counting statistics. The most striking may be to learn that Mihonoseki contains a very low level of 60Co; the content is lower than 1 dpm/kg, which could not be determined accurately by a current-direct gamma counting. This reflects the smaller preatmospheric size of the body, and consistent with other observations such as 22Ne/21Ne = 1.180 [1] and lower activity levels of general products such as 46 dpm 26Al/kg, which is about three-fourths of a common level among L chondrites. Besides, relatively high 56Co in respect to 58Co is also noticed in Mihonoseki. References: [1] Shima M. et al.(1993) LPSC XXIV 1297-1298. [2] Shima M. et al.(1993) Meteoritical Bull., in press.

  2. Large Stratospheric IDPs: Chemical Compostion and Comparison with Smaller Stratospheric IDPs

    NASA Astrophysics Data System (ADS)

    Flynn, G. J.; Bajt, S.; Sutton, S. R.; Klock, W.

    1995-09-01

    2008G10, showed a large Zn depletion (Zn/Fe <0.01xCI). This was accompanied by low contents of Ga, Ge and Br (see Figure 1). This pattern of Zn, Ge, Br and Ga depletions was previously seen in smaller IDPs which were severely heated, presumably on atmospheric entry [2]. Sulfur and K are also low in L2008G10, suggesting these elements are also lost during heating, but the Se content is 0.8xCI. A second particle, L2009C8, has a Zn/Fe=0.26xCI, possibly indicating less severe heating. The low fraction of severely heated IDPs, only one in this set of 7 and none in the set of 6 [1] suggests a very low atmospheric entry velocity for these large IDPs [3]. References: [1] Flynn G. J. et al. (1995) LPS XXVI, 407-408. [2] Flynn G. J. et al. (1993) LPS XXIV, 495-496. [3] Flynn G. J., this volume. Figure 1: Average Fe and CI normalized element abundances in 7 large IDPs, 6 different large IDPs [1], 51 smaller IDPs [2], and the single low-Zn IDP, L2008G10, included in the set of 7 large IDPs.

  3. Constraints on Nubular Electromagnetic Pulses

    NASA Astrophysics Data System (ADS)

    Eisenhour, D. D.; Buseck, P. R.

    1993-07-01

    emission allow further constraints to be placed on the EMPs responsible for "dirty snowball" formation. The absorption and emission efficiencies of grains in a blackbody radiation field were determined by calculating Planck mean cross sections for olivine, pyroxene, and iron as a function of grain size [2,3]. This information was combined with conductive heat flow calculations to determine the behavior of olivine and pyroxene grains with small inclusions of metal. Results indicate that "dirty snowball" formation results only over a narrow flux range for a given multiphase assemblage, with higher fluxes required for smaller, more transparent, or more refractory grains. For a 100-mm olivine chondrule containing a 10-micrometer "dirty snowball," the required flux is ~9 +- 1 x 10^8 ergs cm^-2 sec^-1, with a minimum pulse duration of 4 seconds (assuming an initial grain temperature of 500 K prior to heating). These values are in good agreement with experimentally determined values. The results show that pulses energetic enough to create "dirty snowballs" are also capable of producing the total melting required for chondrule formation with only slight increases in flux, or with only marginally different grain properties (e.g., more opaque inclusions, lower melting points, higher absorption cross sections). Because of the temperature and grain size dependence of the Planck mean cross sections of silicates, an EMP of the type described above will selectively melt larger aggregates and individual grains (>100 micrometer) while leaving smaller aggregates and grains unmelted. Therefore, natural products of EMP heating are: 1) the formation of chondrules in a sustained dusty environment, 2) a paucity of small chondrules, and 3) residual grains relatively unaffected by the EMPs. References: [1] Eisenhour D. D. and Buseck P. R. (1993) LPSC XXIV, 435-436. [2] Falk S. W. and Scalo J. M. (1975) Ap. J., 202, 690-695. [3] Gilman R. C. (1974) Ap. J. Supp., 268, 28, 397-403.

  4. 14C Terrestrial Ages of Meteorites from Desert Regions: Algeria and Australia

    NASA Astrophysics Data System (ADS)

    Jull, A. J. T.; Wlotzka, F.; Bevan, A. W. R.; Brown, S. T.; Donahue, D. J.

    1993-07-01

    might expect that meteorites would be more well preserved in a very arid, hot climate, and some meteorites of longer age would be present, but this appears not to be the case. This interpretation is strengthened by the results from Nullarbor Plain, although the Australian collection does show some older samples. However, these two regions do show the expected exponential drop-off in number of meteorites of a given terrestrial age with time, which indicates the collections have been undisturbed over at least the last 20,000 yr. This is not seen in the U.S. meteorites. The less arid and colder high plains of Texas and New Mexico may be more conducive to storage of meteorites for long periods of time than these areas, but we believe some selection processes must be at work here and there is a deficit of "young" meteorites. References: [1] Suess H. and Wanke H. (1962) GCA, 26, 475. [2] Fireman E. L. (1978) Proc. LPSC 9th, 1647. [3] Beukens R. P. et al. (1988) Proc. NIPR Symp. Antarc. Met., 1, 224. [4] Jull A. J. T. et al. (1989) GCA, 53, 2095. [5] Jull et al. (1993) Meteoritics, in press. [6] Reedy R. C. (1993) LPS XXIV. [7] Boeckl R. P. (1972) Nature, 236, 25. [8] Jull A. J. T. et al. (1991) LPS XXII, 665. [9] Jull A. J. T. et al. (1990) GCA, 54, 2895. Fig. 1, which appears here in the hard copy, shows terrestrial ^14C ages from desert regions.

  5. Plasma Density and Electro-Magnetic Field Perturbations Hf-Induced in the Outer Ionosphere: Review of Experimental Results

    NASA Astrophysics Data System (ADS)

    Frolov, Vladimir; Rauch, Jean-Louis; Parrot, Michel; Rapoport, Victor; Shorokhova, Elena

    wave frequency should be no less than 0.5 - 0.7 MHz below the F _{2} layer critical frequency f _{0F2}. In the opposed case the penetration of the radiated power behind the F _{2} ionospheric layer can take place [4]. 5. Strong variations of the electron temperature are observed inside the ducts, at the same time the ion temperature is unchanged. 6. A feature of the ducts is the presence of strong electro-magnetic field fluctuations in a frequency range from a few Hz to tens of kHz [1,5]. 7. It was revealed that the formation of the ducts in the outer ionosphere can stimulate the precipitation of energetic electrons with E ≥ 100 keV from the Earth’s radiation belts [6]. The work was supported by RFBR grants (## 12-05-00312, 13-02-12074, 13-02-12241) and by the scientific program “Geophysics”. References: 1. Rapoport V.O., V.L. Frolov, G.P. Komrakov, et al. // Radiophysics and Quantum Electronics, 2007. Vol. 50(8), p. 645. 2. Frolov V.L., V.O. Rapoport, G.P. Komrakov, et. al. // JETP Letters, 2008. Vol. 88, No. 12, p. 790. 3. Frolov V.L., I.A. Bolotin, V.O. Rapoport, et. al. // XXIV All-Russian conference “Radio Wave Propagation”. Irkutsk, 2014 (submitted for publication). 4. Frolov V.L., N.A. Mityakov, E.A. Shorokhova, M. Parrot. // Radiophysics and Quantum Electronics, 2013. Vol. 56(6), p. 325. 5. Rapoport V.O., V.L. Frolov, S.V. Polyakov, et al. // J. Geophys. Res., 2010. Vol. 115, A10322, doi:10.1029/2010JA015484. 6. Markov G.A., A.S. Belov, V.L. Frolov, et al. // JETPh, 2010. Vol. 138, No. 6(12), p. 1037.

  6. The Distribution and Modes of Occurrence of Anorthosite on the Moon

    NASA Astrophysics Data System (ADS)

    Hawke, B. R.; Spudis, P. D.; Taylor, G. J.; Lucey, P. G.; Peterson, C. A.

    1993-07-01

    Theophilus and Piccolomini craters. Anorthosites have now been located on, or very near, the four innermost rings of Nectaris. Northern Highlands. Recent studies utilizing both Earth-based spectra and Galileo SSI suggest that pure anorthosite is exposed within Goldschmidt crater and west of Thales [6]. Both areas are plains units that have been affected by nearby large Copernican craters (Thales and Anaxagoras). Other occurrences. Anorthosites have also been identified in the central peaks of Alphonsus and Petavius [5,7]. Both of these craters are very near major rings of ancient impact basins. Discussion: To date, anorthosites have only been identified in a relatively narrow belt in the southern highlands, extending from Petavius in the east to the Inner Rook Mts. on the western limb, and at two locations in the far north. Extensive spectral studies of many nearside regions (e.g., north central highlands, Imbrium) have failed to reveal additional deposits of pure anorthosite. Lunar anorthosite deposits are almost always found on or very near basin rings. This association is significant only for the inner rings of basins such as Grimaldi and Orientale. These rings were derived from beneath more mafic-rich layers in the pre- impact target sites. In contrast, the anorthosites associated with the outer rings of Nectaris and other basins are generally found in the central peaks and walls of large impact craters. It appears that these anorthosites were derived from layers many kilometers beneath the crater target sites and that the surfaces of these outer rings are not composed of anorthosite. References: [1] Spudis P. D. et al. (1984) Proc. LPSC 15th, in JGR, 89, C197. [2] Hawke B. R. et al. (1991) GRL, 18, 2141. [3] Spudis P. D. et al. (1989) LPSC XIX, 51. [4] Hawke B. R. et al. (1993) GRL, 20, 419. [5] Pieters C. M. (1986) Rev. Geophys., 24, 557. [6] Pieters C. M. et al. (1993) LPS XXIV, 1141. [7] Coombs C. R. et al. (1990) LPSC XX, 161.

  7. Remote Sensing Studies of Anorthosite Deposits on the Moon

    NASA Astrophysics Data System (ADS)

    Hawke, B. R.; Taylor, G. J.; Lucey, P. G.; Peterson, C. A.; Blewett, D. T.; Spudis, P. D.

    1995-09-01

    Basin region. While noritic anorthosites and anorthositic norites are the dominant rock types in the region, anorthosites have now been located on, or very near, the four innermost rings of Nectaris [3,4,8]. Relatively low (<4%) FeO values are associated with Kant and Cyrillus A craters. Crisium Basin region. A recent spectral survey of the Crisium region failed to locate pure anorthosite deposits [9]. However, an analysis of Galileo multispectral imagery and FeO map has shown that small exposures of pure anorthosite occur near Proclus crater and in the vicinity of Geminus crater. Other Occurrences. Recent studies utilizing both Earth-based spectra and Galileo SSI data suggest that pure anorthosite is exposed within Goldschmidt crater in the northern highlands [10]. Anorthosites have also been identified in the central peaks of Alphonsus and Petavius craters [8,11]. Very recently, Clementine near-IR images were used to show that anorthosite was present in the central peak of Aristarchus crater [12]. In every instance, the anorthosites on the nearside were exposed from beneath a shallower near-surface layer of more pyroxene-rich material. Recent results from the Clementine mission indicate that pure anorthosite may be quite abundant on certain farside surfaces [7]. References: [1] Spudis P. et al. (1984) Proc. LPSC 15th, in JGR, 89, C197. [2] Hawke B. et al. (1991) GRL, 18, 2141. [3] Spudis P. et al. (1989) Proc. LPSC 19th, 51. [4] Hawke B. et al. (1986) NASA TM-88383, 526. [5] Peterson C. et al. (1995) GRL, in press. [6] Hawke B. et al. (1993) GRL, 20, 419. [7] Lucey P. et al. (1995) Science, 268, 1150. [8] Pieters C. (1986) Rev. Geophys., 24, 557. [9] Blewett D. et al. (1995) GRL, in press. [10] Pieters C. et al. (1993) LPS XXIV, 1141. [11] Coombs C. et al. (1990) Proc. LPS, Vol. 20, 161. [12] McEwen A. et al. (1994) Science, 1858.

  8. Prediction of secular acceleration of axial rotation of Mars

    NASA Astrophysics Data System (ADS)

    Barkin, Yu. V.

    2009-04-01

    of daily rotation of the Earth essentially surpasses non-tidal acceleration (35 %) which as shown the author is caused by the directed redistribution of fluid masses of the Earth, in turn caused by polar drift of the centre of mass of the liquid core of the Earth to the north [1]. In case of Mars the opposite picture is expected. It is quite possible, as show the executed estimations, that tidal deceleration of axial rotation of Mars much less than its positive acceleration caused by global dynamics of shells (the core and mantle). And it means, that as against the Earth in axial rotation of Mars in the present epoch an acceleration, instead of deceleration of rotation should be observed. References [1] Barkin Yu.V. (2001) Explanation and prediction of the secular variations of the Earth rotation, geopotential, force of gravity and geocenter drift. Proceedings of International Conference «AstroKazan-2001». Astronomy and geodesy in new millennium (24-29 September 2001), Kazan State University: Publisher «DAS», pp. 73-79. [2] Barkin Yu.V. (2007) To an explanation of non-tidal acceleration of the Earth diurnal rotation and secular trend of its pole. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007), (G) - IAG, GS003, p. 3799. www. iugg2007perugia.it. [3] Barkin Yu.V. (2007) Celestial geodynamics and solution of the fundamental problems of geodesy, gravimetry and geophysics. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007), (S) - IASPEI, JSS011, p. 2149. www. iugg2007perugia.it. [4] Barkin Yu.V. (2002) Explanation of endogenous activity of planets and satellites and its cyclicity. Izvestia cekzii nauk o Zemle. Rus. Acad. of Nat. Sciences, Issue 9, December 2002, M.: VINITI, pp. 45-97. In Russian.

  9. Oxygen Isotopic Fractionation During Evaporation of SiO2 in Vacuum and in H Gas

    NASA Astrophysics Data System (ADS)

    Nagahara, H.; Young, E. D.; Hoering, T. C.; Mysen, B. O.

    1993-07-01

    isotope measurements, including ^17O and silicon isotope measurements, are now in progress, and some of the results are shown in this paper. Oxygen isotopic compositions of residues in vacuum and in hydrogen gas of total pressure of 2.6 x 10^-5 bar, which approximates the pressure of the solar nebula at the midplane at 2-3 AU, are shown in comparison with evaporation rate (Figs. 1 and 2). Oxygen isotopic fractionation is remarkable in a constant evacuation, but is negligible in hydrogen gas of 2.6 x 10^-5 bar total pressure. In vacuum, delta ^18O of solid residue increases with increasing degree of evaporation. The curve is best fit to delta ^18O = 0.00094x^2 + 0.00173x + 19.606 (r = 0.997), where x is the degree of evaporation in weight percent. The curve is fit to the Rayleigh fractionation curve with a constant fractionation factor (alpha(sub)vap-sol) of 0.9970. Figures 1 and 2 show that evaporation is significant but oxygen isotopic fractionation is insignificant in hydrogen gas in the approximate solar nebular condition. The high evaporation rate in hydrogen gas is due to the fact that evaporation is a decomposition reaction of an oxide, which should be accelerated in reducing condition. The rate, however, can be explained by an unknown diffusion process that is possible when hydrogen is reactive with silica [2]. In a fairly high hydrogen pressure, isotopic fractionation is suppressed. On the other hand, in vacuum, the evaporation rate is small but the degree of isotopic fractionation is significant. The results suggest that chondrules and CAIs without isotopic mass fractionation could have been formed in the solar nebula, but that mass loss during heating should have been significant. The CAIs with significant mass fractionation such as HAL could have been formed in vacuum. References: [1] Davis A. et al. (1990) Nature, 347, 655-658. [2] Nagahara H. (1993) LPS XXIV, 1045-1046. Fig. 1, which appears here in the hard copy, shows the evaporation rate of SiO2 heated at

  10. A gravitational potential finding for rotating cosmological body in the context of proto-planetary dynamics problem solving

    NASA Astrophysics Data System (ADS)

    Krot, Alexander M.

    2008-09-01

    Planetary Science Congress, Berlin, Germany, September 18-22, 2006; Planetary Research Abstracts, ESPC2006-A-00014. [9] Krot A. On the principal difficulties and ways to their solution in the theory of gravitational condensation of infinitely distributed dust substance. Proc. XXIV IUGG General Assembly, Perugia, Italy, July 2-13, 2007; GS002 Symposium "Gravity Field", Abstract GS002-3598: 143-144.

  11. SPIG From Beginning To Today

    NASA Astrophysics Data System (ADS)

    Labat, J.

    2010-07-01

    gradually improved, so that the SPIG meetings were again organized on a regular basis and the number of mainly foreign participants, has increased. Meetings were held in Serbian tourist resources (Zlatibor, Kopaonik) except the last XXIV SPIG that was held in town of Novi Sad. Depending mainly on the financial support, number of invited lectures varied, but it is felt that all the SPIG meetings have been highly successful. Let us hope that also this twenty-fifth jubilary SPIG will be successful proving that that the idea of organizing this type of meetings in the republic of Serbia should be continued in the future.

  12. Reduction of EAO Positional Observations Database

    NASA Astrophysics Data System (ADS)

    Nefedyev, Yuri; Andreev, Alexey; Demina, Natalya; Churkin, Konstantin

    2016-07-01

    There is a large data bank of positional observations of Solar System bodies at Engelhadt Astronomical Observatory (EAO). The positional observations include the major planets, except Jupiter. Modern technologies replace classical methods of observations in astronomy and in astrometry as well. At the same time many positional observations have been gathered at astronomical observatories. So taking into account that observations of the past epochs have presenteda great value for astronomy and as times goes by their importance is growing it is obvious that positional astrometry will not lose its practical importance. This was noted in B3 XXIV IAU resolution by the General Assembly. The results of reduction of solar system bodies observations were published mainly in Proceeding of EAO and Transactions of Kazan City Astronomical Observatory. Earlier there have been made about three thousand observations at EAO and Zelenchuk station with the Zeiss telescope (D=400mm, f=2000mm), AFR-18 (photo visual, D=200, f=2000), refractor (D=400mm, f=3450mm), Meniscus camera (D=340mm, f=1200mm), Schmidt camera (D=350mm, f=2000mm). The major planets except Pluto and Neptune were observed with a special cassette chamber equipped with a rotating disk which had an open sector to reduce the brightness of the planets. The dimension of the sector was chosen accordingto the brightness of the planets. The disk was placed in the centre of the astrograph's field. The stars' true brightness was preserved. A large number of catalogues were compiled by the end of the 20th century. We used Tycho-2 catalogue for reducing our observations. As it is known the catalogue Tycho-2 (Tycho-2 catalogue, 2000) includes 2539913 stars. The stars' proper motions given in the catalogue were obtained by comparing positions from Tycho-2 with positions from the Astrographic Catalogue. Therefore they are considered to be highly accurate. The accuracy of stellar positions in Tycho-2 is about 60 mas and the accuracy of

  13. The Nature of Reduction in Space Weathering

    NASA Astrophysics Data System (ADS)

    McKay, D. S.; Allen, C. C.

    1993-07-01

    particles added to the regolith may supply abundant carbon for supporting space weathering reduction processes during impacts. References: [1] Hapke B. (1993) LPI Tech. Rpt. 93-01, 8-9. [2] Allen C. C. et al. (1992) In Engineering, Construction, and Operations in Space III, 629-640, Am. Soc. Civil Engineers, New York. [3] Allen C. C. et al. (1992) LPS XXIII, 21-22. [4] Allen C. C. et al. (1993) Icarus, submitted. [5] Allen C. C. et al. (1993) LPS XXIV, 19-20. [6] Simonds C. H. et al. (1976) Proc. LSC 7th, 2509-2528. [7] Keller L. P. and McKay D. S. (1992) LPS XXIll, 673-674. [8] Sclar C. B. and Bauer J. F. (1976) Proc. LSC 7th, 2493-2508. [9] Thomas K. L. et al. (1993) GCA, in press.

  14. Noble Gases in the LEW 88663 L7 Chondrite

    NASA Astrophysics Data System (ADS)

    Miura, Y. N.; Sugiura, N.; Nagao, K.

    1995-09-01

    likely terrestrial contamination in origin) rather than chondritic ones seem to be dominant in LEW88663. A K-Ar age of 4.3 +/- 0.2 b.y. is obtained assuming K content of 660 ppm by [9], implying radiogenic ^40Ar is almost retained. Because of low abundance of trapped Xe in the meteorite compared with the abundances in other chondrites, ^244Pu-derived fission Xe could be evaluated more precisely. According to the measured Xe data (for this, three isotope plots such as ^134Xe/^130Xe versus ^136Xe/^130Xe are useful), we conclude that Xe in LEW88663 is the mixture of ^244Pu-derived fission Xe and the terrestrial atmospheric Xe with possibility that a small amount of chondritic Xe is contained. Using the same procedure described in [10], we obtained excess ^136Xe concentration, 1.4 x 10^-12 cm^3STP/g with about 20% uncertainty, of which about 3% is from contribution of ^238U-derived ^136Xe if average U content for L chondrite (14 ppb) is assumed. The calculated Pu abundance of 0.21 ppb is slightly higher than those reported for L chondrites Barwell (0.11 +/- 0.05 ppb [11]) and Marion (0.10+/-0.40 ppb [11]). Acknowledgments: We thank Meteorite Working Group for providing the sample. We are also grateful to Dr. D. Mittlefehldt for showing us his chemical composition data. This work is supported by Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists. References: [1] Mason B. et al. (1992) Antarc. Meteorite Newsletter, 15(2), 30. [2] Mason B. and Marlow R. (1992) Antarc. Meteorite Newsletter, 15(1), 16. [3] Davis A. M. et al. (1993) LPS XXIV, 375-376. [4] Mittlefehldt D. W. (1993) Meteoritics, 28, 401-402. [5] Hervey R. P. (1993) Meteoritics, 28, 360. [6] Eugster O. (1988) GCA, 52, 1649-1662. [7] Marti K. and Graf T.(1992) Annu. Rev. Earth Planet Sci., 20, 221-243. [8] E.g. Marti K. (1967) EPSL, 2, 193-196. [9] Mittlefehldt D. W., personal communication. [10] Miura Y. et al. (1993) GCA, 57, 1857-1866. [11] Hagee B. et al. (1990) GCA, 54

  15. The Orbital Distribution of Earth-crossing Asteroids and Meteoroids

    NASA Astrophysics Data System (ADS)

    Benoit, P. H.; Sears, D. W. G.

    1993-07-01

    are a problem for orbits calculated from the radiants of observed falls). Potential applications of these data include investigation of possible meteorite "streams" [2] and exploring questions such as whether different types and classes of meteorites have different orbital distributions [8]. References: [1] Steel D. I. et al. (1991) Mon. R. Astron. Soc., 251, 632-648. [2] Wolf S. F. and Lipschutz M. E. (1992) Meteoritics, 27, 308. [3] Benoit P. H. et al. (1991) Icarus, 94, 311-325. [4] Benoit P. H. and Sears D. W. G. (1993) LPS XXIV, 95- 96. [5] Wetherill G. W. and ReVelle D. O. (1981) Icarus, 48, 308- 328. [6] Williams J. G. (1975) JGR, 80, 2914-2916. [7] Galibina I. V. and Terent'eva A. K. (1987) Solar Sys. Res., 21, 160-166. [8] Graf Th. and Marti K. (1991) LPS XXII, 473-474.

  16. An prediction and explanation of 'climatic swing

    NASA Astrophysics Data System (ADS)

    Barkin, Yury

    2010-05-01

    core-mantle system and their changes in the time have an important role and value for style and intensity of warming and cooling. References [1] Barkin Yu.V. (2002) An explanation of endogenous activity of planets and satellites and its cyclisity. Isvestia sekcii nauk o Zemle Rossiiskoi akademii ectestvennykh nauk. Vyp. 9, М., VINITI, pp. 45-97. In Russian. [2] Barkin Yu.V. (2004) Dynamics of the Earth shells and variations of paleoclimate. Proceedings of Milutin Milankovitch Anniversary Symposium "Paleoclimate and the Earth climate system" (Belgrade, Serbia, 30 August - 2 September, 2004). Belgrade, Serbian Academy of Sciences and Art, pp. 161-164. [3] Barkin Yu.V. (2007) Inversion of periodic and trend variations of climate in opposite hemispheres of the Earth and their mechanism. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007) (P) - IAPSO, JPS001 "Interannual and Interdecadal Climate Variability", p. 1674. www. iugg2007perugia.it. [4] Barkin Yu.V. (2008) Secular polar drift of the core in present epoch: geodynamical and geophysical consequences and confirmations. General and regional problems of tectonics and geodynamics. Materials of XLI Tectonic Conference. V. 1. -M.:GEOS. p. 55-59. In Russian. [5] Barkin Yu.V. (2009) An explanation of secular variations of a gravity at stations Ny-Alesund, Medicine, Churchill and Syowa. Materials of the International Conference: «Yu.P. Bulashevich's fifth scientific readings. A deep structure. Geodynamics. A thermal field of the Earth. Interpretation of geophysical fields» (Ekaterinburg, 6 - 10 July, 2009). pp. 27-31. In Russian. [6] Barkin Yu.V. (2005) Oscillations of the Earth core, new oceanic tides and dynamical consequences. Materials of XI International Scientific Conference "Structure, geodynamics and mineral genetic processes in lithosphere" (September, 20-22 2005, Syktyvkar, Russia), Publisher of Geology Institute of Komi SC of Ural Section

  17. Methodology of Detailed Geophysical Examination of the Areas of World Recognized Religious and Cultural Artifacts

    NASA Astrophysics Data System (ADS)

    Eppelbaum, Lev

    2010-05-01

    the low altitudes (3-5 meters) will help geophysical cover all the studied area with a regular observation step (Eppelbaum, 2008). At the final step all these measurements (including results of the previous works) could be compiled to 4D models of different geophysical parameters (Eppelbaum and Ben-Avraham, 2002; Eppelbaum et al., 2010). Analysis of temperature field in the boreholes drilled in the vicinity of the studied site will permit to estimate the temperature (e.g., Eppelbaum et al., 2006c) in the historical period when this artifact was constructed and, correspondingly, utilize this characteristic for investigation of mechanical and other properties of the ancient building material. Studying of temporal variations of magnetic (e.g., Finkelstein and Eppelbaum) and VLF fields can be also used for determination of nature of some buried ancient remains. The geophysical investigations must be combined with geochemical, paleostructural, paleobiogeographical, paleomorphological and other methods (Eppelbaum et al., 2010). Application of informational parameters (Khesin et al., 1996; Eppelbaum et al., 2003b) will permit to present all available data by the use of integral convolution units. REFERENCES Eppelbaum, L.V., 1999. Quantitative interpretation of resistivity anomalies using advanced methods developed in magnetic prospecting. Trans. of the XXIV General Assembly of the Europ. Geoph. Soc., Strasburg 1 (1), p.166. Eppelbaum, L.V., 2000. Applicability of geophysical methods for localization of archaeological targets: An introduction. Geoinformatics, 11, No.1, 19-28. Eppelbaum, L.V., 2005. Multilevel observations of magnetic field at archaeological sites as additional interpreting tool. Proceed. of the 6th Conference of Archaeological Prospection, Roma, Italy, 4 pp. Eppelbaum, L.V., 2008. Remote operated vehicle geophysical survey using magnetic and VLF methods: proposed schemes for data processing and interpretation. Proceed. of the Symp. on the Application of

  18. Pouring 'Cold Water' on Hot Accretion

    NASA Astrophysics Data System (ADS)

    Rubin, A. E.

    1995-09-01

    -381. [7] Scott E. R. D. et al. (1986) Proc. LPSC 17th, in JGR, 91, E115-E123. [8] Ashworth J. R. (1980) EPSL, 46, 167-177. [9] Ashworth J. R. et al. (1984) Nature, 308, 259-261. [10] G"pel C. et al. (1994) EPSL, 121, 153-171. [11] Jones R. H. and Brearley A. J. (1988) Meteoritics, 23, 277. [12] Brearley A. J. and Jones R. H. (1988) Eos Trans. AGU, 69, 1506. [13] Brearley A. J. and Jones R. H. (1993) LPS XXIV, 185-186. [14] Watanabe S. et al. (1985) EPSL, 72, 87-98. [15] Robinson P. et al. (1977) Am. Mineral., 62, 857-873. [16] Dodd R. T. (1981) Meteorites: A Petrologic-Chemical Synthesis, Cambridge. [17] Taylor G. J. (1987) Icarus, 69, 1-13. [18] Bevan A. W. R. and Axon H. J. (1980) EPSL, 47, 353-360. [19] Scott E. R. D. and Rajan R. S. (1981) GCA, 45, 53-67. [20] Scott E. R. D. and Rajan R. S. (1981) GCA, 45, 1959. [21] Willis J. and Goldstein J. I. (1981) Nature, 293, 126-127. [22] Smith D. G. W. and Launspach S. (1991) EPSL, 102, 79-93. [23] St"ffler D. et al. (1991) GCA, 55, 3845-3867. [24] Hutchison R. et al. (1979) Nature, 280, 116-119. [25] Wasson J. T. et al. (1995) GCA, 59, 1847-1869. [26] Scott E. R. D. et al. (1984) GCA, 48, 1741-1757. [27] Nagahara H. (1984) GCA, 48, 2581-2595. [28] Morden S. J. and Collinson D. W. (1992) EPSL, 109, 185-204. [29] Scott E. R. D. et al. (1985) Proc. LPSC 16th, in JGR, 90, D137-D148. [30] Rubin A. E. (1990) GCA, 54, 1217-1232. [31] Rubin A. E. and Wasson J. T. (1986) GCA, 50, 307-315.

  19. Decreasing of axial angular momentum of oceanic both fluid continental masses and its contribution to non-tidal acceleration of rotation of the Earth

    NASA Astrophysics Data System (ADS)

    Barkin, Yu. V.

    2009-04-01

    duration of day here makes approximately-0.52 ms/cy. Thus strengthening of redistribution of terrestrial waters and fluids in the western direction really proves to be true. These estimations are obtained at exception of the period 1997.0-1999.0 when there was rather fast spasmodic change (increase) of duration of day approximately on 0.038 ms. References [1] Barkin Yu.V. (2007) Celestial geodynamics and solution of the fundamental problems of geodesy, gravimetry and geophysics. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007), (S) - IASPEI, JSS011, p. 2149. www. iugg2007perugia.it. [2] Cheng M.R., Shum C.K. and Tapley B.D. (1997) Determination of long-periodic changes in the Earth's gravity field from satellite laser ranging observations. Journal of Geophysical research, V. 102, No. B10. pp. 22377-22390. [3] Stephenson F.R. and Morrison L.V. (1995) Long term fluctuations in the Earth's rotation:700 BC to AD 1990, Phil. Trans. R. Soc. Lond., A, 351, p. 165-202. [4] Abarca del Rio R. (1999) The influence of global warming in Earth rotation speed. Ann. Geophys., 17, 806-811. [5] Brosche P., Wunsch J., Maier-Reimer E., Segschneider J., Sundermann J. (1997) The axial angular momentum of the general circulation of the oceans. Astron. Nachr. 318, V.3, 193-199. [6] Chen J. (2005) Global mass balance an the length-of-day variation. Journal of Geophysical research, V. 110, B08404, doi: 10.1029/2004JB003474. [7] Barkin Yu.V. (2002) Explanation of endogenous activity of planets and satellites and its cyclicity. Izvestia cekzii nauk o Zemle. Rus. Acad. of Nat. Sciences, Issue 9, December 2002, M.: VINITI, pp. 45-97. In Russian.

  20. Is subduction really in the plate tectonics driving seat, or do two other global mechanisms do the driving? A review in the 'deep-keeled cratons' frame for global dynamics

    NASA Astrophysics Data System (ADS)

    Osmaston, M. F.

    2012-04-01

    how does that occur? My original proposal [1] for that function was the long-term clockwise rotation of Antarctica and its coupling to the other plates. In another contribution at this meeting [12] the observational basis for its reality is now shown to be very strong. So the conclusion is that plate tectonics has only two primary drivers - this rotation and ridge push - subduction being a wholly passive consequence. [1] Osmaston M. F. (2003) What drives plate tectonics? Slab pull, ridge push or geomagnetic torque from the CMB? A new look at the old players vis-a-vis an exciting new one. XXIII IUGG, B129, Abstr. 016795-2. [2] Osmaston M. (2005) Interrelationships between large-scale plate motions as indicators of mantle structure: new constraints on mantle modelling and compositional layout. In 3rd Workshop on "Earth's mantle composition, structure and phase transitions". http://deep.earth.free.fr/participants.php. [3] Osmaston M. F. (2006) Global tectonic actions emanating from Arctic opening in the circumstances of a two-layer mantle and a thick-plate paradigm involving deep cratonic tectospheres: the Eurekan (Eocene) compressive motion of Greenland and other examples. In Proc. ICAM IV, 2003 (ed. R. Scott & D. Thurston). OCS Study MMS 2006-003, pp.105-124: Also at ; http://www.mms.gov/alaska/icam. [4] Osmaston M. F. (2007) Cratonic keels and a two-layer mantle tested: mantle expulsion during Arabia-Russia closure linked to westward enlargement of the Black Sea, formation of the Western Alps and subduction of the Tyrrhenian (not the Ionian) Sea. XXIV IUGG, Session JSS 011 Abstr #2105, http://www.iugg2007perugia.it/webbook/. [5] Osmaston M. F. (2009) Deep cratonic keels and a 2-layer mantle? Tectonic basis for some far-reaching new insights on the dynamical properties of the Earth's mantle: example motions from Mediterranean, Atlantic-Arctic and India. Geophys. Res.Abstr 11, EGU2009-6359 (Solicited). [6] Karato S. (1986) Does partial melting reduce the creep strength

  1. Recognition of Intermediate Crust (IC), its construction and its distinctive epeirogenic behaviour: an exciting new tool for plate kinematic analysis (PKA) of the Arctic margins and western Siberia

    NASA Astrophysics Data System (ADS)

    Osmaston, M. F.

    2012-04-01

    the supposed assemblage will be geographically upside down in relation to the rest. Finally, a quick visit to the Chukchi-Bering-Alaska sector of the Arctic margin. Here, too, recognition of IC may provide a key. I suggest that northward emplacement of the Brooks Range Ophiolite at close to 170 Ma was swiftly followed by the (now) westward extraction of the Seward-Chukchi MCC assemblage to form, as IC, both the extensive Koyukuk basin system which lies south of Brooks Range and, ultimately, the Bering gap in the Pacific rim of cratonic keels, through which mantle to put at depth under the widening Eurasian Basin ocean floor has been drawn, initiating the Aleutian arc in the Palaeocene, trapping OC/IC behind it. I discuss a global reason for the initiation of the Bering gap, and its timing, in another session (GD6.1) of this meeting. [1] Osmaston M. F. (2006) Global tectonic actions emanating from Arctic opening in the circumstances of a two-layer mantle and a thick-plate paradigm involving deep cratonic tectospheres: the Eurekan (Eocene) compressive motion of Greenland and other examples. In, Proc. ICAM IV 2003 (ed. R. Scott & D. Thurston). OCS Study MMS 2006-003, pp.105-124: Also published on: http://www.mms.gov/alaska/icam [2] Osmaston M. F. (2007) Cratonic keels and a two-layer mantle tested: mantle expulsion during Arabia-Russia closure linked to westward enlargement of the Black Sea, formation of the Western Alps and subduction of the Tyrrhenian (not the Ionian) Sea. XXIV IUGG, Session JSS 011 Abstr #2105. http://www.iugg2007perugia.it/webbook/. [3] Osmaston M. F. (2009) Deep cratonic keels and a 2-layer mantle? Tectonic basis for some far-reaching new insights on the dynamical properties of the Earth's mantle: example motions from Mediterranean, Atlantic-Arctic and India. Geophys. Res. Abst. 11, EGU2009-6359 (Solicited). [4] Karato S. (1986) Does partial melting reduce the creep strength of the upper mantle? Nature 319, 309-310. [5] Hirth G. & Kohlstedt D. L

  2. Did clockwise rotation of Antarctica cause the break-up of Gondwanaland? An investigation in the 'deep-keeled cratons' frame for global dynamics

    NASA Astrophysics Data System (ADS)

    Osmaston, M. F.

    2012-04-01

    considered a major agent in plate motion dynamics for the period during which East Antarctica, or any other sufficiently deep-keeled craton previously, was located at one of the Earth's poles. [1] Osmaston M. F. (2006) Global tectonic actions emanating from Arctic opening in the circumstances of a two-layer mantle and a thick-plate paradigm involving deep cratonic tectospheres: the Eurekan (Eocene) compressive motion of Greenland and other examples. In Proc. ICAM IV, 2003 (ed. R. Scott & D. Thurston). OCS Study MMS 2006-003, p.105-124: Also at: http://www.mms.gov/alaska/icam. [2] Osmaston M. (2005) Interrelationships between large-scale plate motions as indicators of mantle structure: new constraints on mantle modelling and compositional layout. In 3rd Workshop on "Earth's mantle composition, structure and phase transitions" St Malo, France. http://deep.earth.free.fr/participants.php. [3] Osmaston M. F. (2007) Cratonic keels and a two-layer mantle tested: mantle expulsion during Arabia-Russia closure linked to westward enlargement of the Black Sea, formation of the Western Alps and subduction of the Tyrrhenian (not the Ionian) Sea. XXIV IUGG, Session JSS 011, Abstr #2105 http://www.iugg2007perugia.it/webbook/. [4] Osmaston M. F. (2009) Deep cratonic keels and a 2-layer mantle? Tectonic basis for some far-reaching new insights on the dynamical properties of the Earth's mantle: example motions from Mediterranean, Atlantic-Arctic and India. Geophys. Res. Abstr. 11, EGU2009-6359 (Solicited). [5] Karato S. (1986) Does partial melting reduce the creep strength of the upper mantle? Nature 319, 309-310. [6] Hirth G. & Kohlstedt D. L. (1996) Water in the oceanic upper mantle: implication for rheology, melt extraction, and the evolution of the lithosphere. EPSL 144, 93-108. [7] Osmaston M. F. (2010) On the actual variety of plate dynamical mechanisms and how mantle evolution affected them through time, from core formation to the Indian collision. Geophys. Res. Abstr. 12, EGU2010

  3. Prediction and explanation of increases of mean sea levels in northern hemisphere, in southern hemisphere and all ocean of the Earth

    NASA Astrophysics Data System (ADS)

    Barkin, Yu. V.

    2009-04-01

    -05-92507. References [1] Barkin Yu.V. (2002) An explanation of endogenous activity of planets and satellites and its cyclisity, Isvestia sekcii nauk o Zemle Rossiiskoi akademii ectestvennykh nauk, Vyp. 9, M., VINITI, 45-97. In Russian. [2] Barkin Yu.V. (2005) Oscillations of the Earth core, new oceanic tides and dynamical consequences. Materials of XI International Scientific Conference "Structure, geodynamics and mineral genetic processes in lithosphere" (September, 20-22 2005, Syktyvkar, Russia), Publisher of Geology Institute of Komi SC of Ural Section of RAS, Syktyvkar, pp. 26-28. In Russian. [3] Barkin Yu.V. (2007) Forced redistribution of air masses between southern and northern hemispheres of the Earth. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007), (A)-IAGA, JAS008, p. 326. www. iugg2007perugia.it. [4] Burlutsky R.F. Determination of the global concentration of pair on the ground pressure. Materials of Sagitov's readings. M., SAI, MSU, 2007, www.sai.msu.ru.

  4. Global Geological Map of Venus

    NASA Astrophysics Data System (ADS)

    Ivanov, M. A.

    2008-09-01

    units is ~81.7% of the map area, whereas the younger units cover ~14.1% of the surface. Depending upon the estimates of T (750 Ma [36], 500 Ma [37], 300 Ma [38]), duration of Fortunian Period can be from 300 m.y (T=750 Ma) to 120 m.y (T=300 Ma). The minimum integrated resurfacing rate (both volcanic and tectonic) at this time was from ~1.2 to ~3.1 km2/y. Duration of Atlian Period is estimated to be from 750 to 300 m.y and the integrated resurfacing rate during this period could be from ~0.2 to ~0.4 km2/y. Such a significant drop of the resurfacing rates suggests that Fortunian and Atlian periods correspond to two different geodynamic regimes that probably were related to different regimes of mantle convection and lithospheric properties. References: 1) Basilevsky, A. T. and J.W. Head, PSS, 43, 1523, 1995; 2) Basilevsky, A.T. and J.W. Head, PSS, 48, 75, 2000 3) DeShon, H.R. et al., JGR, 105, 6983, 2000; 4) Head, J.W. et al., JGR, 97, 13153, 1992; 5) Solomon, S.C. et al., JGR, 97, 13199, 1992; 6) Squyres, S.W. et al., JGR, 97, 13579, 1992; 7) Stofan, E. R. et al., JGR, 97, 13347, 1992; 8) Guest, J.E., and E.R., Icarus139, 56, 1999; 9) Basilevsky, A.T.,et al., in: Venus II, S.W. Bougher et al. eds., Univ. Arizona Press 1047, 1997; 10) Head, J.W. and A.T. Basilevsky, Geology, 26, 35, 1998; 11) Ivanov, M.A. and J.W. Head, JGR, 106, 17515, 2001; 12) Price, M. and J., Nature, 372, 756, 1994; 13) Price, M. et al., JGR, 101, 4657, 1996 14) Namiki, N. and S.C. Solomon, Science, 265, 929, 1994 15) Parmentier, E.M. and P.C. Hess, GRL, 19, 2015, 1992; 16) Head, J.W. et al., PSS, 42, 803, 1994; 17) Turcotte, D.L., JGR, 98, 127061, 1993; 18) Arkani-Hamed, J. and M.N. Toksoz, PEPI, 34, 232, 1984; 19) Solomon, S.C, LPSC (Abstr.), XXIV, 1331, 1993; 20) Phillips R.J. and V.L. Hansen, Science, 279, 1492, 1998; 21) Solomatov, S.V. and L.-N. Moresi, JGR, 101, 4737, 1996; 22) Bender, K.C., et al., USGS Map I-2620, 2000; 23) Rosenberg, E. and G. E. McGill, USGS Map I-2721, 2001; 24) Ivanov, M

  5. Warming: mechanism and latitude dependence

    NASA Astrophysics Data System (ADS)

    Barkin, Yury

    2010-05-01

    asymmetry in decade variations of temperatures in northern and southern hemispheres (smaller variations in a southern hemisphere). References [1] Barkin Yu.V. (2002) An explanation of endogenous activity of planets and satellites and its cyclisity. Isvestia sekcii nauk o Zemle Rossiiskoi akademii ectestvennykh nauk. Vyp. 9, M., VINITI, pp. 45-97. In Russian. [2] Barkin Yu.V. (2009) Moons and planets: mechanism of their life. Proceedings of International Conference 'Astronomy and World Heritage: across Time and Continents' (Kazan, 19-24 August 2009). KSU, pp. 142-161. [3] Barkin Yu.V. (2004) Dynamics of the Earth shells and variations of paleoclimate. Proceedings of Milutin Milankovitch Anniversary Symposium 'Paleoclimate and the Earth climate system' (Belgrade, Serbia, 30 August - 2 September, 2004). Belgrade, Serbian Academy of Sciences and Art, pp. 161-164. [4] Barkin Yu.V. (2007) Inversion of periodic and trend variations of climate in opposite hemispheres of the Earth and their mechanism. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007) (P) - IAPSO, JPS001 'Interannual and Interdecadal Climate Variability', p. 1674. www. iugg2007perugia.it. [5] Barkin Yu.V. (2008) Secular polar drift of the core in present epoch: geodynamical and geophysical consequences and confirmations. General and regional problems of tectonics and geodynamics. Materials of XLI Tectonic Conference. V. 1. -M.:GEOS. p. 55-59. In Russian. [6] Yang Wang, Jiyang Wangand Zongji Ma (1998) On the asymmetric distribution of heat loss from the Earth's interior. Chinese Science Bulletin, Volume 43, Number 18 , p. 1566-1570.

  6. S-N secular ocean tide: explanation of observably coastal velocities of increase of a global mean sea level and mean sea levels in northern and southern hemispheres and prediction of erroneous altimetry velocities

    NASA Astrophysics Data System (ADS)

    Barkin, Yury

    2010-05-01

    scientific readings. A deep structure. Geodynamics. A thermal field of the Earth. Interpretation of geophysical fields» (Ekaterinburg, 6 - 10 July, 2009). pp. 27-31. In Russian. [7] Barkin Yu.V. (2009) The mechanism of translational displacements of the core of the Earth at inversion molten and solidification of substance at core-mantle-boundary in opposite hemispheres. EGU General Assembly (Vienna, Austria, 19-24 April 2009). Geophysical Research Abstracts, Volume 11, 2009, abstract # EGU2009-6241. [8] Barkin Yu.V. (2007) Forced redistribution of air masses between southern and northern hemispheres of the Earth. Proceedings of IUGG XXIV General Assembly, Perugia, Italy 2007: Earth: Our Changing Planet (Perugia, Italy, July 2-13, 2007), (A)-IAGA, JAS008, p. 326. www. iugg2007perugia.it. [9] Burlutsky R.F. (2007) Determination of the global concentration of pair on the ground pressure. Materials of Sagitov's readings. M., SAI, MSU, 2007, www.sai.msu.ru. [10] Barkin Yu.V., J.M. Ferrandiz, Garcia D. (2008) Contrast secular variations of the mean atmospheric presure and mean sea level in northern and southern hemispheres of the Earth. Proceedings of International Symposium "Topical Problems of Nonlinear Wave Physics-2008" (NWP-2008). Session 3. p. 15-16. [11] Barkin Yu.V. and S. Jin (2007) On variations of the mean radius of the Northern and Southern Hemispheres of the Earth. EGU General Assembly (Vienna, Austria, 15-20 April 2007). Geoph. Res. Abstr., Vol. 9, abstr. # EGU07-A-08183. [12] Miller L. and B.C. Douglas, Mass and volume contributions to twentieth-century global sea level rise. Nature, v. 428, 25 March 2004, pp. 406-409. [13] Jevreeva S., Grinsted A., Moore J.C., Holgate S. (2006) Nonlinear trends and multiyear cycles in sea level records. Journal Geophysical Research, v. 111, C09012, doi: 10.1029/2005JC0032 29, 2006.

  7. Archaeological Geophysics in Israel: Past, Present and Future

    NASA Astrophysics Data System (ADS)

    Eppelbaum, L. V.

    2009-04-01

    . Application of multifocusing seismic processing to the GPR data analysis. Proceed. of the Symp. on the Application of Geophysics to Engineering and Environmental Problems, Hyatt Regency Crystal City, Arlington, USA, 597-606. Borradaile, G. J., 2003. Viscous magnetization, archaeology and Bayesian statistics of small samples from Israel and England. Geophysical Research Letters, 30 (10), 1528, doi:10.1029/2003GL016977. Boyce, J.I., Reinhardt, E.G., Raban, A., and Pozza, M.R., 2004. The utility of marine magnetic surveying for mapping buried hydraulic concrete harbour structures: Marine Magnetic Survey of a Submerged Roman Harbour, Caesarea Maritima, Israel. The International Journal of Nautical Archaeology, 33, 1, 122-136. Bruins, H.J., van der Plicht, J., and Mazar, A., 2003. 14C dates from Tel-Rehov: Iron-age chronology, Pharaohs and Hebrew kings. Science, 300, 315-318. Daniels, J., Blumberg, D.J., Vulfson, L.D., Kotlyar, A.L., Freiliker, V., Ronen, G., and Ben-Asher, J., 2003. Microwave remote sensing of physically buried objects in the Negev Desert: implications for environmental research. Remote Sensing of Environment, 86, 243-256, 2003. Dolphin, L.T., 1981. Geophysical methods for archaeological surveys in Israel. Stanford Research International, Menlo Park, Calif., USA, 7 pp. Ellenblum, R., Marco, M., Agnon, A., Rockwell, T., and Boas, A., 1998. Crusader castle torn apart by earthquake at dawn, 20 May 1202. Geology, 26, No. 4, 303-306. Eppelbaum, L.V., 1999. Quantitative interpretation of resistivity anomalies using advanced methods developed in magnetic prospecting. Trans. of the XXIV General Assembly of the Europ. Geoph. Soc., Strasburg 1 (1), p.166. Eppelbaum, L.V., 2000a. Detailed geophysical investigations at archaeological sites. In: (Ed. A. Nissenbaum), Relation between archaeology and other scientific disciplines, Collection of Papers, Weitzman Inst., Rehovot, Israel, No.8, 39-54 (in Hebrew). Eppelbaum, L.V., 2000b. Applicability of geophysical methods for