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Sample records for great meteor seamount

  1. Evidence for age and evolution of Corner seamounts and Great Meteor seamount chain from multibeam bathymetry

    NASA Technical Reports Server (NTRS)

    Tucholke, Brian E.; Smoot, N. Christian

    1990-01-01

    The morphology of the Corner and Cruiser seamounts is discussed and the apparent age of seamount geomorphic features that are thought to have formed at sea level is derived. High-resolution, multibeam bathymetry of the seamounts shows geomorphic features such as guyots and terraces. The pattern of volcanism is consistent with the sequential formation of the New England, Corner, and Great Meteor chain seamounts above the New England hotspot. However, Late Cretaceous and Cenozoic absolute motion of the African plate over the hotspot differs significantly from predictions of the existing models. The derived age pattern of volcanism indicates formation of the Corner seamounts at ca. 80 Ma to 76 Ma.

  2. Evidence for age and evolution of Corner seamounts and Great Meteor seamount chain from multibeam bathymetry

    NASA Astrophysics Data System (ADS)

    Tucholke, Brian E.; Smoot, N. Christian

    1990-10-01

    The morphology of the Corner and Cruiser seamounts is discussed and the apparent age of seamount geomorphic features that are thought to have formed at sea level is derived. High-resolution, multibeam bathymetry of the seamounts shows geomorphic features such as guyots and terraces. The pattern of volcanism is consistent with the sequential formation of the New England, Corner, and Great Meteor chain seamounts above the New England hotspot. However, Late Cretaceous and Cenozoic absolute motion of the African plate over the hotspot differs significantly from predictions of the existing models. The derived age pattern of volcanism indicates formation of the Corner seamounts at ca. 80 Ma to 76 Ma.

  3. Crowdsourcing, the great meteor storm of 1833, and the founding of meteor science.

    PubMed

    Littmann, Mark; Suomela, Todd

    2014-06-01

    Yale science professor Denison Olmsted used crowdsourcing to gather observations from across the United States of the unexpected deluge of meteors on 13 November 1833--more than 72,000/h. He used these observations (and newspaper accounts and correspondence from scientists) to make a commendably accurate interpretation of the meteor storm, overturning 2100 years of erroneous teachings about shooting stars and establishing meteor science as a new branch of astronomy. Olmsted's success was substantially based on his use of newspapers and their practice of news pooling to solicit observations from throughout the country by lay and expert observers professionally unaffiliated with Yale College and him. In today's parlance, Olmsted was a remarkably successful early practitioner of scientific crowdsourcing, also known as citizen science. He may have been the first to use mass media for crowdsourcing in science. He pioneered many of the citizen-science crowdsourcing practices that are still in use today: an open call for citizen participation, a clearly defined task, a large geographical distribution for gathering data and a rapid response to opportunistic events. Olmsted's achievement is not just that he used crowdsourcing in 1833 but that crowdsourcing helped him to advance science significantly. PMID:24917173

  4. Crowdsourcing, the great meteor storm of 1833, and the founding of meteor science.

    PubMed

    Littmann, Mark; Suomela, Todd

    2014-06-01

    Yale science professor Denison Olmsted used crowdsourcing to gather observations from across the United States of the unexpected deluge of meteors on 13 November 1833--more than 72,000/h. He used these observations (and newspaper accounts and correspondence from scientists) to make a commendably accurate interpretation of the meteor storm, overturning 2100 years of erroneous teachings about shooting stars and establishing meteor science as a new branch of astronomy. Olmsted's success was substantially based on his use of newspapers and their practice of news pooling to solicit observations from throughout the country by lay and expert observers professionally unaffiliated with Yale College and him. In today's parlance, Olmsted was a remarkably successful early practitioner of scientific crowdsourcing, also known as citizen science. He may have been the first to use mass media for crowdsourcing in science. He pioneered many of the citizen-science crowdsourcing practices that are still in use today: an open call for citizen participation, a clearly defined task, a large geographical distribution for gathering data and a rapid response to opportunistic events. Olmsted's achievement is not just that he used crowdsourcing in 1833 but that crowdsourcing helped him to advance science significantly.

  5. Spionidae (Polychaeta: Canalipalpata: Spionida) from seamounts in the NE Atlantic.

    PubMed

    Meißner, Karin; Bick, Andreas; Guggolz, Theresa; Götting, Miriam

    2014-01-01

    Spionidae (Polychaeta) collected from seamounts in the Atlantic Ocean were studied. Altogether six species were found of which two are new to science and one belongs to a new genus. Aonidella cf. dayi Maciolek in López-Jamar, 1989 and Glandulospio orestes gen. et sp. nov. were the most common species and occurred on both the Great and Little Meteor Seamount, the Irving Seamount and the Hyeres Seamount. Laonice norgensis Sikorski, 2003 and Malacoceros jirkovi Sikorski, 1992 have a wider distribution in the North Atlantic, including the Mediterranean Sea in case of L. norgensis. Aonides selvagensis Brito, Núñez and Riera, 2006 is only known from the Macaronesian Region. Dipolydora paracaulleryi sp. nov. has been collected from both the Great and Little Meteor Seamounts. All species are compared with morphological similar species and their taxonomy is discussed. Detailed descriptions are provided for the species new to science and descriptions of the previously known species are amended. Accompanying histological studies revealed the presence of very strong dorsoventral musculature in A. cf. dayi and for G. orestes gen. et sp. nov. the presence of glandular organs in the middle body region. Laonice maciolekae Aguirrezabalaga & Ceberio, 2005 was found to be a junior synonym of L. appellöfi Söderström, 1920 and is formally synonymised. Molecular data suggest gene flow between seamounts and autochthonous as well as allochthonous larval recruitment for different species. The results of previous studies by other authors, that polychaete communities of the North Atlantic Seamounts are characterized by low diversity, low rates of endemism, and the predominance of widely distributed (and cosmopolitan) species is not corroborated by our results.  PMID:24869536

  6. Spionidae (Polychaeta: Canalipalpata: Spionida) from seamounts in the NE Atlantic.

    PubMed

    Meißner, Karin; Bick, Andreas; Guggolz, Theresa; Götting, Miriam

    2014-04-10

    Spionidae (Polychaeta) collected from seamounts in the Atlantic Ocean were studied. Altogether six species were found of which two are new to science and one belongs to a new genus. Aonidella cf. dayi Maciolek in López-Jamar, 1989 and Glandulospio orestes gen. et sp. nov. were the most common species and occurred on both the Great and Little Meteor Seamount, the Irving Seamount and the Hyeres Seamount. Laonice norgensis Sikorski, 2003 and Malacoceros jirkovi Sikorski, 1992 have a wider distribution in the North Atlantic, including the Mediterranean Sea in case of L. norgensis. Aonides selvagensis Brito, Núñez and Riera, 2006 is only known from the Macaronesian Region. Dipolydora paracaulleryi sp. nov. has been collected from both the Great and Little Meteor Seamounts. All species are compared with morphological similar species and their taxonomy is discussed. Detailed descriptions are provided for the species new to science and descriptions of the previously known species are amended. Accompanying histological studies revealed the presence of very strong dorsoventral musculature in A. cf. dayi and for G. orestes gen. et sp. nov. the presence of glandular organs in the middle body region. Laonice maciolekae Aguirrezabalaga & Ceberio, 2005 was found to be a junior synonym of L. appellöfi Söderström, 1920 and is formally synonymised. Molecular data suggest gene flow between seamounts and autochthonous as well as allochthonous larval recruitment for different species. The results of previous studies by other authors, that polychaete communities of the North Atlantic Seamounts are characterized by low diversity, low rates of endemism, and the predominance of widely distributed (and cosmopolitan) species is not corroborated by our results. 

  7. Meteor Showers.

    ERIC Educational Resources Information Center

    Kronk, Gary W.

    1988-01-01

    Described are the history, formation, and observing techniques of meteors and comets. Provided are several pictures, diagrams, meteor organizations and publications, and meteor shower observation tables. (YP)

  8. Practical Meteor Stream Forecasting

    NASA Technical Reports Server (NTRS)

    Cooke, William J.; Suggs, Robert M.

    2003-01-01

    Inspired by the recent Leonid meteor storms, researchers have made great strides in our ability to predict enhanced meteor activity. However, the necessary calibration of the meteor stream models with Earth-based ZHRs (Zenith Hourly Rates) has placed emphasis on the terran observer and meteor activity predictions are published in such a manner to reflect this emphasis. As a consequence, many predictions are often unusable by the satellite community, which has the most at stake and the greatest interest in meteor forecasting. This paper suggests that stream modelers need to pay more attention to the needs of this community and publish not just durations and times of maxima for Earth, but everything needed to characterize the meteor stream in and out of the plane of the ecliptic, which, at a minimum, consists of the location of maximum stream density (ZHR) and the functional form of the density decay with distance from this point. It is also suggested that some of the terminology associated with meteor showers may need to be more strictly defined in order to eliminate the perception of crying wolf by meteor scientists. An outburst is especially problematic, as it usually denotes an enhancement by a factor of 2 or more to researchers, but conveys the notion of a sky filled with meteors to satellite operators and the public. Experience has also taught that predicted ZHRs often lead to public disappointment, as these values vastly overestimate what is seen.

  9. Introduction to Seamount Special Section

    NASA Astrophysics Data System (ADS)

    Watts, A. B.

    1984-12-01

    This special section is the outcome of a symposium held at the Lamont-Doherty Geological Observatory November 17-19, 1982, on the origin and evolution of seamounts. The topic for the symposium arose from the realization that although there is now a wealth of new ideas on the geology, geophysics, and geochemistry of the ocean floor, the study of seamounts has been relatively neglected despite their great importance to plate tectonics. One of the most interesting features of the ocean floor is the large number of small volcanoes or seamounts. Usually, these features are circular in plan view and have a sharp summit. There has been extensive debate in the literature about the significance of the different morphological types of seamounts. A traditional view has been that flattopped seamounts (e.g., guyots) formed as a result of subaerial erosion when the volcanoes were above sea level. Seamounts covered by fringing reefs or sediments (e.g., atolls), on the other hand, are believed to have formed when the original volcanic foundation subsided below sea level.

  10. Major and minor element geochemistry of deep-sea sediments in the Azores Platform and southern seamount region.

    PubMed

    Palma, Carla; Oliveira, Anabela; Valença, Manuela; Cascalho, João; Pereira, Eduarda; Lillebø, Ana I; Duarte, Armando C; Pinto de Abreu, Manuel

    2013-10-15

    The Azores Platform and the Irving and Great Meteor seamounts south of the archipelago (38°N-29°N) have rarely been studied geochemically, a fact which is surprising given that they represent the south-eastern limit of region V outlined in the Convention for the Protection of the Marine Environment of the North-East Atlantic (OSPAR Convention). The main aim of the present work was therefore to characterise the spatial variability of major and minor elements in deep-sea sediment cores from these two regions. XRD and geochemical analyses revealed that whereas the Azores Platform sediments are composed of a mixture of biogenic and detrital volcanic material, those at the seamounts are characterised by carbonated biogenic remains. The latter sediments were found to contain very low amounts of volcanic or hydrothermal detrital material, being almost entirely comprised of CaCO3 (more than 80%). PMID:23896401

  11. Major and minor element geochemistry of deep-sea sediments in the Azores Platform and southern seamount region.

    PubMed

    Palma, Carla; Oliveira, Anabela; Valença, Manuela; Cascalho, João; Pereira, Eduarda; Lillebø, Ana I; Duarte, Armando C; Pinto de Abreu, Manuel

    2013-10-15

    The Azores Platform and the Irving and Great Meteor seamounts south of the archipelago (38°N-29°N) have rarely been studied geochemically, a fact which is surprising given that they represent the south-eastern limit of region V outlined in the Convention for the Protection of the Marine Environment of the North-East Atlantic (OSPAR Convention). The main aim of the present work was therefore to characterise the spatial variability of major and minor elements in deep-sea sediment cores from these two regions. XRD and geochemical analyses revealed that whereas the Azores Platform sediments are composed of a mixture of biogenic and detrital volcanic material, those at the seamounts are characterised by carbonated biogenic remains. The latter sediments were found to contain very low amounts of volcanic or hydrothermal detrital material, being almost entirely comprised of CaCO3 (more than 80%).

  12. Meteor44 Video Meteor Photometry

    NASA Technical Reports Server (NTRS)

    Swift, Wesley R.; Suggs, Robert M.; Cooke, William J.

    2004-01-01

    Meteor44 is a software system developed at MSFC for the calibration and analysis of video meteor data. The dynamic range of the (8bit) video data is extended by approximately 4 magnitudes for both meteors and stellar images using saturation compensation. Camera and lens specific saturation compensation coefficients are derived from artificial variable star laboratory measurements. Saturation compensation significantly increases the number of meteors with measured intensity and improves the estimation of meteoroid mass distribution. Astrometry is automated to determine each image's plate coefficient using appropriate star catalogs. The images are simultaneously intensity calibrated from the contained stars to determine the photon sensitivity and the saturation level referenced above the atmosphere. The camera s spectral response is used to compensate for stellar color index and typical meteor spectra in order to report meteor light curves in traditional visual magnitude units. Recent efforts include improved camera calibration procedures, long focal length 'streak' meteor photometry and two-station track determination. Meteor44 has been used to analyze data from the 2001, 2002 and 2003 MSFC Leonid observational campaigns as well as several lesser showers. The software is interactive and can be demonstrated using data from recent Leonid campaigns.

  13. Meteor44 Video Meteor Photometry

    NASA Technical Reports Server (NTRS)

    Swift, Wesley R.; Suggs, Robert M.; Cooke, William J.

    2004-01-01

    Meteor44 is a software system developed at MSFC for the calibration and analysis of video meteor data. The dynamic range of the (8bit) video data is extended by approximately 4 magnitudes for both meteors and stellar images using saturation compensation. Camera and lens specific saturation compensation coefficients are derived from artificial variable star laboratory measurements. Saturation compensation significantly increases the number of meteors with measured intensity and improves the estimation of meteoroid mass distribution. Astrometry is automated to determine each image s plate coefficient using appropriate star catalogs. The images are simultaneously intensity calibrated from the contained stars to determine the photon sensitivity and the saturation level referenced above the atmosphere. The camera s spectral response is used to compensate for stellar color index and typical meteor spectra in order to report meteor light curves in traditional visual magnitude units. Recent efforts include improved camera calibration procedures, long focal length "streak" meteor photome&y and two-station track determination. Meteor44 has been used to analyze data from the 2001.2002 and 2003 MSFC Leonid observational campaigns as well as several lesser showers. The software is interactive and can be demonstrated using data from recent Leonid campaigns.

  14. Can seamounts provide a good habitat for polychaete annelids? Example of the northeastern Atlantic seamounts

    NASA Astrophysics Data System (ADS)

    Surugiu, Victor; Dauvin, Jean-Claude; Gillet, Patrick; Ruellet, Thierry

    2008-11-01

    Two seamount groups in the northeastern Atlantic were investigated during the 1980s and 1990s: the first was located along the Iberian and African coasts (Galicia, to the north of Portugal; and the Ampere, Gorringe, Josephine and Seine banks near the Madeira-Canary Islands) and the second was located offshore of the southern part of the Azores Islands, included the Atlantis, Hyeres, Irving, Meteor and Plato banks. Among the invertebrates, Annelida, specifically Polychaeta, were studied as surrogates for the biogeographical relationship between coastal and mid-oceanic seamounts in the northeastern Atlantic and the fauna in these areas. The dominant families were Onuphidae (27.46%), Syllidae (18.23%), Eunicidae (15.65%), Amphinomidae (11.45%) and Nereididae (5.61%), representing 78.4% of the total fauna. Data analyses clearly distinguished two seamount groups, one for coastal seamounts and the other offshore. Although the species distinguished and the family composition at the sampled sites were different (i.e., most diversified at the Josephine site and most impoverished at the Irving site), no coastal/offshore faunal impoverishment gradient could be identified. Thus, it seems that seamount environments do not favour any relationship between planktotrophic development and the direct development of polychaetes. Though the number of apparent endemic species was low (<7%), it remained in keeping with other invertebrate groups. Still, while seamounts may well encourage oceanic biodiversity in some zoological groups, this was clearly not the case for the polychaetes. We offer two explanations for this paradox: pelagic productivity and local environmental conditions.

  15. The history of meteors and meteor showers

    NASA Astrophysics Data System (ADS)

    Hughes, David W.

    The history of meteors and meteor showers can effectively start with the work of Edmond Halley who overcome the Aristotelean view of meteors as being an upper atmospheric phenomenon and introduced their extraterrestrial nature. Halley also estimated their height and velocity. The observations of the Leonids in 1799, 1833 and 1866 established meteoroids as cometary debris. Two red herrings were caught — fixed radiants and hyperbolic velocities. But the 1890 to 1950 period with two-station meteor photography, meteor spectroscopy and the radar detection of meteors saw the subject well established.

  16. Meteor Beliefs Project: ``Year of Meteors''

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair; Drobnock, George J.; Gheorghe, Andrei Dorian

    2011-10-01

    We present a discussion linking ideas from a modern music album by Laura Veirs back to a turbulent time in American history 150 years ago, which inspired poet Walt Whitman to compose his poem "Year of Meteors", and the meteor beliefs of the period around 1859-1860, when collection of facts was giving way to analyses and theoretical explanations in meteor science.

  17. The Meteor Meter.

    ERIC Educational Resources Information Center

    Eggensperger, Martin B.

    2000-01-01

    Introduces the Meteor Scatter Project (MSP) in which high school students build an automated meteor observatory and learn to monitor meteor activity. Involves students in activities such as radio frequency survey, antenna design, antenna construction, manual meteor counts, and computer board configuration and installation. (YDS)

  18. Google for Seamounts

    NASA Astrophysics Data System (ADS)

    Staudigel, D.; Minnett, R.; Koppers, A. A.; Staudigel, H.; Konter, J.

    2006-12-01

    The Seamount Catalog (SC) under http://earthref.org is a hub for a variety of data. It has been growing steadily since its launch, and now has records for thousands of seamounts, each with carefully prepared maps, data entries, and large volumes of multibeam data. Until recently data have been accessible through searches based on their names, regions or location. Results from these searches are presented in a list of seamounts, each with data records that are associated with them. These traditional search/retrieval methods, however, can be overwhelming for the user, in particular, when trying to find the relevant seamount data from very large (text) listings. To solve this, we have started to use the "Google Maps" tool to create a visually intuitive web interface that does justice to the large data load and makes it easier for the user to search for and download data. Analogous to "Google Maps," a typical search begins with the user offering some basic information about the search area such as the seamount trail, region or ocean name, and the map automatically pans to the area and displays the user with seamounts in the region. Built into our tool is a full-coverage, high- resolution altimetry/bathymetry world map based on Smith and Sandwell (1997), merged with multibeam and USGS SRTM2 satellite data where available. With this basemap, the user can pan around the seamounts, looking for the seamount they are interested in, making use of Google-style balloons that contain supplemental information. Upon finding the appropriate seamount, the seamount can be selected and used as a text-based database query. Alternatively, the user can choose to zoom in, allowing them to see samples exactly where they were taken. Selecting these points offers more information about them, including direct download links for the data, and perhaps online plotting and manipulation tools. The most powerful aspect of this interface is its wide applicability. With just a few simple, server

  19. Abundance of litter on Condor seamount (Azores, Portugal, Northeast Atlantic)

    NASA Astrophysics Data System (ADS)

    Pham, C. K.; Gomes-Pereira, J. N.; Isidro, E. J.; Santos, R. S.; Morato, T.

    2013-12-01

    Marine litter is an emerging problem for the world's ocean health but little is known on its distribution and abundance on seamounts and how it affects deep-sea ecosystems. The scientific underwater laboratory set up on Condor seamount offered an ideal case study for the first documentation of litter distribution on a shallow seamount with historical fishing. A total of 48 video transects deployed on the summit (n=45) and the northern flank (n=3) covered an area of 0.031 and 0.025km2, respectively, revealing 55 litter items. Litter density on the summit was 1439 litter items km-2, whilst on the deeper northern flank, estimates indicate densities of 397 litter items km-2. Lost fishing line was the dominant litter item encountered on both areas (73% of total litter on the summit and 50% on northern flank), all being entirely or partly entangled in the locally abundant gorgonians Dentomuricea cf. meteor and Viminella flagellum. Other items included lost weights, anchors and glass bottles. The predominance of lost fishing gear identifies the source of litter on Condor seamount as exclusively ocean-based and related to fishing activities. Abundance of litter on the Condor seamount was much lower than that reported from other locations closer to populated areas.

  20. Quadrantid Meteor, 2013

    NASA Video Gallery

    An allsky camera in New Mexico captured a brief video of this Quadrantid fireball meteor on Jan. 3, 2013 at 2:04 a.m. EST. The Quadrantid meteor shower occurs each January and derives its name from...

  1. Catalogue of representative meteor spectra

    NASA Astrophysics Data System (ADS)

    Vojáček, V.; Borovička, J.; Koten, P.; Spurný, P.; Štork, R.

    2016-01-01

    We present a library of low-resolution meteor spectra that includes sporadic meteors, members of minor meteor showers, and major meteor showers. These meteors are in the magnitude range from +2 to ‑3, corresponding to meteoroid sizes from 1 mm to10 mm. This catalogue is available online at the CDS for those interested in video meteor spectra.

  2. Catalogue of representative meteor spectra

    NASA Astrophysics Data System (ADS)

    Vojáček, V.; Borovička, J.; Koten, P.; Spurný, P.; Štork, R.

    2016-01-01

    We present a library of low-resolution meteor spectra that includes sporadic meteors, members of minor meteor showers, and major meteor showers. These meteors are in the magnitude range from +2 to -3, corresponding to meteoroid sizes from 1 mm to10 mm. This catalogue is available online at the CDS for those interested in video meteor spectra.

  3. Apparatus for photographing meteors

    NASA Technical Reports Server (NTRS)

    Harvey, G. A. (Inventor)

    1973-01-01

    Apparatus for photographing meteors in a selected area of the sky is described. A photomultiplier is pointed in the direction of the area. When a meteor passes through the area the signal output of the photomultiplier increases. Means are provided that activate a camera, pointed at the area, in response to an increased signal from the photomultiplier. Hence, the camera photographs the selected are only while meteors are likely to be passing through the area.

  4. The Eratosthenes Seamount - Eastern Mediterranean

    NASA Astrophysics Data System (ADS)

    Ehrhardt, A.; Schnabel, M.; Damm, V.

    2012-04-01

    The Eratosthenes Seamount forms a prominent landmark in the Eastern Mediterranean. It is located south of Cyprus with the Levantine Basin on its eastern side, the Herodotus Basin on its western side and the Nile Cone south of the seamount. The Eratosthenes Seamount rises up to 750 m below sea surface and is about 1200 m higher than the surrounding seafloor of the Levantine Basin and the Nile Cone sediments. The Eratosthenes Seamount is considered as a continental fragment of the former African-Nubian Plate that was rifted to its present position relative to Africa during the formation of the Tethyan Ocean. In 2010 a detailed geophysical survey was carried out in the area of the Eratosthenes Seamount by the Federal Institute for Geosciences and Natural Resources of Germany including multichannel seismic (MCS), refraction seismics, magnetic, gravity and magnetotelluric data acquisition. First results show a highly deformed seamount, with a plateau-like top that is impacted by west-east trending graben formation. The slopes of the seamount are eroded showing deep incised ripple patterns and recent submarine landslides. The Eratosthenes Seamount produces also a prominent magnetic and gravity anomaly, both supporting its uniqueness in the area of the Eastern Mediterranean. Velocity information by refraction seismic modeling, as well as the models of the magnetic and gravity data show evidence for a volcanic core of the seamount with carbonate layers on top of the volcanic core. The slopes of the seamount terminate against a conspicuous rim-like escarpment that forms in addition the northern and western termination of the Messinian Evaporites in the study area. The MCS and refraction seismic data show a very deep Levantine Basin with maximum acoustic basement depths of 12 to 14 km very close to the slope of the Eratosthenes Seamount. The deepest sediments resolved by the MCS data are of Lower Cretaceous to Jurassic age. The refraction seismic model shows a 14 km thick

  5. Rare Double Quadrantid Meteor Sighting

    NASA Video Gallery

    The wide-field meteor camera at NASA's Marshall Space Flight Center recorded these two simultaneous Quadrantid meteors on Jan. 4 at approximately 5 a.m. EST. Moving at 92,000 mph, the meteors flash...

  6. Global distribution of seamounts from Seasat profiles

    NASA Technical Reports Server (NTRS)

    Craig, Claire H.; Sandwell, David T.

    1988-01-01

    A new measurement techique based on a model of a Gaussian seamount loading a thin elastic lithosphere was developed to analyze seamounts that, until then, were not surveyed or seamounts with poor bathymetric coverage. The model predicts that the seamount diameter is equal to the peak-to-trough distance along the vertical deflection profile and that the flexural diameter of a seamount is related to the age of the lithosphere when the seamount formed. This model also suggests that these two measurements are relatively insensitive to the cross-track location from the seamount. These model predictions were confirmed using Seasat altimeter profiles crossing 14 surveyed seamounts in the Pacific. The analysis of the seamount distribution indicated considerable variations in population density and type across the oceans. Most notable among them are the absence of seamounts in the Atlantic, variations in population density across large fracture zones in the Pacific, and the prevalence of small signatures in the Indian Ocean.

  7. Meteor Beliefs Project: Introduction

    NASA Astrophysics Data System (ADS)

    McBeath, A.; Gheorghe, A. D.

    2003-05-01

    A new project to investigate beliefs in meteors and meteoric phenomena in past and present times using chiefly folklore, mythology, prose and poetic literature, is described. Some initial examples are given, along with a bibliography of relevant items already in print in IMO publications.

  8. Meteor Researches at Khnure

    NASA Astrophysics Data System (ADS)

    Kolomiyets, Svitlana V.; Voloshchuk, Yuri I.; Kashcheyev, Boris L.; Slipchenko, Nikolay I.

    The Scientific Educational Center of Radioengineering of the Kharkiv National University of Radioelectronics (KHNURE: ) is one of the oldest radar meteor centers which was founded by B. L. Kashcheyev in 1958. The first automatic meteor radar system in Ukraine “MARS” is connected with our University. There are long-term observational series of meteor rates and orbital data in the Center. Fields of the KHNURE researches are: a structure of meteor showers a determination of meteoroid orbits an influx of cosmic rubbish in the Earth atmosphere search of parental bodies of meteoroids a statistic analysis of measurement results of radiometeors an estimation of errors of meteor radar measurements a search for real hyperbolic orbits and interstellar meteoroids. KHNURE disposes a unique electronic orbital catalogue. This catalogue contains the primary information velocities radiants and orbits of nearly 250000 radiometeoroids with masses from 0.001 to 0.000001 g. The “MARS” registered these data during observations of 1972 1978. From these data 5160 meteor streams are singled out. New classification of streams is made in view of their structure. The study of meteor stream orbits from the KHNURE data bank allow to predict orbits of a big number of undiscovered “dangerous” NEOs

  9. Meteor researches at KHNURE

    NASA Astrophysics Data System (ADS)

    Kolomiyets, Svitlana V.; Voloshchuk, Yuri I.; Kashcheyev, Boris L.; Slipchenko, Nikolay I.

    2005-01-01

    The Scientific Educational Center of Radioengineering of the Kharkiv National University of Radioelectronics (KHNURE: ) is one of the oldest radar meteor centers which was founded by B. L. Kashcheyev in 1958. The first automatic meteor radar system in Ukraine “MARS” is connected with our University. There are long-term observational series of meteor rates and orbital data in the Center. Fields of the KHNURE researches are: a structure of meteor showers a determination of meteoroid orbits an influx of cosmic rubbish in the Earth atmosphere search of parental bodies of meteoroids a statistic analysis of measurement results of radiometeors an estimation of errors of meteor radar measurements a search for real hyperbolic orbits and interstellar meteoroids. KHNURE disposes a unique electronic orbital catalogue. This catalogue contains the primary information velocities radiants and orbits of nearly 250000 radiometeoroids with masses from 0.001 to 0.000001 g. The “MARS” registered these data during observations of 1972 1978. From these data 5160 meteor streams are singled out. New classification of streams is made in view of their structure. The study of meteor stream orbits from the KHNURE data bank allow to predict orbits of a big number of undiscovered “dangerous” NEOs.

  10. Meteors and meteorites spectra

    NASA Astrophysics Data System (ADS)

    Koukal, J.; Srba, J.; Gorková, S.; Lenža, L.; Ferus, M.; Civiš, S.; Knížek, A.; Kubelík, P.; Kaiserová, T.; Váňa, P.

    2016-01-01

    The main goal of our meteor spectroscopy project is to better understand the physical and chemical properties of meteoroids. Astrometric and spectral observations of real meteors are obtained via spectroscopic CCD video systems. Processed meteor data are inserted to the EDMOND database (European viDeo MeteOr Network Database) together with spectral information. The fully analyzed atmospheric trajectory, orbit and also spectra of a Leonid meteor/meteoroid captured in November 2015 are presented as an example. At the same time, our target is the systematization of spectroscopic emission lines for the comparative analysis of meteor spectra. Meteoroid plasma was simulated in a laboratory by laser ablation of meteorites samples using an (ArF) excimer laser and the LIDB (Laser Induced Dielectric Breakdown) in a low pressure atmosphere and various gases. The induced plasma emissions were simultaneously observed with the Echelle Spectrograph and the same CCD video spectral camera as used for real meteor registration. Measurements and analysis results for few selected meteorite samples are presented and discussed.

  11. Dynamics of meteor streams

    NASA Technical Reports Server (NTRS)

    Babadjanov, P. B.; Obrubov, Yu. U.

    1987-01-01

    The overwhelming majority of meteor streams are generally assumed to be formed due to the decay of comets. The most effective process of the release of solid particles from a cometary nucleus is their ejection by sublimating gases when the comet approaches the Sun. The results of investigation of the Geminids and Quadrantids meteor stream evolution show that under the influence of planetary perturbations, the stream may originally be flat but then thicken depending on the variation range of orbital inclinations. Eventually, due to planetary perturbations, a meteor stream may take such a shape as to cause the start of several active showers at different solar longitudes.

  12. Minor meteor shower activity

    NASA Astrophysics Data System (ADS)

    Rendtel, J.

    2016-01-01

    Video meteor observations provide us with data to analyze structures in minor meteor showers or weak features in flux profiles. Samples obtained independently by other techniques allow to calibrate the data sets and to improve the confidence of results as demonstrated with a few results. Both, the confirmation of events predicted by model calculation and the input of observational data to improve the modelling results may help to better understand meteoroid stream evolution processes. Furthermore, calibrated data series can be used for studies of the long-term evolution of meteor shower activity.

  13. Optical electronics for meteor observations

    NASA Technical Reports Server (NTRS)

    Shafiev, R. I.; Mukhamednazarov, S.; Atamas, I. A.

    1987-01-01

    Spectral observations of meteors have been carried out for several years using an optical electronics facility. Interest has centered on faint meteors and their trails in the period of intensive meteor showers. Over 800 meteors were registered during the observation period, with spectrograms obtained for 170 of these. A total of 86 meteors were photographed from two sites and for 25 of these spectrograms of the meteors as well as their trails were obtained. All meteors have undergone routine processing in order to determine atmospheric characteristics. Results are discussed.

  14. Current trends in meteor spectroscopy

    NASA Technical Reports Server (NTRS)

    Millman, P. M.

    1982-01-01

    The history of progress over more than a century in meteor spectroscopy is summarized. The observational data were originally visual records, but in the beginning of the 20th century photography of meteor spectra was undertaken. In the forties, 60 meteor spectra were photographed. Interest in the upper atmosphere led to the development of more efficient meteor cameras which employ replica gratings, and electronic image intensification systems recordings on video tape which resulted in the availability of several thousand meteor spectra.

  15. Meteor Beliefs Project: Musical Meteors, meteoric imagery as used in near-contemporary song lyrics

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair; Gheorghe, Andrei Dorian

    2010-01-01

    Items collected from contemporary song lyrics featuring meteoric imagery, or inspired by meteors, are given, with some discussion. While not a major part of the Meteor Beliefs Project, there are points of interest in how such usage may become passed into popular beliefs about meteors.

  16. Meteoric Head Echoes

    NASA Astrophysics Data System (ADS)

    Hajduk, A.; Galád, A.

    1995-01-01

    Results of the analysis of 3261 radar meteor head echoes observed during the Orionid and Lyrid periods by the high-power radar of the Springhill Meteor Observatory are given. Dependence of the occurence of head echoes on the geometrical factors and physical properties of the meteoroids has been studied. Increas of the head echo rates with the elevation of the shower radiant and with the velocity of meteoroids has been observed.

  17. Resolving Seamounts in Satellite Altimetry

    NASA Astrophysics Data System (ADS)

    Marks, K. M.; Smith, W. H.

    2006-12-01

    We have examined three factors influencing the use of satellite altimeter data to map seamounts and guyots in the deep ocean: (1) the resolution of seamount and guyot gravity anomalies by altimetry; (2) the non-linearity of the relationship between gravity and bathymetry; and (3) the homogeneity of the mass density within the seamount or guyot. When altimeter data are used to model the marine gravity anomaly field the result may have limited resolution due to noise levels in the altimeter data, track spacing of the satellite profiles, inclination angles of the orbits, and filters used to combine and interpolate the data (Sandwell and Smith, JGR, 1997). We compared the peak-to-trough amplitude of gravity anomalies in Sandwell and Smith`'s version 15.1 field to peak-to-trough amplitudes measured by gravimeters on board ships. The satellite gravity field amplitudes match ship measurements well over seamounts and guyots having volumes exceeding ~2000 km3. Over smaller volume seamounts, where the anomalies have most of their power at quite short wavelengths, the satellite field under-estimates the anomaly amplitude. If less filtering could be done, or a new mission with a lower noise level were flown, more of the anomalies associated with small seamounts might be resolved. Smith and Sandwell (Science, 1997) predicted seafloor topography from altimetric gravity assuming that the density of seafloor topography is nearly constant over ~100 km distances, and that the relationship between gravity and topography may be approximated by a liner filter over those distances. In fact, the true theoretical relationship is non-linear (Parker, Geophys. J. R. astr. Soc, 1972); it can be expressed as an N-th order expansion, with the N=1 term representing a linear filter and the N>1 terms accounting for higher-order corrections. We find that N=2 is a sufficient approximation at both seamounts and guyots. Constant density models of large volume guyots do not fit the observed gravity

  18. Influence of the meteoric stream on weather conditions: preliminary consideration

    NASA Astrophysics Data System (ADS)

    Granitskii, Lev V.; Borisevich, A. N.

    2000-12-01

    By the some estimation, about 150 tons of the meteoric matter are fall on the Earth every day. Some researchers note coincidence of the periods of activity of the most powerful meteoric stream with the periods of intensive falling of atmospheric precipitation. The unique meteoric stream Leonids represents the great interest as an example of possible correlation between meteors and power precipitation. The comet produced this stream is well known as Tempel-Tuttl comet, its orbital period is 33.3 years. With the same periodicity, the sharp strengthening of activity of a stream, which is called meteoric shower, is observed. Such meteoric stream during a night could cover the average monthly norm of fall of meteoric bodies at once in tens time. The analysis of meteorological data shows, that the winters of 1933, 1966, 1998 and 1999 years of a maximum Leonids activity are characterized by huge amount of snow. These anomalies have resulted in disasters in some of region. Under our suggestions, the anomaly rate of falling precipitation can be explained by the meteoric dust, which plays the role of the nucleuses of condensation. Thus, taking in to account the dada of regular meteoric stream, it's possible to make long term weather forecasting with the more preciseness.

  19. The Southern Argentine Agile Meteor Radar (SAAMER)

    NASA Astrophysics Data System (ADS)

    Janches, Diego

    2014-11-01

    The Southern Argentina Agile Meteor Radar (SAAMER) is a new generation system deployed in Rio Grande, Tierra del Fuego, Argentina (53 S) in May 2008. SAAMER transmits 10 times more power than regular meteor radars, and uses a newly developed transmitting array, which focuses power upward instead of the traditional single-antenna-all-sky configuration. The system is configured such that the transmitter array can also be utilized as a receiver. The new design greatly increases the sensitivity of the radar enabling the detection of large number of particles at low zenith angles. The more concentrated transmitted power enables additional meteor studies besides those typical of these systems based on the detection of specular reflections, such as routine detections of head echoes and non-specular trails, previously only possible with High Power and Large Aperture radars. In August 2010, SAAMER was upgraded to a system capable to determine meteoroid orbital parameters. This was achieved by adding two remote receiving stations approximately 10 km away from the main site in near perpendicular directions. The upgrade significantly expands the science that is achieved with this new radar enabling us to study the orbital properties of the interplanetary dust environment. Because of the unique geographical location, SAAMER allows for additional inter-hemispheric comparison with measurements from Canadian Meteor Orbit Radar, which is geographically conjugate. Initial surveys show, for example, that SAAMER observes a very strong contribution of the South Toroidal Sporadic meteor source, of which limited observational data is available. In addition, SAAMER offers similar unique capabilities for meteor showers and streams studies given the range of ecliptic latitudes that the system enables detailed study of showers at high southern latitudes (e.g July Phoenicids or Puppids complex). Finally, SAAMER is ideal for the deployment of complementary instrumentation in both, permanent

  20. Age of Kōko Seamount, Emperor Seamount chain

    USGS Publications Warehouse

    Clague, David A.; Dalrymple, G. Brent

    1973-01-01

    KAr ages obtained by the conventional isotope-dilution and the 40Ar/39Ar techniques on two sanidine trachytes, four basalts, and a phonolite dredged from the top of Ko¯ko Seamount, 300 km north of the Hawaiian-Emperor bend, show that the seamount is 46.4 ± 1.1 my old. These data indicate that the volcanoes in the Hawaiian-Emperor chain continue to increase in age to the west and north beyond Midway Atoll, as predicted by the melting-spot hypothesis for the origin of the chain, and that the rate of volcanic migration along the chain was nonlinear between the time of formation of the island of Hawaii and Ko¯ko Seamount.

  1. EISCAT meteor observations

    NASA Astrophysics Data System (ADS)

    Häggström, Ingemar; Pellinen-Wannberg, Asta; Westman, Assar; Vierinen, Juha; Brosch, Noah

    2010-05-01

    We present preliminary results from a 24-hour run to observe meteors conducted at EISCAT (Tromsø, Norway) on 17-18 December 2009, when no strong meteor showers were active. These pertain to the single-beam echoes detected at zenith by the Tromsø VHF and UHF systems and are compared with similar results obtained in 2008 during the peak of the Geminid meteor shower (Brosch et al. 2009). We present statistics of the echoes and concentrate, in particular, on the population of high-altitude echoes defined as being at 150-km altitude or higher, and on decelerating meteors. We also report on the character of tristatic echoes detected during the same period around 100-km altitude using the UHF receiver stations at Kiruna (Sweden) and Sodankylä (Finland), and on some low-altitude trails detected during this run. References: Brosch, N., Häggström, I., Pellinen-Wannberg, A., Westman, A. "Unusual features in high statistics radar meteor studies at EISCAT" Monthly Notices of the Royal Astronomical Society, 2009.

  2. Meteor Beliefs Project: A Goodly Gallerye - William Fulke's "Meteors"

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair; Gheorghe, Andrei Dorian

    2007-02-01

    An examination is presented of meteorically-relevant material from Englishman William Fulke's treatise on meteors from 1563, which encompassed much more than would modernly fall into this category, and which remained continually in print for over a century.

  3. METEORIC-HYDROTHERMAL SYSTEMS.

    USGS Publications Warehouse

    Criss, Robert E.; Taylor, Hugh P.

    1986-01-01

    This paper summarizes the salient characteristics of meteoric-hydrothermal systems, emphasing the isotopic systematics. Discussions of permeable-medium fluid dynamics and the geology and geochemistry of modern geothermal systems are also provided, because they are essential to any understanding of hydrothermal circulation. The main focus of the paper is on regions of ancient meteoric-hydrothermal activity, which give us information about the presently inaccessible, deep-level parts of modern geothermal systems. It is shown oxygen and hydrogen isotopes provide a powerful method to discover and map fossil hydrothermal systems and to investigate diverse associated aspects of rock alteration and ore deposition.

  4. Martian Meteor Crater

    NASA Technical Reports Server (NTRS)

    2004-01-01

    20 February 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a fairly young meteor impact crater on Mars that is about the same size ( 1 kilometer; 0.62 miles) as the famous Meteor Crater in northern Arizona, U.S.A. Like the Arizona crater, boulders of ejected bedrock can be seen on the crater's ejecta blanket and in the crater itself. This crater is located in the Aethiopis region of Mars near 4.7oN, 224.1oW. Sunlight illuminates the scene from the lower left.

  5. Asteroids, Comets, Meteors 1991

    NASA Technical Reports Server (NTRS)

    Harris, Alan W. (Editor); Bowell, Edward (Editor)

    1992-01-01

    Papers from the conference are presented and cover the following topics with respect to asteroids, comets, and/or meteors: interplanetary dust, cometary atmospheres, atmospheric composition, comet tails, astronomical photometry, chemical composition, meteoroid showers, cometary nuclei, orbital resonance, orbital mechanics, emission spectra, radio astronomy, astronomical spectroscopy, photodissociation, micrometeoroids, cosmochemistry, and interstellar chemistry.

  6. Martian Meteor Ionization Layers

    NASA Technical Reports Server (NTRS)

    Grebowsky, J. M.; Pesnell, W. D.

    1999-01-01

    Small interplanetary grains bombard Mars, like all the solar system planets, and, like all the planets with atmospheres, meteoric ion and atom layers form in the upper atmosphere. We have developed a comprehensive one-dimensional model of the Martian meteoric ionization layer including a full chemical scheme. A persistent layer of magnesium ions should exist around an altitude of 70 km. Unlike the terrestrial case, where the metallic ions are formed via charge-exchange with the ambient ions, Mg(+) in the Martian atmosphere is produced by photoionization. Nevertheless, the predicted metal layer peak densities for Earth and Mars are similar. Diffusion solutions, such as those presented here, should be a good approximation of the metallic ions in regions where the magnetic field is negligible and may provide a significant contribution to the nightside ionosphere. The low ultraviolet absorption of the Martian atmosphere may make Mars an excellent laboratory in which to study meteoric ablation. Resonance lines not seen in the spectra of terrestrial meteors may be visible to a surface observatory in the Martian highlands.

  7. Video Meteor Fluxes

    NASA Technical Reports Server (NTRS)

    Campbell-Brown, M. D.; Braid, D.

    2011-01-01

    The flux of meteoroids, or number of meteoroids per unit area per unit time, is critical for calibrating models of meteoroid stream formation and for estimating the hazard to spacecraft from shower and sporadic meteors. Although observations of meteors in the millimetre to centimetre size range are common, flux measurements (particularly for sporadic meteors, which make up the majority of meteoroid flux) are less so. It is necessary to know the collecting area and collection time for a given set of observations, and to correct for observing biases and the sensitivity of the system. Previous measurements of sporadic fluxes are summarized in Figure 1; the values are given as a total number of meteoroids striking the earth in one year to a given limiting mass. The Gr n et al. (1985) flux model is included in the figure for reference. Fluxes for sporadic meteoroids impacting the Earth have been calculated for objects in the centimeter size range using Super-Schmidt observations (Hawkins & Upton, 1958); this study used about 300 meteors, and used only the physical area of overlap of the cameras at 90 km to calculate the flux, corrected for angular speed of meteors, since a large angular speed reduces the maximum brightness of the meteor on the film, and radiant elevation, which takes into account the geometric reduction in flux when the meteors are not perpendicular to the horizontal. They bring up corrections for both partial trails (which tends to increase the collecting area) and incomplete overlap at heights other than 90 km (which tends to decrease it) as effects that will affect the flux, but estimated that the two effects cancelled one another. Halliday et al. (1984) calculated the flux of meteorite-dropping fireballs with fragment masses greater than 50 g, over the physical area of sky accessible to the MORP fireball cameras, counting only observations in clear weather. In the micron size range, LDEF measurements of small craters on spacecraft have been used to

  8. Studies of Transient Meteor Activity

    NASA Technical Reports Server (NTRS)

    Jenniskens, Peter M. M.

    2002-01-01

    Meteoroids bombard Earth's atmosphere daily, but occasionally meteor rates increase to unusual high levels when Earth crosses the relatively fresh ejecta of comets. These transient events in meteor activity provide clues about the whereabouts of Earth-threatening long-period comets, the mechanisms of large-grain dust ejection from comets, and the particle composition and size distribution of the cometary ejecta. Observations of these transient events provide important insight in natural processes that determine the large grain dust environment of comets, in natural phenomena that were prevalent during the time of the origin of life, and in processes that determine the hazard of civilizations to large impacts and of man-made satellites to the periodic blizzard of small meteoroids. In this proposal, three tasks form a coherent program aimed at elucidating various aspects of meteor outbursts, with special reference to planetary astronomy and astrobiology. Task 1 was a ground-based effort to observe periods of transient meteor activity. This includes: (1) stereoscopic imaging of meteors during transient meteor events for measurements of particle size distribution, meteoroid orbital dispersions and fluxes; and (2) technical support for Global-MS-Net, a network of amateur-operated automatic counting stations for meteor reflections from commercial VHF radio and TV broadcasting stations, keeping a 24h vigil on the level of meteor activity for the detection of new meteor streams. Task 2 consisted of ground-based and satellite born spectroscopic observations of meteors and meteor trains during transient meteor events for measurements of elemental composition, the presence of organic matter in the meteoroids, and products generated by the interaction of the meteoroid with the atmosphere. Task 3 was an airborne effort to explore the 2000 Leonid meteor outbursts, which are anticipated to be the most significant of transient meteor activity events in the remainder of the

  9. [Fecal fermentation in meteorism].

    PubMed

    León-Barúa, R; Zapata-Solari, C

    1977-12-01

    An old test to investigate fecal fermentation was modified with the purpose of changing it from qualitative to quantitative. The modified test consists in placing in stove, at 37 degrees C for 24 hours, 5 grams of feces, suspended in water. The fermentable alimentary residues, present in the feces, suffer the action of bacteria, also there present, yielding gas that is collected and measured. Using the test, fecal fermentation was determined in 3 groups of individuals: a) 40 patients with meteorism that had persisted or improved only slightly or fairly with treatment; b) 28 apparently healthy subjects; and c) 6 patients with meteorism that had disappeared or become minimal with treatment. In the group of 28 apparently healthy subject, the obtained results varied from 0.1 to 1.1 ml gas/24 h., with a mean +/- s.d. of 0.55 +/- 0.29 ml. gas/24 h. When a distribution curve was made with the results obtained in the group of 40 patients with meteorism, these results separated into 2 subgroups: one subgroup with 28 patients, in whom results varied from 1.0 to 13.3 ml. gas/24 h., with a mean of 4.8 gas/24 h. (only) in 1 of these 28 patients a normal result of 1.0 ml. gas/24 h. was obtained, while in the remaining 27 patients results of 1.5 or more ml. gas/24 h. were obtained); and the other subgroup with 12 patients, in whom results varied from 0.0 to 0.9 ml. gas/24 h., with a mean of 0.29 ml. gas/24 h. Finally, in the group of 6 patients with successfully treated meteorism, results were from 0.1 to 0.9 ml. gas/24 h., with a mean of 0.4 ml. gas/24 h. The above mentioned results strongly suggest the existence of a relationship between meteorism and exagerated fecal fermentation. The nature of this relationship has not yet been completely clarified. However, the test used to determine fecal fermentation already promises to be very helpful for a better understanding and management of meteorism.

  10. Elemental abundance determinations for meteors by spectroscopy.

    NASA Technical Reports Server (NTRS)

    Harvey, G. A.

    1973-01-01

    Relative elemental abundance determinations for meteors by spectroscopy are discussed. Relative abundances of spectroscopically accessible elements of four major shower meteors and one sporadic meteor are presented. A sporadic meteor with dominant sodium radiation and an iron-deficient sporadic meteor are analyzed. Empirical and theoretical tests for self-absorption in optical meteor plasmas have been conducted. Both ionization and incomplete dissociation are found to severely deplete certain neutral atoms from meteor plasmas.

  11. Zhamanshin meteor crater

    NASA Technical Reports Server (NTRS)

    Florenskiy, P. V.; Dabizha, A. I.

    1987-01-01

    A historical survey and geographic, geologic and geophysical characteristics, the results of many years of study of the Zhamanshin meteor crater in the Northern Aral region, are reported. From this data the likely initial configuration and cause of formation of the crater are reconstructed. Petrographic and mineralogical analyses are given of the brecciated and remelted rocks, of the zhamanshinites and irgizite tektites in particular. The impact melting, dispersion and quenching processes resulting in tektite formation are discussed.

  12. Meteor signature interpretation

    SciTech Connect

    Canavan, G.H.

    1997-01-01

    Meteor signatures contain information about the constituents of space debris and present potential false alarms to early warnings systems. Better models could both extract the maximum scientific information possible and reduce their danger. Accurate predictions can be produced by models of modest complexity, which can be inverted to predict the sizes, compositions, and trajectories of object from their signatures for most objects of interest and concern.

  13. Optical fluxes and meteor properties of the camelopardalid meteor shower

    NASA Astrophysics Data System (ADS)

    Campbell-Brown, M. D.; Blaauw, R.; Kingery, A.

    2016-10-01

    Observations of the Camelopardalid meteor shower in May 2014 were obtained with six different sets of cameras, with limiting meteor magnitudes varying from -2M to +7M. Shower fluxes were calculated for each of the systems, from which the mass index of the shower was found to be 2.17 ± 0.04. Faint meteors in the shower were found to be stronger than average, ablating at lower altitudes than meteors at the same speed recorded with the same system, while the brightest meteors had higher ablation heights and were therefore weaker than typical meteors. These findings can be explained if large Camelopardalids are weak agglomerations of more refractory grains, which are easily disrupted in space and keep the shower supplied with small material and depleted in large material.

  14. Oceanographic aspects of the Emperor Seamounts region

    SciTech Connect

    Roden, G.I.; Taft, B.A.; Ebbesmeyer, C.C.

    1982-11-20

    Effects of the Emperor Seamount Chain on the thermohaline structure and baroclinic flow are investigated on the basis of historical hydrographic data. The amplitudes of dynamic height perturbations are 3 to 5 times larger west than east of the chain. The intensity of the thermal fronts is stronger west than east of the seamounts; near the crest of the southern seamounts, strong east-west thermohaline fronts and a strong northward baroclinic flow are observed. The Kuroshio Extension west of the seamount chain is a well-defined meandering current, the axis of which generally lies between 33/sup 0/ and 36/sup 0/N. The available data indicate that the Kuroshio Extension turns northward and then flows eastward through the gaps of the seamount chain. East of the seamounts, the Kuroshio Extension widens threefold and appears to be poorly defined.

  15. Light curves of faint meteors

    NASA Astrophysics Data System (ADS)

    Koten, Pavel; Borovička, Jiří

    2001-11-01

    The results of the light curves analysis of 234 meteors observed and recorded within the double-station image intensifier observations at the Ondřejov observatory are presented. Double-station observations allow to compute the meteor trajectory in the solar system and in the atmosphere as well as to determinate the absolute magnitude of meteor and its mass. Light curves and heights data of all major meteor showers - Lyrids, η-Aquarids, Perseids, Orionids, Leonids, Geminids as well as many sporadic meteors - were analysed. The differences between individual showers were found, e.g. Perseids appear to be more compact than Leonids. There is also difference between 1998 and 1999 Leonids. This suggests different composition or structure of parent bodies. Our data show that the beginning heights of Perseids, Orionids and Leonids are weakly dependent on meteor mass, although the dust-ball theory assumes they should be mass independent.

  16. Meteors in Australian Aboriginal Dreamings

    NASA Astrophysics Data System (ADS)

    Hamacher, Duane W.; Norris, Ray P.

    2010-06-01

    We present a comprehensive analysis of Australian Aboriginal accounts of meteors. The data used were taken from anthropological and ethnographic literature describing oral traditions, ceremonies, and Dreamings of 97 Aboriginal groups representing all states of modern Australia. This revealed common themes in the way meteors were viewed between Aboriginal groups, focusing on supernatural events, death, omens, and war. The presence of such themes around Australia was probably due to the unpredictable nature of meteors in an otherwise well-ordered cosmos.

  17. Co-rich Mn crusts from the Magellan Seamount cluster: the long journey through time

    NASA Astrophysics Data System (ADS)

    Glasby, Geoffrey P.; Ren, Xiangwen; Shi, Xuefa; Pulyaeva, Irina A.

    2007-10-01

    The Magellan seamounts began forming as large submarine shield volcanoes south of the equator during the Cretaceous. These volcanoes formed as a cluster on the small Pacific plate in a period when tectonic stress was absent. Thermal subsidence of the seafloor led to sinking of these volcanoes and the formation of guyots as the seamounts crossed the equatorial South Pacific (10-0°S) sequentially and ocean surface temperatures became too high for calcareous organisms to survive. Guyot formation was completed between about 59 and 45 Ma and the guyots became phosphatized at about 39-34 and 27-21 Ma. Ferromanganese crusts began formation as proto-crusts on the seamounts and guyots of the Magellan Seamount cluster towards the end of the Cretaceous up to 55 Ma after the formation of the seamounts themselves. The chemical composition of these crusts evolved over time in a series of steps in response to changes in global climate and ocean circulation. The great thickness of these crusts (up to 15-20 cm) reflects their very long period of growth. The high Co contents of the outer parts of the crusts are a consequence of the increasing deep circulation of the ocean and the resulting deepening of the oxygen minimum zone with time. Growth of the Co-rich Mn crusts in the Magellan Seamount cluster can be considered to be the culmination of a long journey through time.

  18. Meteor Beliefs Project: Meteoric references in Ovid's Metamorphoses

    NASA Astrophysics Data System (ADS)

    Gheorghe, A. D.; McBeath, A.

    2003-10-01

    Three sections of Ovid's Metamorphoses are examined, providing further information on meteoric beliefs in ancient Roman times. These include meteoric imagery among the portents associated with the death of Julius Caesar, which we mentioned previously from the works of William Shakespeare (McBeath and Gheorghe, 2003b).

  19. James Joule and meteors

    NASA Astrophysics Data System (ADS)

    Hughes, David W.

    1989 was the hundredth anniversary of the death of James Prescott Joule, the Prescott being his mother's family name and the Joule, rhyming with cool, originating from the Derbyshire village of Youlgreave. Joule is rightly famous for his experimental efforts to establish the law of conservation of energy, and for the fact that J, the symbol known as the mechanical equivalent of heat, is named after him. Astronomically his "light has been hidden under a bushel". James Joule had a major influence on the physics of meteors.

  20. Meteor detections at the Metsähovi Fundamental Geodetic Research Station (Finland)

    NASA Astrophysics Data System (ADS)

    Raja-Halli, A.; Gritsevich, M.; Näränen, J.; Moreno-Ibáñez, M.; Lyytinen, E.; Virtanen, J.; Zubko, N.; Peltoniemi, J.; Poutanen, M.

    2016-01-01

    We provide an overview and present some spectacular examples of the recent meteor observations at the Metsähovi Geodetic Research Station. In conjunction with the Finnish Fireball Network the all-sky images are used to reconstruct atmospheric trajectories and to calculate the pre-impact meteor orbits in the Solar System. In addition, intensive collaborative work is pursued with the meteor research groups worldwide. We foresee great potential of this activity also for educational and outreach purposes.

  1. Meteor fireball sounds identified

    NASA Technical Reports Server (NTRS)

    Keay, Colin

    1992-01-01

    Sounds heard simultaneously with the flight of large meteor fireballs are electrical in origin. Confirmation that Extra/Very Low Frequency (ELF/VLF) electromagnetic radiation is produced by the fireball was obtained by Japanese researchers. Although the generation mechanism is not fully understood, studies of the Meteorite Observation and Recovery Project (MORP) and other fireball data indicate that interaction with the atmosphere is definitely responsible and the cut-off magnitude of -9 found for sustained electrophonic sounds is supported by theory. Brief bursts of ELF/VLF radiation may accompany flares or explosions of smaller fireballs, producing transient sounds near favorably placed observers. Laboratory studies show that mundane physical objects can respond to electrical excitation and produce audible sounds. Reports of electrophonic sounds should no longer be discarded. A catalog of over 300 reports relating to electrophonic phenomena associated with meteor fireballs, aurorae, and lightning was assembled. Many other reports have been cataloged in Russian. These may assist the full solution of the similar long-standing and contentious mystery of audible auroral displays.

  2. Asteroids, Comets, Meteors 2014

    NASA Astrophysics Data System (ADS)

    Muinonen, K.; Penttilä, A.; Granvik, M.; Virkki, A.; Fedorets, G.; Wilkman, O.; Kohout, T.

    2014-08-01

    Asteroids, Comets, Meteors focuses on the research of small Solar System bodies. Small bodies are the key to understanding the formation and evolution of the Solar System, carrying signals from pre-solar times. Understanding the evolution of the Solar System helps unveil the evolution of extrasolar planetary systems. Societally, small bodies will be important future resources of minerals. The near-Earth population of small bodies continues to pose an impact hazard, whether it be small pieces of falling meteorites or larger asteroids or cometary nuclei capable of causing global environmental effects. The conference series entitled ''Asteroids, Comets, Meteors'' constitutes the leading international series in the field of small Solar System bodies. The first three conferences took place in Uppsala, Sweden in 1983, 1985, and 1989. The conference is now returning to Nordic countries after a quarter of a century. After the Uppsala conferences, the conference has taken place in Flagstaff, Arizona, U.S.A. in 1991, Belgirate, Italy in 1993, Paris, France in 1996, Ithaca, New York, U.S.A. in 1999, in Berlin, Germany in 2002, in Rio de Janeiro, Brazil in 2005, in Baltimore, Maryland, U.S.A. in 2008, and in Niigata, Japan in 2012. ACM in Helsinki, Finland in 2014 will be the 12th conference in the series.

  3. Radar Meteor Observations in Australia

    NASA Astrophysics Data System (ADS)

    Elford, W. G.

    1993-01-01

    During the last decade extensive meteor studies have been carried out in Australia using radio systems operating at frequencies between 2 and 30 MHz. Part of this program has been a deliberate effort to detect meteors above the "echo ceiling" of about 105 km associated with radars operating above 30 MHz. In fact the echo ceiling has been raised to 140 km with a dramatic increase in meteor flux [1]. The other aspect of these studies has been the use a low frequency (6-30MHz) surveillance radar to detect and record meteors over the horizon, using backscatter via ionospheric F-region. The power of the radar is such that the micrometeoroid limit is being approached [2]. The surveillance radar has confirmed the new estimates of meteor flux and extended to a mass limit of 0.2 microgram.

  4. Computational Physics of Small Meteors

    NASA Astrophysics Data System (ADS)

    Surzhikov, S. T.

    2015-10-01

    This paper is dedicated to application of the modern computational aero physical models, which were developed for mathematical modeling of aerothermodynamics and radiative gasdynamics of space vehicles, for investigation of meteoric phenomena. Short analysis of modern problems of meteoric physics is presented. The typical chemical compositions of meteoric bodies are discussed. Considerable attention is given to investigation of the non-equilibrium physical-chemical processes accompanying a meteor with relatively small size at altitude of 70 km, in the conditions, when the vibrational relaxation zone exceeds the size of meteoric body. Two-dimensional numerical simulation radiative gas dynamics model of physically and chemically nonequilibrium flow field around the meteoroid bodies entering Earth atmosphere is presented.

  5. 50 CFR 665.209 - Fishing moratorium at Hancock Seamounts.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 50 Wildlife and Fisheries 11 2011-10-01 2011-10-01 false Fishing moratorium at Hancock Seamounts... Hawaii Fisheries § 665.209 Fishing moratorium at Hancock Seamounts. Fishing for, and possession of, Hawaii bottomfish and seamount groundfish MUS in the Hancock Seamounts Ecosystem Management Area...

  6. 50 CFR 665.209 - Fishing moratorium on Hancock Seamount.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 50 Wildlife and Fisheries 9 2010-10-01 2010-10-01 false Fishing moratorium on Hancock Seamount... Hawaii Fisheries § 665.209 Fishing moratorium on Hancock Seamount. Fishing for Hawaii bottomfish and seamount groundfish MUS on the Hancock Seamount is prohibited through August 31, 2010....

  7. 50 CFR 665.209 - Fishing moratorium at Hancock Seamounts.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 50 Wildlife and Fisheries 13 2013-10-01 2013-10-01 false Fishing moratorium at Hancock Seamounts... Hawaii Fisheries § 665.209 Fishing moratorium at Hancock Seamounts. Fishing for, and possession of, Hawaii bottomfish and seamount groundfish MUS in the Hancock Seamounts Ecosystem Management Area...

  8. 50 CFR 665.209 - Fishing moratorium at Hancock Seamounts.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 50 Wildlife and Fisheries 13 2012-10-01 2012-10-01 false Fishing moratorium at Hancock Seamounts... Hawaii Fisheries § 665.209 Fishing moratorium at Hancock Seamounts. Fishing for, and possession of, Hawaii bottomfish and seamount groundfish MUS in the Hancock Seamounts Ecosystem Management Area...

  9. 50 CFR 665.209 - Fishing moratorium at Hancock Seamounts.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 50 Wildlife and Fisheries 13 2014-10-01 2014-10-01 false Fishing moratorium at Hancock Seamounts... Hawaii Fisheries § 665.209 Fishing moratorium at Hancock Seamounts. Fishing for, and possession of, Hawaii bottomfish and seamount groundfish MUS in the Hancock Seamounts Ecosystem Management Area...

  10. Deep-sea fish distribution varies between seamounts: results from a seamount complex off New Zealand.

    PubMed

    Tracey, Dianne M; Clark, Malcolm R; Anderson, Owen F; Kim, Susan W

    2012-01-01

    Fish species data from a complex of seamounts off New Zealand termed the "Graveyard Seamount Complex' were analysed to investigate whether fish species composition varied between seamounts. Five seamount features were included in the study, with summit depths ranging from 748-891 m and elevation from 189-352 m. Measures of fish species dominance, rarity, richness, diversity, and similarity were examined. A number of factors were explored to explain variation in species composition, including latitude, water temperature, summit depth, depth at base, elevation, area, slope, and fishing effort. Depth at base and slope relationships were significant with shallow seamounts having high total species richness, and seamounts with a more gradual slope had high mean species richness. Species similarity was modelled and showed that the explanatory variables were driven primarily by summit depth, as well as by the intensity of fishing effort and elevation. The study showed that fish assemblages on seamounts can vary over very small spatial scales, in the order of several km. However, patterns of species similarity and abundance were inconsistent across the seamounts examined, and these results add to a growing literature suggesting that faunal communities on seamounts may be populated from a broad regional species pool, yet show considerable variation on individual seamounts. PMID:22745656

  11. Deep-sea fish distribution varies between seamounts: results from a seamount complex off New Zealand.

    PubMed

    Tracey, Dianne M; Clark, Malcolm R; Anderson, Owen F; Kim, Susan W

    2012-01-01

    Fish species data from a complex of seamounts off New Zealand termed the "Graveyard Seamount Complex' were analysed to investigate whether fish species composition varied between seamounts. Five seamount features were included in the study, with summit depths ranging from 748-891 m and elevation from 189-352 m. Measures of fish species dominance, rarity, richness, diversity, and similarity were examined. A number of factors were explored to explain variation in species composition, including latitude, water temperature, summit depth, depth at base, elevation, area, slope, and fishing effort. Depth at base and slope relationships were significant with shallow seamounts having high total species richness, and seamounts with a more gradual slope had high mean species richness. Species similarity was modelled and showed that the explanatory variables were driven primarily by summit depth, as well as by the intensity of fishing effort and elevation. The study showed that fish assemblages on seamounts can vary over very small spatial scales, in the order of several km. However, patterns of species similarity and abundance were inconsistent across the seamounts examined, and these results add to a growing literature suggesting that faunal communities on seamounts may be populated from a broad regional species pool, yet show considerable variation on individual seamounts.

  12. The Chelyabinsk meteor

    NASA Astrophysics Data System (ADS)

    Popova, O.; Jenniskens, P.; Shuvalov, V.; Emel'yanenko, V.; Rybnov, Y.; Kharlamov, V.; Kartashova, A.; Biryukov, E.; Khaibrakhmanov, S.

    2014-07-01

    A review is given about what was learned about the 0.5-Mt Chelyabinsk airburst of 15 February 2013 by field studies, the analysis of recovered meteorites, and numerical models of meteoroid fragmentation and airburst propagation. Previous events with comparable or larger energy in recent times include only the 0.5-Mt -sized 3 August 1963 meteor over the south Atlantic, for which only an infrasound signal was recorded, and the famous Tunguska impact of 1908. Estimates of the initial kinetic energy of the Tunguska impact range from 3 to 50 Mt, due to the lack of good observations at the time. The Chelyabinsk event is much better documented than both, and provides a unique opportunity to calibrate the different approaches used to model meteoroid entry and calculate the damaging effects of a shock wave from a large meteoroid impact. A better understanding of what happened might help future impact hazard mitigation efforts by calibrating models of what might happen under somewhat different circumstances. The initial kinetic energy is estimated from infrasonic signals and the fireball's lightcurve, as well as the extent of the glass damage on the ground. Analysis of video observations of the fireball and the shadow movements provided an impact trajectory and a record of the meteor lightcurve, which describes how that energy was deposited in the atmosphere. Ablation and fragmentation scenarios determine the success of attempts to reproduce the observed meteor lightcurve and deceleration profile by numerical modeling. There was almost no deceleration until peak brightness. Meteoroid fragmentation occurred in different forms, some part of the initial mass broke in well separated fragments, the surviving fragments falling on the ground as meteorites. The specific conditions during energy deposition determined the fraction of surviving mass. The extent of the glass damage was mapped by visiting over 50 villages in the area. A number of numerical simulations were conducted that

  13. JEM-EUSO: Meteor and nuclearite observations

    NASA Astrophysics Data System (ADS)

    Adams, J. H.; Ahmad, S.; Albert, J.-N.; Allard, D.; Anchordoqui, L.; Andreev, V.; Anzalone, A.; Arai, Y.; Asano, K.; Ave Pernas, M.; Baragatti, P.; Barrillon, P.; Batsch, T.; Bayer, J.; Bechini, R.; Belenguer, T.; Bellotti, R.; Belov, K.; Berlind, A. A.; Bertaina, M.; Biermann, P. L.; Biktemerova, S.; Blaksley, C.; Blanc, N.; Błȩcki, J.; Blin-Bondil, S.; Blümer, J.; Bobik, P.; Bogomilov, M.; Bonamente, M.; Briggs, M. S.; Briz, S.; Bruno, A.; Cafagna, F.; Campana, D.; Capdevielle, J.-N.; Caruso, R.; Casolino, M.; Cassardo, C.; Castellinic, G.; Catalano, C.; Catalano, G.; Cellino, A.; Chikawa, M.; Christl, M. J.; Cline, D.; Connaughton, V.; Conti, L.; Cordero, G.; Crawford, H. J.; Cremonini, R.; Csorna, S.; Dagoret-Campagne, S.; de Castro, A. J.; De Donato, C.; de la Taille, C.; De Santis, C.; del Peral, L.; Dell'Oro, A.; De Simone, N.; Di Martino, M.; Distratis, G.; Dulucq, F.; Dupieux, M.; Ebersoldt, A.; Ebisuzaki, T.; Engel, R.; Falk, S.; Fang, K.; Fenu, F.; Fernández-Gómez, I.; Ferrarese, S.; Finco, D.; Flamini, M.; Fornaro, C.; Franceschi, A.; Fujimoto, J.; Fukushima, M.; Galeotti, P.; Garipov, G.; Geary, J.; Gelmini, G.; Giraudo, G.; Gonchar, M.; González Alvarado, C.; Gorodetzky, P.; Guarino, F.; Guzmán, A.; Hachisu, Y.; Harlov, B.; Haungs, A.; Hernández Carretero, J.; Higashide, K.; Ikeda, D.; Ikeda, H.; Inoue, N.; Inoue, S.; Insolia, A.; Isgrò, F.; Itow, Y.; Joven, E.; Judd, E. G.; Jung, A.; Kajino, F.; Kajino, T.; Kaneko, I.; Karadzhov, Y.; Karczmarczyk, J.; Karus, M.; Katahira, K.; Kawai, K.; Kawasaki, Y.; Keilhauer, B.; Khrenov, B. A.; Kim, J.-S.; Kim, S.-W.; Kim, S.-W.; Kleifges, M.; Klimov, P. A.; Kolev, D.; Kreykenbohm, I.; Kudela, K.; Kurihara, Y.; Kusenko, A.; Kuznetsov, E.; Lacombe, M.; Lachaud, C.; Lee, J.; Licandro, J.; Lim, H.; López, F.; Maccarone, M. C.; Mannheim, K.; Maravilla, D.; Marcelli, L.; Marini, A.; Martinez, O.; Masciantonio, G.; Mase, K.; Matev, R.; Medina-Tanco, G.; Mernik, T.; Miyamoto, H.; Miyazaki, Y.; Mizumoto, Y.; Modestino, G.; Monaco, A.; Monnier-Ragaigne, D.; Morales de los Ríos, J. A.; Moretto, C.; Morozenko, V. S.; Mot, B.; Murakami, T.; Murakami, M. Nagano; Nagata, M.; Nagataki, S.; Nakamura, T.; Napolitano, T.; Naumov, D.; Nava, R.; Neronov, A.; Nomoto, K.; Nonaka, T.; Ogawa, T.; Ogio, S.; Ohmori, H.; Olinto, A. V.; Orleański, P.; Osteria, G.; Panasyuk, M. I.; Parizot, E.; Park, I. H.; Park, H. W.; Pastircak, B.; Patzak, T.; Paul, T.; Pennypacker, C.; Perez Cano, S.; Peter, T.; Picozza, P.; Pierog, T.; Piotrowski, L. W.; Piraino, S.; Plebaniak, Z.; Pollini, A.; Prat, P.; Prévôt, G.; Prieto, H.; Putis, M.; Reardon, P.; Reyes, M.; Ricci, M.; Rodríguez, I.; Rodríguez Frías, M. D.; Ronga, F.; Roth, M.; Rothkaehl, H.; Roudil, G.; Rusinov, I.; Rybczyński, M.; Sabau, M. D.; Sáez-Cano, G.; Sagawa, H.; Saito, A.; Sakaki, N.; Sakata, M.; Salazar, H.; Sánchez, S.; Santangelo, A.; Santiago Crúz, L.; Sanz Palomino, M.; Saprykin, O.; Sarazin, F.; Sato, H.; Sato, M.; Schanz, T.; Schieler, H.; Scotti, V.; Segreto, A.; Selmane, S.; Semikoz, D.; Serra, M.; Sharakin, S.; Shibata, T.; Shimizu, H. M.; Shinozaki, K.; Shirahama, T.; Siemieniec-Oziȩbło, G.; Silva López, H. H.; Sledd, J.; Słomińska, K.; Sobey, A.; Sugiyama, T.; Supanitsky, D.; Suzuki, M.; Szabelska, B.; Szabelski, J.; Tajima, F.; Tajima, N.; Tajima, T.; Takahashi, Y.; Takami, H.; Takeda, M.; Takizawa, Y.; Tenzer, C.; Tibolla, O.; Tkachev, L.; Tokuno, H.; Tomida, T.; Tone, N.; Toscano, S.; Trillaud, F.; Tsenov, R.; Tsunesada, Y.; Tsuno, K.; Tymieniecka, T.; Uchihori, Y.; Unger, M.; Vaduvescu, O.; Valdés-Galicia, J. F.; Vallania, P.; Valore, L.; Vankova, G.; Vigorito, C.; Villaseñor, L.; von Ballmoos, P.; Wada, S.; Watanabe, J.; Watanabe, S.; Watts, J.; Weber, M.; Weiler, T. J.; Wibig, T.; Wiencke, L.; Wille, M.; Wilms, J.; Włodarczyk, Z.; Yamamoto, T.; Yamamoto, Y.; Yang, J.; Yano, H.; Yashin, I. V.; Yonetoku, D.; Yoshida, K.; Yoshida, S.; Young, R.; Zotov, M. Yu.; Zuccaro Marchi, A.

    2015-11-01

    Meteor and fireball observations are key to the derivation of both the inventory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capability. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission.

  14. Radar observations of the Volantids meteor shower

    NASA Astrophysics Data System (ADS)

    Younger, J.; Reid, I.; Murphy, D.

    2016-01-01

    A new meteor shower occurring for the first time on 31 December 2015 in the constellation Volans was identified by the CAMS meteor video network in New Zealand. Data from two VHF meteor radars located in Australia and Antarctica have been analyzed using the great circle method to search for Volantids activity. The new shower was found to be active for at least three days over the period 31 December 2015 - 2 January 2016, peaking at an apparent radiant of R.A. = 119.3 ± 3.7, dec. = -74.5 ± 1.9 on January 1st. Measurements of meteoroid velocity were made using the Fresnel transform technique, yielding a geocentric shower velocity of 28.1 ± 1.8 km s-1. The orbital parameters for the parent stream are estimated to be a = 2.11 AU, e = 0.568, i = 47.2°, with a perihelion distance of q = 0.970 AU.

  15. Seamount resolution in satellite-derived bathymetry

    NASA Astrophysics Data System (ADS)

    Etnoyer, Peter

    2005-03-01

    I compare satellite-derived global relief data on 13 seamounts in the northeast Pacific Ocean to echosounder-derived multibeam values from the Gulf of Alaska Seamount Expeditions and the West Coast Seamounts and Ridges Multibeam Surveys for peak height, latitude, longitude, and midsection area. I find Smith and Sandwell's (1997) global sea floor topography relatively accurate for peak geoposition but generally deeper than multibeam by 192 m (±132 m). Cell size alone can explain 50-90% of peak height variation, suggesting higher-resolution geodetic altimetry could improve the accuracy of these estimates. Nevertheless, midsection areas overlap by 80 ± 11%. The altimetric technique clearly resolves the presence and general form of numerous unnamed deep seamounts, though predicted seamount peak height estimates for small features may vary from their true depth by up to 50%. These findings support high-end estimates of global seamount abundance since small seamount features (˜1200 m relief) revealed by satellite may, in actuality, be quite substantial features (˜2500 m relief).

  16. Catalogue of representative meteor spectra

    NASA Astrophysics Data System (ADS)

    Vojáček, V.; Borovička, J.; Koten, P.; Spurný, P.; Štork, R.

    2015-08-01

    Aims: We present a library of low-resolution meteor spectra that includes sporadic meteors, members of minor meteor showers, and major meteor showers. These meteors are in the magnitude range from +2 to -3, corresponding to meteoroid sizes from 1 mm to 10 mm. Methods: Parallel double-station video observations allowed us to compute heliocentric orbits for all meteors. Most observations were performed during the periods of activity of major meteor showers in the years between 2006 and 2012. Spectra are classified according to relative intensities of the low-temperature emission lines of Mg, Na, and Fe. Results: Shower meteors were found to be of normal composition, except for Southern δ Aquariids and some members of the Geminid shower, neither of which have Na in the meteor spectra. Variations in Na content are typical for the Geminid shower. Three populations of Na-free mereoroids were identified. The first population are iron meteorites, which have an asteroidal-chondritic origin, but one meteoroid with low perihelion (0.11 AU) was found among the iron meteorites. The second population were Sun-approaching meteoroids in which sodium is depleted by thermal desorption. The third population were Na-free meteoroids of cometary origin. Long exposure to cosmic rays on the surface of comets in the Oort cloud and disintegration of this crust might be the origin of this population of meteoroids. Spectra (Figs. 17-30) are only, Tables 4-6 are also available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A67

  17. Artificial meteor test towards: On-demand meteor shower

    NASA Astrophysics Data System (ADS)

    Abe, S.; Okajima, L.; Sahara, H.; Watanabe, T.; Nojiri, Y.; Nishizono, T.

    2016-01-01

    An arc-heated wind tunnel is widely used for ground-based experiments to simulate environments of the planetary atmospheric entry under hypersonic and high-temperature conditions. In order to understand details of a meteor ablation such as temperature, composition ratio and fragmentation processes, the artificial meteor test was carried out using a JAXA/ISAS arc-heated wind tunnel. High-heating rate around 30 MW/m2 and High-enthalpy conditions, 10000 K arc-heated flow at velocity around 6 km/s were provided. Newly developed artificial metallic meteoroids and real meteorites such as Chelyabinsk were used for the ablation test. The data obtained by near-ultraviolet and visible spectrograph (200 and 1100nm) and high-speed camera (50 μs) have been examined to develop more efficient artificial meteor materials. We will test artificial meteors from a small satellite in 2018.

  18. Recent meteor observing activities in Japan

    NASA Astrophysics Data System (ADS)

    Yamamoto, M.

    2005-02-01

    The meteor train observation (METRO) campaign is described as an example of recent meteor observing activity in Japan. Other topics of meteor observing activities in Japan, including Ham-band radio meteor observation, the ``Japan Fireball Network'', the automatic video-capture software ``UFOCapture'', and the Astro-classroom programme are also briefly introduced.

  19. The Southern Argentina Agile Meteor Radar (SAAMER): Platform for comprehensive meteor radar observations and studies

    NASA Astrophysics Data System (ADS)

    Janches, D.; Hormaechea, J.; Pifko, S.; Hocking, W.; Fritts, D.; Brunini, C.; Close, S.; Michell, R.; Samara, M.

    2014-07-01

    The Southern Argentina Agile Meteor Radar (SAAMER) is a new generation system deployed in Rio Grande, Tierra del Fuego, Argentina (53^oS) in May 2008 (Janches et al., 2013,2014). SAAMER transmits 10 times more power than regular meteor radars, and uses a newly developed transmitting array, which focuses power upward instead of the traditional single-antenna-all-sky configuration. The system is configured such that the transmitter array can also be utilized as a receiver. The new design greatly increases the sensitivity of the radar enabling the detection of large numbers of particles at low zenith angles. The more concentrated transmitted power enables additional meteor studies besides those typical of these systems based on the detection of specular reflections, such as routine detections of head echoes and non-specular trails, previously only possible with High Power and Large Aperture radars (Janches et al., 2014). In August 2010, SAAMER was upgraded to a system capable to determine meteoroid orbital parameters. This was achieved by adding two remote receiving stations approximately 10 km away from the main site in near perpendicular directions (Pifko et al., 2014). The upgrade significantly expands the science that is achieved with this new radar enabling us to study the orbital properties of the interplanetary dust environment. Because of the unique geographical location, the SAAMER allows for additional inter-hemispheric comparison with measurements from Canadian Meteor Orbit Radar, which is geographically conjugate. Initial surveys show, for example, that SAAMER observes a very strong contribution of the South Toroidal Sporadic meteor source (Pifko et al., 2014), of which limited observational data is available. In addition, SAAMER offers similar unique capabilities for meteor showers and streams studies given the range of ecliptic latitudes that the system enables to survey (Janches et al., 2013). It can effectively observe radiants from the ecliptic south

  20. Meteor Beliefs Project: Seven years and counting

    NASA Astrophysics Data System (ADS)

    McBeath, A.; Drobnock, G. J.; Gheorghe, A. D.

    2010-04-01

    The Meteor Beliefs Project's seventh anniversary is celebrated with an eclectic mixture of meteor beliefs from the 1799 Leonids in Britain, the folkloric link between meteors and wishing in some Anglo-American sources, how a meteoric omen came to feature in Nathaniel Hawthorne's 1850 novel The Scarlet Letter, and a humorous item from the satirical magazine Punch in 1861, all helping to show how meteor beliefs can be transformed by different parts of society.

  1. On the interaction meteor complex

    NASA Astrophysics Data System (ADS)

    Rajchl, J.

    An approach to the problem of a meteoric complex called the interaction meteor complex (IMC) is applied and discussed, generalizing the idea of the interaction layer (Rajchl 1969). The role of an extended interaction of meteoroids is emphasized, both with planet surfaces and/or their satellites and with planet atmospheres, elastic or inelastic in form. The dissipation and related formative aspect are joined in one complex and compared with a topological compact. Examples of these types of interaction are presented.

  2. Kodiak seamount not flat-topped.

    PubMed

    Hamilton, E L; von Huene, R E

    1966-12-01

    Earlier surveys in the Aleutian Trench southeast of Kodiak Island, Alaska, indicated that Kodiak Seamount had a flat top and was a tablemount or guyot. This seamount is of special significance because it has been supposed that its surface was eroded at the same time as those of a line of guyots to the southeast. If so, its present position in the axis of the Aleutian Trench indicates that the line of guyots was formed before the trench. A two-part survey in 1965 showed that Kodiak Seamount is not flat-topped, and should be eliminated from the category of guyots. Reflection profiling records indicate that the seamount was formed before the adjacent sediments were deposited, and that the small trough, or moat, on the south side is a depositional feature probably formed by a scouring effect or by the acceleration of turbidity currents around the base of the mount.

  3. Detection of uncharted seamounts using satellite altimetry

    SciTech Connect

    Lazarewicz, A.P.; Schwank, D.C.

    1982-04-01

    The topography of the marine geoid (and corresponding sea surface) contains characteristic local features caused by sediments. These features can be successfully detected and located using matched filters to process single tracks of satellite altimeter data. Comparison of detected seamount features with the SNYBAPS and Scripps bathymetric data bases can reveal uncharted seamounts. This technique has been applied to 33 Seasat tracks in a region of the western Pacific bounded by 0 to 15 degrees North and 160 and 165 degrees East. From this analysis, we find three uncharted seamounts in this region. In all three cases, a detailed examination of the bathymetry shows no known bathymetric feature consistent with the detected signature. The method used to estimate the size and location of these uncharted seamounts is discussed.

  4. Kodiak seamount not flat-topped.

    PubMed

    Hamilton, E L; von Huene, R E

    1966-12-01

    Earlier surveys in the Aleutian Trench southeast of Kodiak Island, Alaska, indicated that Kodiak Seamount had a flat top and was a tablemount or guyot. This seamount is of special significance because it has been supposed that its surface was eroded at the same time as those of a line of guyots to the southeast. If so, its present position in the axis of the Aleutian Trench indicates that the line of guyots was formed before the trench. A two-part survey in 1965 showed that Kodiak Seamount is not flat-topped, and should be eliminated from the category of guyots. Reflection profiling records indicate that the seamount was formed before the adjacent sediments were deposited, and that the small trough, or moat, on the south side is a depositional feature probably formed by a scouring effect or by the acceleration of turbidity currents around the base of the mount. PMID:17770303

  5. Meteors and showers a millennium ago

    NASA Astrophysics Data System (ADS)

    Ahn, Sang-Hyeon

    2003-08-01

    Meteors can be classified into either sporadic meteors or showery meteors. We compile the meteor records in the astronomical archives in the chronicle of the Koryo dynasty (918-1392), and investigate the spatial distribution of meteor streams along the orbit of the Earth from the 10th to the 14th century. We see that meteors from meteor streams signalize themselves over noisy sporadic meteors, and that the seasonal activity of sporadic meteors is apparently regular. We discover the presence of a few meteor streams by analysing about 700 meteors in the Koryo period. We also compile the records of meteor showers and storms in the chronicles of Korea, Japan, China, Arabia and Europe, and compare their appearance dates with those of showers obtained in our analysis, as well as with the modern observations. We confirm that the three sets of data are in agreement with each other. The representative meteor showers are the Perseids, the Leonids, and the η Aquarids/Orionids pair formed by Halley's comet. The other weak or relic meteor streams are also observable but uncertain. Hence we witness the regularity of meteor activity, which is seen to persist for a millennium.

  6. Coded continuous wave meteor radar

    NASA Astrophysics Data System (ADS)

    Vierinen, Juha; Chau, Jorge L.; Pfeffer, Nico; Clahsen, Matthias; Stober, Gunter

    2016-03-01

    The concept of a coded continuous wave specular meteor radar (SMR) is described. The radar uses a continuously transmitted pseudorandom phase-modulated waveform, which has several advantages compared to conventional pulsed SMRs. The coding avoids range and Doppler aliasing, which are in some cases problematic with pulsed radars. Continuous transmissions maximize pulse compression gain, allowing operation at lower peak power than a pulsed system. With continuous coding, the temporal and spectral resolution are not dependent on the transmit waveform and they can be fairly flexibly changed after performing a measurement. The low signal-to-noise ratio before pulse compression, combined with independent pseudorandom transmit waveforms, allows multiple geographically separated transmitters to be used in the same frequency band simultaneously without significantly interfering with each other. Because the same frequency band can be used by multiple transmitters, the same interferometric receiver antennas can be used to receive multiple transmitters at the same time. The principles of the signal processing are discussed, in addition to discussion of several practical ways to increase computation speed, and how to optimally detect meteor echoes. Measurements from a campaign performed with a coded continuous wave SMR are shown and compared with two standard pulsed SMR measurements. The type of meteor radar described in this paper would be suited for use in a large-scale multi-static network of meteor radar transmitters and receivers. Such a system would be useful for increasing the number of meteor detections to obtain improved meteor radar data products.

  7. The Structure and Distribution of Benthic Communities on a Shallow Seamount (Cobb Seamount, Northeast Pacific Ocean)

    PubMed Central

    Curtis, Janelle M. R.; Clarke, M. Elizabeth

    2016-01-01

    Partially owing to their isolation and remote distribution, research on seamounts is still in its infancy, with few comprehensive datasets and empirical evidence supporting or refuting prevailing ecological paradigms. As anthropogenic activity in the high seas increases, so does the need for better understanding of seamount ecosystems and factors that influence the distribution of sensitive benthic communities. This study used quantitative community analyses to detail the structure, diversity, and distribution of benthic mega-epifauna communities on Cobb Seamount, a shallow seamount in the Northeast Pacific Ocean. Underwater vehicles were used to visually survey the benthos and seafloor in ~1600 images (~5 m2 in size) between 34 and 1154 m depth. The analyses of 74 taxa from 11 phyla resulted in the identification of nine communities. Each community was typified by taxa considered to provide biological structure and/or be a primary producer. The majority of the community-defining taxa were either cold-water corals, sponges, or algae. Communities were generally distributed as bands encircling the seamount, and depth was consistently shown to be the strongest environmental proxy of the community-structuring processes. The remaining variability in community structure was partially explained by substrate type, rugosity, and slope. The study used environmental metrics, derived from ship-based multibeam bathymetry, to model the distribution of communities on the seamount. This model was successfully applied to map the distribution of communities on a 220 km2 region of Cobb Seamount. The results of the study support the paradigms that seamounts are diversity 'hotspots', that the majority of seamount communities are at risk to disturbance from bottom fishing, and that seamounts are refugia for biota, while refuting the idea that seamounts have high endemism. PMID:27792782

  8. Barringer Meteor Crater, Arizona

    NASA Technical Reports Server (NTRS)

    2001-01-01

    Barringer Crater, also known as 'Meteor Crater,' is a 1,300-meter (0.8 mile) diameter, 174-meter (570-feet) deep hole in the flat-lying desert sandstones 30 kilometers (18.6 miles) west of Winslow, Arizona. Since the 1890s geologic studies here played a leading role in developing an understanding of impact processes on the Earth, the moon and elsewhere in the solar system.

    This view was acquired by the Landsat 4 satellite on December 14, 1982. It shows the crater much as a lunar crater might appear through a telescope. Morning sun illumination is from the southeast (lower right). The prominent gully meandering across the scene is known as Canyon Diablo. It drains northward toward the Little Colorado River and eventually to the Grand Canyon. The Interstate 40 highway crosses and nearly parallels the northern edge of the scene.

    The ejecta blanket around the crater appears somewhat lighter than the surrounding terrain, perhaps in part due to its altered mineralogic content. However, foot traffic at this interesting site may have scarred and lightened the terrain too. Also, the roughened surface here catches the sunlight on the southerly slopes and protects a highly reflective patchy snow cover in shaded northerly slopes, further lightening the terrain as viewed from space on this date.

  9. How to estimate the affect of an intense meteor

    NASA Astrophysics Data System (ADS)

    Wu, G. J.

    In the present age the potential threat to space projects coming from some intense meteor storms has been noticed Meteoroids have not the big size and great mass of the man-made space debris but they have high velocities up to 11-72 km s -1 and energies In addition a tremendous number of meteoroids might be encountered in a short time Moreover the destroy of the meteoroids is extensive In an impact the shock waves can be generated and propagate along colliding bodies compressing and heating both the target and meteoroid-self A plasma cloud may enclose the target and expands into the surrounding vacuum emitting electromagnetic radiation in a wide spectral range Especially the increasing activity of mankind in space for scientific commercial and military purposes has lead to an increase in safety-related problems about the satellites space stations and astronauts The actual destroy has been recorded many times making the data being lost or solar panels being severely damaged even the satellite lost its control and culminated in an early end of the mission Up to date several new techniques for observing meteors and meteor showers have been developed However the initial definition about a meteor storm based on visual observations with a Zenithal Hourly Rate of above one thousand seems insufficient since it only means a storm or burst of meteors in numbers means an eyewitness could have a chance to see a spectacular meteor show How to define the intense activity of a meteor storm how to estimate and predict the affect of

  10. Some models of the Geminids meteor stream formation

    NASA Technical Reports Server (NTRS)

    Belkovich, O. I.; Ryabova, G. O.

    1987-01-01

    Further development of methods of investigations of meteor shower structure and a great deal of observational data have made it possible to obtain a precise flux density profile along the Earth's orbit for the Geminids meteor shower. This curve proved to be adequately described by a exponential law. Examined are: (1) which ejection model will fit the observed shower structure; and (2) to what extent the subsequent process of evolution modifies the formed structure. The following conclusions are drawn: (1) When studying the mechanism of formation of meteor streams, it is necessary to take into consideration the velocity distribution of particles that have been ejected from the parent body; (2) On the basis of the observed density variations, it is possible to determine what kind of ejection takes place (a single ejection or that around an orbital arch); and (3) The original structure of the Geminids cross section persists for no more than 1,500 to 2,000 years.

  11. Database of Properties of Meteors

    NASA Technical Reports Server (NTRS)

    Suggs, Rob; Anthea, Coster

    2006-01-01

    A database of properties of meteors, and software that provides access to the database, are being developed as a contribution to continuing efforts to model the characteristics of meteors with increasing accuracy. Such modeling is necessary for evaluation of the risk of penetration of spacecraft by meteors. For each meteor in the database, the record will include an identification, date and time, radiant properties, ballistic coefficient, radar cross section, size, density, and orbital elements. The property of primary interest in the present case is density, and one of the primary goals in this case is to derive densities of meteors from their atmospheric decelerations. The database and software are expected to be valid anywhere in the solar system. The database will incorporate new data plus results of meteoroid analyses that, heretofore, have not been readily available to the aerospace community. Taken together, the database and software constitute a model that is expected to provide improved estimates of densities and to result in improved risk analyses for interplanetary spacecraft. It is planned to distribute the database and software on a compact disk.

  12. Coded continuous wave meteor radar

    NASA Astrophysics Data System (ADS)

    Vierinen, J.; Chau, J. L.; Pfeffer, N.; Clahsen, M.; Stober, G.

    2015-07-01

    The concept of coded continuous wave meteor radar is introduced. The radar uses a continuously transmitted pseudo-random waveform, which has several advantages: coding avoids range aliased echoes, which are often seen with commonly used pulsed specular meteor radars (SMRs); continuous transmissions maximize pulse compression gain, allowing operation with significantly lower peak transmit power; the temporal resolution can be changed after performing a measurement, as it does not depend on pulse spacing; and the low signal to noise ratio allows multiple geographically separated transmitters to be used in the same frequency band without significantly interfering with each other. The latter allows the same receiver antennas to be used to receive multiple transmitters. The principles of the signal processing are discussed, in addition to discussion of several practical ways to increase computation speed, and how to optimally detect meteor echoes. Measurements from a campaign performed with a coded continuous wave SMR are shown and compared with two standard pulsed SMR measurements. The type of meteor radar described in this paper would be suited for use in a large scale multi-static network of meteor radar transmitters and receivers. This would, for example, provide higher spatio-temporal resolution for mesospheric wind field measurements.

  13. A fast meteor detection algorithm

    NASA Astrophysics Data System (ADS)

    Gural, P.

    2016-01-01

    A low latency meteor detection algorithm for use with fast steering mirrors had been previously developed to track and telescopically follow meteors in real-time (Gural, 2007). It has been rewritten as a generic clustering and tracking software module for meteor detection that meets both the demanding throughput requirements of a Raspberry Pi while also maintaining a high probability of detection. The software interface is generalized to work with various forms of front-end video pre-processing approaches and provides a rich product set of parameterized line detection metrics. Discussion will include the Maximum Temporal Pixel (MTP) compression technique as a fast thresholding option for feeding the detection module, the detection algorithm trade for maximum processing throughput, details on the clustering and tracking methodology, processing products, performance metrics, and a general interface description.

  14. Leonid meteors, 2001 November 18

    NASA Astrophysics Data System (ADS)

    McGee, H. W.; Mobberley, M. P.

    2002-02-01

    Leonid meteors photographed from Palau, Micronesia, on 2001 November 18. Clockwise from top right: 3 meteors in Corvus, 19.18-19.20 UT; brilliant fireball in Orion, 18.48.30 UT; bright Leonid in Hydra, 19.06 UT. 50mm f/1.8 lens, 1600 ISO Fuji Superia film; M.P. Mobberley. Top left: Composite of three 5-minute exposures between 19.15 and 19.36 UT. 28mm f2.8 lens, 800 ISO Kodak Gold film; H.W. McGee.

  15. Wake in faint television meteors

    NASA Technical Reports Server (NTRS)

    Robertson, M. C.; Hawkes, Robert L.

    1992-01-01

    The two component dustball model was used in numerical lag computation. Detached grain lag is typically less than 2 km, with expected wakes of a few hundred meters. True wake in television meteors is masked by apparent wake due to the combined effects of image persistence and blooming. To partially circumvent this problem, we modified a dual MCP intensified CID video system by addition of a rotating shutter to reduce the effective exposure time to about 2.0 ms. Preliminary observations showed that only 2 of 27 analyzed meteors displayed statistically significant wake.

  16. Momentum loss for antimatter meteors

    NASA Astrophysics Data System (ADS)

    Papaelias, P. M.

    1991-02-01

    The momentum loss for a possible antimatter meteor entrance can be described by the combination of two terms. One which can be characterized by the mechanism of annihilation and a second one, the well known mechanism which is common for all koinomatter (ordinary) meteors. That is, the momentum loss caused by the air molecules swept up by the moving object. This paper discusses the contribution of the rocket effect caused by the action of the secondaries which can be produced by the annihilation interactions of the antiatoms with the air molecules.

  17. The making of meteor astronomy: part V.

    NASA Astrophysics Data System (ADS)

    Beech, M.

    1993-12-01

    The first true comparisons between the observations and the "rising vapors" hypothesis of meteor origins were made in the early eighteenth century. One of the key figures in the new meteoric dialogue was Edmond Halley.

  18. Global Variation of Meteor Trail Plasma Turbulence

    NASA Technical Reports Server (NTRS)

    Dyrud, L. P.; Hinrichs, J.; Urbina, J.

    2011-01-01

    We present the first global simulations on the occurrence of meteor trail plasma irregularities. These results seek to answer the following questions: when a meteoroid disintegrates in the atmosphere will the resulting trail become plasma turbulent, what are the factors influencing the development of turbulence, and how do they vary on a global scale. Understanding meteor trail plasma turbulence is important because turbulent meteor trails are visible as non-specular trails to coherent radars, and turbulence influences the evolution of specular radar meteor trails, particularly regarding the inference of mesospheric temperatures from trail diffusion rates, and their usage for meteor burst communication. We provide evidence of the significant effect that neutral atmospheric winds and density, and ionospheric plasma density have on the variability of meteor trail evolution and the observation of nonspecular meteor trails, and demonstrate that trails are far less likely to become and remain turbulent in daylight, explaining several observational trends using non-specular and specular meteor trails.

  19. Meteor Shower Identification and Characterization with Python

    NASA Technical Reports Server (NTRS)

    Moorhead, Althea

    2015-01-01

    The short development time associated with Python and the number of astronomical packages available have led to increased usage within NASA. The Meteoroid Environment Office in particular uses the Python language for a number of applications, including daily meteor shower activity reporting, searches for potential parent bodies of meteor showers, and short dynamical simulations. We present our development of a meteor shower identification code that identifies statistically significant groups of meteors on similar orbits. This code overcomes several challenging characteristics of meteor showers such as drastic differences in uncertainties between meteors and between the orbital elements of a single meteor, and the variation of shower characteristics such as duration with age or planetary perturbations. This code has been proven to successfully and quickly identify unusual meteor activity such as the 2014 kappa Cygnid outburst. We present our algorithm along with these successes and discuss our plans for further code development.

  20. David Levy's Guide to Observing Meteor Showers

    NASA Astrophysics Data System (ADS)

    Levy, David H.

    2007-11-01

    Preface; 1. July 4, 1956; 2. What is a meteor?; 3. Some historical notes; 4. Small rocks and dust in space; 5. Observing meteors; 6. Recording meteors; 7. Quadrantids; 8. Lyrids; 9. The Eta Aquarids; 10. The Omicron Draconids; 11. Delta Aquarids; 12. Perseids; 13. The Gamma Pavonids; 14. Orionids; 15. Taurids; 16. Leonids; 17. Geminids; 18. Ursids; 19. Meteor showers throughout the year; Appendix.

  1. Note on the 1972 Giacobinid meteor shower.

    NASA Technical Reports Server (NTRS)

    Harvey, G. A.

    1973-01-01

    It is shown that the 1972 Giacobinid meteor shower was extremely weak with a peak activity of two to three visual meteors per hour. Only two meteor spectra were obtained from the 17 slitless spectrograph systems operated by the Langley Research Center. The largely unexpected, essentially null results of the 1972 Giacobinid meteor shower observations are indicative of the present limited understanding and predictability of cosmic dust storms.

  2. The new July meteor shower

    NASA Astrophysics Data System (ADS)

    Zoladek, Przemyslaw; Wisniewski, Mariusz

    2012-12-01

    A new meteor stream was found after an activity outburst observed on 2005 July 15. The radiant was located five degrees west of the possible early Perseid radiant, close to the star Zeta Cassiopeiae. Numerous bright meteors and fireballs were observed during this maximum. Analysis of the IMO Video Database and the SonotaCo orbital database revealed an annual stream which is active just before the appearance of the first Perseids, with a clearly visible maximum at solar longitude 113°1. Activity of the stream was estimated as two times higher than activity of the Alpha Capricornids at the same time. The activity period extends from July 12 to 17, during maximum the radiant is visible at coordinates alpha = 5°9, delta = +50°5, and observed meteors are fast, with Vg = 57.4 km/s. The shower was reported to the IAU Meteor Data Center and recognized as a new discovery. According to IAU nomenclature the new stream should be named the Zeta Cassiopeiids (ZCS). %z Arlt R. (1992). WGN, Journal of the IMO, 20:2, 62-69. Drummond J. D. (1981). Icarus, 45, 545-553. Kiraga M. and Olech A. (2001). In Arlt R., Triglav M., and Trayner C., editors, Proceedings of the International Meteor Conference, Pucioasa, Romania, 21-24 September 2000, pages 45-51. IMO. Molau S. (2007). In Bettonvil F. and Kac J., editors, Proceedings of the International Meteor Conference, Roden, The Netherlands, 14-17 September 2006, pages 38-55. IMO. Molau S. and Rendtel J. (2009). WGN, Journal of the IMO, 37:4, 98-121. Olech A., Zoladek P., Wisniewski M., Krasnowski M., Kwinta M., Fajfer T., Fietkiewicz K., Dorosz D., Kowalski L., Olejnik J., Mularczyk K., and Zloczewski K. (2006). In Bastiaens L., Verbert J., Wislez J.-M., and Verbeeck C., editors, Proceedings of the International Meteor Conference, Oostmalle, Belgium, 15-18 September 2005, pages 53-62. IMO. Poleski R. and Szaruga K. (2006). In Bastiaens L., Verbert J., Wislez J.-M., and Verbeeck C., editors, Proceedings of the International Meteor

  3. Meteor radiant mapping with MU radar

    NASA Technical Reports Server (NTRS)

    Watanabe, Jun-Ichi; Nakamura, Tsuko; Tsuda, T.; Tsutsumi, M.; Miyashita, A.; Yoshikawa, M.

    1992-01-01

    The radiant point mapping of meteor showers with the MU radar by using a modified mapping method originally proposed by Morton and Jones (1982) was carried out. The modification is that each meteor echo was weighted by using the beam pattern of the radar system. A preliminary result of the radiant point mapping of the Geminids meteor shower in 1989 is presented.

  4. Croatian Meteor Network: Ongoing work 2015 - 2016

    NASA Astrophysics Data System (ADS)

    Šegon, D.; Vida, D.; Korlević, K.; Andreić, Ž.

    2016-01-01

    Ongoing work of the Croatian Meteor Network (CMN) between the 2015 and 2016 International Meteor Conferences is presented. The current sky coverage is considered, software updates and updates of orbit catalogues are described. Furthermore, the work done on meteor shower searches, international collaborations as well as new fields of research are discussed. Finally, the educational efforts made by the CMN are described.

  5. New trends in meteor radio receivers

    NASA Astrophysics Data System (ADS)

    Rault, Jean-Louis

    2014-01-01

    Recent progresses in low cost—but performing—SDR (software defined radio) technology presents a major breakthrough in the domain of meteor radio observations. Their performances are now good enough for meteor work and should therefore encourage newcomers to join the meteor radio community.

  6. Meteor Crater, AZ

    NASA Technical Reports Server (NTRS)

    2002-01-01

    The Barringer Meteorite Crater (also known as 'Meteor Crater') is a gigantic hole in the middle of the arid sandstone of the Arizona desert. A rim of smashed and jumbled boulders, some of them the size of small houses, rises 50 m above the level of the surrounding plain. The crater itself is nearly a 1500 m wide, and 180 m deep. When Europeans first discovered the crater, the plain around it was covered with chunks of meteoritic iron - over 30 tons of it, scattered over an area 12 to 15 km in diameter. Scientists now believe that the crater was created approximately 50,000 years ago. The meteorite which made it was composed almost entirely of nickel-iron, suggesting that it may have originated in the interior of a small planet. It was 50 m across, weighed roughly 300,000 tons, and was traveling at a speed of 65,000 km per hour. This ASTER 3-D perspective view was created by draping an ASTER bands 3-2-1image over a digital elevation model from the US Geological Survey National Elevation Dataset.

    This image was acquired on May 17, 2001 by the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on NASA's Terra satellite. With its 14 spectral bands from the visible to the thermal infrared wavelength region, and its high spatial resolution of 15 to 90 meters (about 50 to 300 feet), ASTER will image Earth for the next 6 years to map and monitor the changing surface of our planet.

    ASTER is one of five Earth-observing instruments launched December 18,1999, on NASA's Terra satellite. The instrument was built by Japan's Ministry of Economy, Trade and Industry. A joint U.S./Japan science team is responsible for validation and calibration of the instrument and the data products. Dr. Anne Kahle at NASA's Jet Propulsion Laboratory, Pasadena, California, is the U.S. Science team leader; Bjorn Eng of JPL is the project manager. ASTER is the only high resolution imaging sensor on Terra. The Terra mission is part of NASA's Earth Science Enterprise, along

  7. Jasper Seamount: Seven million years of volcanism

    SciTech Connect

    Pringle, M.S. ); Staudigel, H.; Gee, J. )

    1991-04-01

    Jasper Seamount is a young, mid-sized (690 km{sup 3}) oceanic intraplate volcano located about 500 km west-southwest of San Diego, California. Reliable {sup 40}Ar/{sup 39}Ar age data were obtained for several milligram-sized samples of 4 to 10 Ma plagioclase by using a defocused laser beam to clean the samples before fusion. Gee and Staudigel suggested that Jasper Seamount consists of a transitional to tholeiitic shield volcano formed by flank transitional series lavas, overlain by flank alkalic series lavas and summit alkalic series lavas. Twenty-nine individual {sup 40}Ar/{sup 39}Ar laser fusion analyses on nine samples confirm the stratigraphy: 10.3-10.0 Ma for the flank transitonal series, 8.7-7.5 Ma for the flank alkalic series, and 4.8-4.1 Ma for the summit alkalic series. The alkalinity of the lavas clearly increases with time, and there appear to be 1 to 3 m.y. hiatuses between each series. The age data are consistent with the complex magnetic anomaly of Jasper; however the dominant reversed polarity inferred from the anomaly suggests that most of the seamount formed at ca. 11 Ma, prior to the onset of Chron C5N. The duration of volcanism of Jasper Seamount is slightly longer than the duration of volcanism at Hawaiian volcanoes, suggesting that individual age data from seamounts may constrain the age of a seamount only to within about 7 m.y. unless the stage of volcanism can be unambiguously determined. Extrapolating from the results of our study, similar precision in age determinations should be possible on 50 mg of 1 Ma plagioclase from mid-ocean ridge basalt, opening new possibilities in the geochronology of young, low-potassium volcanic rocks.

  8. Comparing Eyewitness-Derived Trajectories of Bright Meteors to Ground Truth Data

    NASA Technical Reports Server (NTRS)

    Moser, D. E.

    2016-01-01

    The NASA Meteoroid Environment Office (MEO) is the only US government agency tasked with analyzing meteors of public interest. When queried about a meteor observed over the United States, the MEO must respond with a characterization of the trajectory, orbit, and size within a few hours. Using observations from meteor networks like the NASA All Sky Fireball Network or the Southern Ontario Meteor Network, such a characterization is often easy. If found, casual recordings from the public and stationary web cameras can be used to roughly analyze a meteor if the camera's location can be identified and its imagery calibrated. This technique was used with great success in the analysis of the Chelyabinsk meteorite fall. But if the event is outside meteor network coverage, if an insufficient number of videos are found, or if the imagery cannot be geolocated or calibrated, a timely assessment can be difficult if not impossible. In this situation, visual reports made by eyewitnesses may be the only resource available. This has led to the development of a tool to quickly calculate crude meteor trajectories from eyewitness reports made to the American Meteor Society. The output is illustrated in Figure 1. A description of the tool, example case studies, and a comparison to ground truth data observed by the NASA All Sky Fireball Network will be presented.

  9. Meteor Beliefs Project: Meteors in the Maori astronomical traditions of New Zealand

    NASA Astrophysics Data System (ADS)

    Britton, Tui R.; Hamacher, Duane W.

    2014-02-01

    We review the literature for perceptions of meteors in the Maori culture of Aotearoa or New Zealand. We examine representations of meteors in religion, story, and ceremony. We find that meteors are sometimes personified as gods or children, or are seen as omens of death and destruction. The stories we found highlight the broad perception of meteors found throughout the Maori culture, and note that some early scholars conflated the terms comet and meteor.

  10. Chasing Meteors With a Microscope.

    ERIC Educational Resources Information Center

    Jones, Richard C.

    1993-01-01

    Describes types of meteors and micrometeorites that enter the Earth's atmosphere. Presents an activity where students collect micrometeorites with a strip of tape in an undisturbed outdoor area. After 24 hours, they examine the tape by sandwiching it between 2 glass slides and view through a microscope at 100X. (PR)

  11. Video spectra of Leonids and other meteors

    NASA Astrophysics Data System (ADS)

    Borovička, Jiří

    2001-11-01

    Video spectra of 33 meteors of medium brightness (+1 to -1 mag) were compared. The intensity of the main meteoric emissions of Mg, Na, Fe, and atmospheric emissions of N2, O, N were studied. The Na/Mg ratio is different in different meteors, showing variations in Na abundance. Moreover, much earlier ablation of Na during the atmospheric entry than of other elements observed in some Leonids and one Orionid, Quadrantid and Leo Minorid evidences fragile structure of those meteoroids. One sporadic meteor was completely deficient in sodium. The strength of atmospheric emission increases with increasing meteor velocity. Taurids are notable by the near-absence of O and N emissions.

  12. Petrologic evolution of the Louisville seamount chain

    NASA Astrophysics Data System (ADS)

    Hawkins, James W.; Lonsdale, Peter F.; Batiza, Rodey

    The Louisville Seamount Chain (LSC) extends for 4300 km from Osbourn Seamount, at the junction of the Tonga and Kermadec Trenches, southeasterly towards the Pacific Antarctic Ridge. The chain is formed of 60 or more seamounts and guyots which are aligned along a trend concentric with the Emperor-Hawaii Chain. The Louisville Chain crosses at a low angle several fracture zones which are part of the Eltanin Fracture Zone system, but there is no apparent genetic relation between the two structures. Rocks collected from the Louisville Chain comprise a spectrum of rock types including alkalic basalt, hawaiite, and basanitoid. Some samples have compositions suggesting that they are transitional to tholeiitic basalt, but no true tholeiites have been collected from the seamounts. Osbourn Seamount, at the westernmost end of the chain, is capped with basanitoid; these have been dated as ˜66 Ma. Clinopyroxene phenocrysts in basaltic composition pebbles and detrital grains of clinopyroxene have been recovered from DSDP site 204, north of Osbourn Seamount, at subbottom depths of 112 to 114 meters (Late? Cretaceous age). Some of these pyroxenes have compositions indicating a tholeiitic parental magma, some were derived from alkalic magmas. Osbourn Seamount or an older neighbor were likely sources of the clastic sediments. This is an indication that the early stages of seamount volcanism included tholeiitic magmas, magmatism subsequently evolved through alkalic and basanitic types. Samples dredged from the carapaces of seamounts east of Osbourn are mainly alkalic basalt, or hawaiite, or both. The young, eastern end of the chain near Long. 139°10'W has alkalic basalt lavas. Modeling of trace element and REE data suggest that small amounts (e.g., 4%) melting of garnet Iherzolite could have provided the parental alkalic basalt magmas. Basanitoids represent slightly higher (˜9%) levels of melting. Element ratios of Ti/Zr, Nb/Zr, Y/Zr, Ba/La, La/Ce, La/Sm, Nb/La suggest that the

  13. Characteristics of Seamounts Near Hawaii as Viewed by GLORIA

    NASA Technical Reports Server (NTRS)

    Bridges, Nathan T.

    1997-01-01

    Using images and data acquired from the GLORIA sonar system, 390 seamounts within the U.S. Hawaiian Exclusive Economic Zone (HEEZ) off Hawaii have been studied. Their diameters range from 1 to 57 km. with most less than 15 km. Seamount abundance increases exponentially with decreasing size. The areal density of observed seamounts having diameters greater than 1 km is 182/10(exp 6) sq km. The theoretical abundance of seamounts of all sizes normalized to a unit area is (309 +/- 17)/10(exp 6) sq km, about an order of magnitude less than other surveyed areas of the Pacific. This may reflect a lower abundance of Cretaceous seamounts in this region, the covering of small seamounts by sediment, or discrepancies from the use of different data sets to derive the abundance statistics. The seamounts have morphologies ranging from steep-sided, flat-topped structures to cones to more amorphous structures; they are similar to volcanoes found elsewhere on the seafloor. A suite of secondary features associated with the seamounts includes summit craters, summit mounds, coalesced boundaries, landslides, and graben. Several seamount chains are aligned parallel to Cretaceous fracture zones, consistent with an origin close to the ancestral East Pacific Rise. Others are aligned parallel to the Necker Ridge, suggesting that they formed contemporaneously with Necker in the plate interior. This observation, together with high abundances of seamounts where other intraplate igneous processes have occurred, suggests some seamounts formed since leaving the spreading center.

  14. The Seamount Catalog: Creating a Data Infrastructure for the Seamount Biogeoscience Network (SBN)

    NASA Astrophysics Data System (ADS)

    Staudigel, H.; Koppers, A. A.; Minett, R.; Staudigel, D.; Konter, J.; Martin, P.

    2006-12-01

    The Seamount Biogeoscience Network (SBN), an international and interdisciplinary association of seamount scientists, argues that seamount research can fundamentally benefit from promoting collaboration and improved data sharing between seamount science disciplines. Seamount scientists cover a wide range of biological sciences, geochemistry, geophysics, geology and physical oceanography. An effective SBN data resource has to be capable of helping access a wide range of disciplinary data relevant to all these fields, but the need for bathymetry data is common to all disciplines. The SBN has used the Seamount Catalog (SC) as its main data portal with a capability of carrying any data, but focusing on bathymetry. Recent SC developments aimed atfacilitating interoperability with other data bases, expanding its contents, and creating an interface that is easy to use on almost any expert level, similarly useful for specialists and interdisciplinary scientists, as well as educational users. Key to interoperability is our choice of giving each seamount an identifier that is made up by an alphanumeric combination of the latitude and longitude values (of the midpoint of the seamount). This identifier serves as a unique name, but it may also be parsed into its geospatial information. Data contents of the SC have now grown to more than 2,500 seamounts worldwide, with a cumulative data inventory of 800 Gb. A variety of search methods are offered by name or location, whereby the latter includes a recent application of "Google Maps" as a particularly promising method of visualizing available information in the user's browser. On the Seamount Catalog website seamounts can be compared or quickly identified through thumbnails and an "index card" with a tabulated description of its size and some vital statistics (size, volume, shape) and a listing of files that can be viewed and/or downloaded from the SC. These files may include any type of data, but the SC focus currently is on

  15. The ecology of seamounts: structure, function, and human impacts.

    PubMed

    Clark, Malcolm R; Rowden, Ashley A; Schlacher, Thomas; Williams, Alan; Consalvey, Mireille; Stocks, Karen I; Rogers, Alex D; O'Hara, Timothy D; White, Martin; Shank, Timothy M; Hall-Spencer, Jason M

    2010-01-01

    In this review of seamount ecology, we address a number of key scientific issues concerning the structure and function of benthic communities, human impacts, and seamount management and conservation. We consider whether community composition and diversity differ between seamounts and continental slopes, how important dispersal capabilities are in seamount connectivity, what environmental factors drive species composition and diversity, whether seamounts are centers of enhanced biological productivity, and whether they have unique trophic architecture. We discuss how vulnerable seamount communities are to fishing and mining, and how we can balance exploitation of resources and conservation of habitat. Despite considerable advances in recent years, there remain many questions about seamount ecosystems that need closer integration of molecular, oceanographic, and ecological research. PMID:21141665

  16. The ecology of seamounts: structure, function, and human impacts.

    PubMed

    Clark, Malcolm R; Rowden, Ashley A; Schlacher, Thomas; Williams, Alan; Consalvey, Mireille; Stocks, Karen I; Rogers, Alex D; O'Hara, Timothy D; White, Martin; Shank, Timothy M; Hall-Spencer, Jason M

    2010-01-01

    In this review of seamount ecology, we address a number of key scientific issues concerning the structure and function of benthic communities, human impacts, and seamount management and conservation. We consider whether community composition and diversity differ between seamounts and continental slopes, how important dispersal capabilities are in seamount connectivity, what environmental factors drive species composition and diversity, whether seamounts are centers of enhanced biological productivity, and whether they have unique trophic architecture. We discuss how vulnerable seamount communities are to fishing and mining, and how we can balance exploitation of resources and conservation of habitat. Despite considerable advances in recent years, there remain many questions about seamount ecosystems that need closer integration of molecular, oceanographic, and ecological research.

  17. The Ecology of Seamounts: Structure, Function, and Human Impacts

    NASA Astrophysics Data System (ADS)

    Clark, Malcolm R.; Rowden, Ashley A.; Schlacher, Thomas; Williams, Alan; Consalvey, Mireille; Stocks, Karen I.; Rogers, Alex D.; O'Hara, Timothy D.; White, Martin; Shank, Timothy M.; Hall-Spencer, Jason M.

    2010-01-01

    In this review of seamount ecology, we address a number of key scientific issues concerning the structure and function of benthic communities, human impacts, and seamount management and conservation. We consider whether community composition and diversity differ between seamounts and continental slopes, how important dispersal capabilities are in seamount connectivity, what environmental factors drive species composition and diversity, whether seamounts are centers of enhanced biological productivity, and whether they have unique trophic architecture. We discuss how vulnerable seamount communities are to fishing and mining, and how we can balance exploitation of resources and conservation of habitat. Despite considerable advances in recent years, there remain many questions about seamount ecosystems that need closer integration of molecular, oceanographic, and ecological research.

  18. Recent Advances in Video Meteor Photometry

    NASA Technical Reports Server (NTRS)

    Swift, Wesley R.; Suggs, Robert M.; Meachem, Terry; Cooke, William J.

    2003-01-01

    One of the most common (and obvious) problems with video meteor data involves the saturation of the output signal produced by bright meteors, resulting in the elimination of such meteors from photometric determinations. It is important to realize that a "bright" meteor recorded by intensified meteor camera is not what would be considered "bright" by a visual observer - indeed, many Generation II or III camera systems are saturated by meteors with a visual magnitude of 3, barely even noticeable to the untrained eye. As the relatively small fields of view (approx.30 ) of the camera systems captures at best modest numbers of meteors, even during storm peaks, the loss of meteors brighter than +3 renders the determination of shower population indices from video observations even more difficult. Considerable effort has been devoted by the authors to the study of the meteor camera systems employed during the Marshall Space Flight Center s Leonid ground-based campaigns, and a calibration scheme has been devised which can extend the useful dynamic range of such systems by approximately 4 magnitudes. The calibration setup involves only simple equipment, available to amateur and professional, and it is hoped that use of this technique will make for better meteor photometry, and move video meteor analysis beyond the realm of simple counts.

  19. Determination of the Meteor Limiting Magnitude

    NASA Technical Reports Server (NTRS)

    Kingery, A.; Blaauw, R.; Cooke, W. J.

    2016-01-01

    The limiting meteor magnitude of a meteor camera system will depend on the camera hardware and software, sky conditions, and the location of the meteor radiant. Some of these factors are constants for a given meteor camera system, but many change between meteor shower or sporadic source and on both long and short timescales. Since the limiting meteor magnitude ultimately gets used to calculate the limiting meteor mass for a given data set, it is important to have an understanding of these factors and to monitor how they change throughout the night, as a 0.5 magnitude uncertainty in limiting magnitude translates to a uncertainty in limiting mass by a factor of two.

  20. Science priorities for seamounts: research links to conservation and management.

    PubMed

    Clark, Malcolm R; Schlacher, Thomas A; Rowden, Ashley A; Stocks, Karen I; Consalvey, Mireille

    2012-01-01

    Seamounts shape the topography of all ocean basins and can be hotspots of biological activity in the deep sea. The Census of Marine Life on Seamounts (CenSeam) was a field program that examined seamounts as part of the global Census of Marine Life (CoML) initiative from 2005 to 2010. CenSeam progressed seamount science by collating historical data, collecting new data, undertaking regional and global analyses of seamount biodiversity, mapping species and habitat distributions, challenging established paradigms of seamount ecology, developing new hypotheses, and documenting the impacts of human activities on seamounts. However, because of the large number of seamounts globally, much about the structure, function and connectivity of seamount ecosystems remains unexplored and unknown. Continual, and potentially increasing, threats to seamount resources from fishing and seabed mining are creating a pressing demand for research to inform conservation and management strategies. To meet this need, intensive science effort in the following areas will be needed: 1) Improved physical and biological data; of particular importance is information on seamount location, physical characteristics (e.g. habitat heterogeneity and complexity), more complete and intensive biodiversity inventories, and increased understanding of seamount connectivity and faunal dispersal; 2) New human impact data; these shall encompass better studies on the effects of human activities on seamount ecosystems, as well as monitoring long-term changes in seamount assemblages following impacts (e.g. recovery); 3) Global data repositories; there is a pressing need for more comprehensive fisheries catch and effort data, especially on the high seas, and compilation or maintenance of geological and biodiversity databases that underpin regional and global analyses; 4) Application of support tools in a data-poor environment; conservation and management will have to increasingly rely on predictive modelling

  1. Science Priorities for Seamounts: Research Links to Conservation and Management

    PubMed Central

    Clark, Malcolm R.; Schlacher, Thomas A.; Rowden, Ashley A.; Stocks, Karen I.; Consalvey, Mireille

    2012-01-01

    Seamounts shape the topography of all ocean basins and can be hotspots of biological activity in the deep sea. The Census of Marine Life on Seamounts (CenSeam) was a field program that examined seamounts as part of the global Census of Marine Life (CoML) initiative from 2005 to 2010. CenSeam progressed seamount science by collating historical data, collecting new data, undertaking regional and global analyses of seamount biodiversity, mapping species and habitat distributions, challenging established paradigms of seamount ecology, developing new hypotheses, and documenting the impacts of human activities on seamounts. However, because of the large number of seamounts globally, much about the structure, function and connectivity of seamount ecosystems remains unexplored and unknown. Continual, and potentially increasing, threats to seamount resources from fishing and seabed mining are creating a pressing demand for research to inform conservation and management strategies. To meet this need, intensive science effort in the following areas will be needed: 1) Improved physical and biological data; of particular importance is information on seamount location, physical characteristics (e.g. habitat heterogeneity and complexity), more complete and intensive biodiversity inventories, and increased understanding of seamount connectivity and faunal dispersal; 2) New human impact data; these shall encompass better studies on the effects of human activities on seamount ecosystems, as well as monitoring long-term changes in seamount assemblages following impacts (e.g. recovery); 3) Global data repositories; there is a pressing need for more comprehensive fisheries catch and effort data, especially on the high seas, and compilation or maintenance of geological and biodiversity databases that underpin regional and global analyses; 4) Application of support tools in a data-poor environment; conservation and management will have to increasingly rely on predictive modelling

  2. Science priorities for seamounts: research links to conservation and management.

    PubMed

    Clark, Malcolm R; Schlacher, Thomas A; Rowden, Ashley A; Stocks, Karen I; Consalvey, Mireille

    2012-01-01

    Seamounts shape the topography of all ocean basins and can be hotspots of biological activity in the deep sea. The Census of Marine Life on Seamounts (CenSeam) was a field program that examined seamounts as part of the global Census of Marine Life (CoML) initiative from 2005 to 2010. CenSeam progressed seamount science by collating historical data, collecting new data, undertaking regional and global analyses of seamount biodiversity, mapping species and habitat distributions, challenging established paradigms of seamount ecology, developing new hypotheses, and documenting the impacts of human activities on seamounts. However, because of the large number of seamounts globally, much about the structure, function and connectivity of seamount ecosystems remains unexplored and unknown. Continual, and potentially increasing, threats to seamount resources from fishing and seabed mining are creating a pressing demand for research to inform conservation and management strategies. To meet this need, intensive science effort in the following areas will be needed: 1) Improved physical and biological data; of particular importance is information on seamount location, physical characteristics (e.g. habitat heterogeneity and complexity), more complete and intensive biodiversity inventories, and increased understanding of seamount connectivity and faunal dispersal; 2) New human impact data; these shall encompass better studies on the effects of human activities on seamount ecosystems, as well as monitoring long-term changes in seamount assemblages following impacts (e.g. recovery); 3) Global data repositories; there is a pressing need for more comprehensive fisheries catch and effort data, especially on the high seas, and compilation or maintenance of geological and biodiversity databases that underpin regional and global analyses; 4) Application of support tools in a data-poor environment; conservation and management will have to increasingly rely on predictive modelling

  3. Extraterrestrial meteors: a martian meteor and its parent comet.

    PubMed

    Selsis, Franck; Lemmon, Mark T; Vaubaillon, Jérémie; Bell, James F

    2005-06-01

    Regular meteor showers occur when a planet approaches the orbit of a periodic comet--for example, the Leonid shower is evident around 17 November every year as Earth skims past the dusty trail of comet Tempel-Tuttle. Such showers are expected to occur on Mars as well, and on 7 March last year, the panoramic camera of Spirit, the Mars Exploration Rover, revealed a curious streak across the martian sky. Here we show that the timing and orientation of this streak, and the shape of its light curve, are consistent with the existence of a regular meteor shower associated with the comet Wiseman-Skiff, which could be characterized as martian Cepheids. PMID:15931208

  4. Extraterrestrial meteors: a martian meteor and its parent comet.

    PubMed

    Selsis, Franck; Lemmon, Mark T; Vaubaillon, Jérémie; Bell, James F

    2005-06-01

    Regular meteor showers occur when a planet approaches the orbit of a periodic comet--for example, the Leonid shower is evident around 17 November every year as Earth skims past the dusty trail of comet Tempel-Tuttle. Such showers are expected to occur on Mars as well, and on 7 March last year, the panoramic camera of Spirit, the Mars Exploration Rover, revealed a curious streak across the martian sky. Here we show that the timing and orientation of this streak, and the shape of its light curve, are consistent with the existence of a regular meteor shower associated with the comet Wiseman-Skiff, which could be characterized as martian Cepheids.

  5. High temperature condensates among meteors

    NASA Technical Reports Server (NTRS)

    Wilkening, L. L.

    1975-01-01

    It is noted that two meteors which exhibited no lines of iron or sodium in their spectra have been tentatively attributed to aubrites in order to explain their lack of iron. It is shown, however, that no meteorites, including aubrites, have simultaneously low abundances of iron and sodium and that possible parent materials other than aubrites must be considered for the observed meteors. Other possible parent materials considered in this letter include melilite and diopside, two minerals containing both Ca and Mg but neither Fe nor Na. It is suggested that meteoroids rich in Ca and Mg but lacking Fe and Na might form a reservoir for the so-called 'lost' elements (Ca, Mg, Al, Ti, the lanthanides, and other refractory elements) which are depleted in ordinary and enstatite chondrites relative to cosmic abundances.

  6. Meteors in the Earth's Atmosphere

    NASA Astrophysics Data System (ADS)

    Murad, Edmond; Williams, Iwan P.

    2002-09-01

    1. Introduction Iwan Williams and Edmond Murad; 2. The evolution of meteoroid streams Iwan Williams; 3. Space dust measurements Eberhard Grun, Valeri Dikarev, Harald Kruger and Markus Landgraf; 4. Extraterrestrial dust in the near-Earth environment George Flynn; 5. Detection and analysis procedures for visual photographic and image intensified CCD meteor observations Robert Hawkes; 6. Radar observations W. Jack Baggaley; 7. Meteor trails as observed by Lidar Ulf von Zahn, J. Hoffner and William McNeil; 8. In situ measurements of meteoritic ions Joseph Grebowsky and Arthur Aikin; 9. Collected extraterrestrial materials: interplanetary dust particles, micrometeorites, meteorites, and meteoritic dust Frans Rietmeijer; 10. Meteoroid impacts on spacecraft; Luigi Foschini; 11. Models of meteoritic metals in the atmosphere William McNeil, Edmond Murad and John Plane; 12. Laboratory studies of meteoritic metal chemistry John Plane; 13. Summary and future outlook Edmond Murad and Iwan Williams.

  7. The ALTAIR Meteor Measurements Program

    NASA Technical Reports Server (NTRS)

    Cooke, William J.

    2007-01-01

    Established in late 2006, the Meteor Measurements Program is in the process of using the ALTAIR radar located on Kwajelein Atoll to obtain radar observations of sporadic and shower meteoroids. The goals are to determine meteoroid masses, orbits, ballistic coefficients and densities, which shall be provided to the Meteoroid Environment Office (MEO) at Marshall Space Flight Center. These data and analyses shall then be used by the MEO to 1) Add a realistic density distribution to the new Meteoroid Engineering Model (MEM), which is the specified environment for vehicle design in the NASA Constellation (return to Moon) program. This program is the implementation of President Bush's Vision for Space Exploration (VSE). 2) Investigate the meteoroid velocity distribution at smaller masses. 3) Strive to understand the differences (biases) in meteoroid observations produced by systems like ALTAIR and those of the meteor patrol radars, such as the University of Western Ontario's CMOR system. This paper outlines the program details and its progress.

  8. Meteor observations under the INASAN supervision

    NASA Astrophysics Data System (ADS)

    Kartashova, A. P.; Bagrov, A. V.

    2012-09-01

    Meteor observations have the specific property: we do not know in advance neither area on the celestial sphere, not the time when the event occurs. Besides that, a meteor flash in the atmosphere has duration few seconds or less, and it is hard problem to gather enough photons from it to register a faint or fast meteor. There are a number of tasks in meteor astronomy for solution of which not only a simple registration of meteors in the optical range is required, but a high spatial and time resolution as well. Television method is the most acceptable for such a case and is widely used in the practice of meteor observations. Television meteor observations in Russia are carried out under the Institute of Astronomy of the Russian Academy of Sciences (INASAN) supervision in different regions of Russia: Moscow region, Irkutsk, Ryazan and North Caucasus. The TV system PatrolCa designed for observations in the wide field of view (the ordinary for most of meteor cameras), consists of the following components: the high resolution cameras Watec LCL-902HS, the wide-angle photograph objectives Canon 6/0.8 (F=6 mm, the aperture 1:0.8). The cameras have fields of view of 50°x40° and have a limiting magnitude (for meteors) of +4 m ÷ +5 m. The FAVOR (FAst Variability Optical Registrator) camera is used for observations of faint meteors at the North Caucasus [1]. The basic components of this camera are the following: the high-aperture lense objective with the aperture 150 mm and the focal length 180mm (the aperture 1:1.2), the image intensifier, the objective reversal, CCD receiver "Videoscan" VS-СTT285 2001. The CCD "Sony" ICX285 has format 1380 х 1024 pixels. The camera has a field of view of 18 ° х 20°, and has a limiting magnitude of above +10m (for meteors). The two cameras similar to FAVOR (named SMAC) were designed for double-station observations of faint meteors. The results of observations at these cameras are presented. The observations were held by both methods

  9. Kharkiv Meteor Radar System (the XX Age)

    NASA Astrophysics Data System (ADS)

    Kolomiyets, S. V.

    2012-09-01

    Kharkiv meteor radar research are of historic value (Kolomiyets and Sidorov 2007). Kharkiv radar observations of meteors proved internationally as the best in the world, it was noted at the IAU General Assembly in 1958. In the 1970s Kharkiv meteor automated radar system (MARS) was recommended at the international level as a successful prototype for wide distribution. Until now, this radar system is one of the most sensitive instruments of meteor radars in the world for astronomical observations. In 2004 Kharkiv meteor radar system is included in the list of objects which compose the national property of Ukraine. Kharkiv meteor radar system has acquired the status of the important historical astronomical instrument in world history. Meteor Centre for researching meteors in Kharkiv is a analogue of the observatory and performs the same functions of a generator and a battery of special knowledge and skills (the world-famous studio). Kharkiv and the location of the instrument were brand points on the globe, as the place where the world-class meteor radar studies were carried out. They are inscribed in the history of meteor astronomy, in large letters and should be immortalized on a world-wide level.

  10. SPA Meteor Section Results: 2006

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair

    2010-12-01

    A summary of the main analyzed results and other information provided to the SPA Meteor Section from 2006 is presented and discussed. Events covered include: the radio Quadrantid maximum on January 3/4; an impressive fireball seen from parts of England, Belgium and the Netherlands at 22h53m51s UT on July 18, which was imaged from three EFN stations as well; the Southern delta-Aquarid and alpha-Capricornid activity from late July and early August; the radio Perseid maxima on August 12/13; confirmation that the October 5/6 video-meteor outburst was not observed by radio; visual and radio findings from the strong, bright-meteor, Orionid return in October; another impressive UK-observed fireball on November 1/2, with an oil painting of the event as seen from London; the Leonids, which produced a strong visual maximum around 04h-05h UT on November 18/19 that was recorded much less clearly by radio; radio and visual reports from the Geminids, with a note regarding NASA-observed Geminid lunar impact flashes; and the Ursid outburst recorded by various techniques on December 22.

  11. Morphology and distribution of seamounts surrounding Easter Island

    USGS Publications Warehouse

    Rappaport, Y.; Naar, D.F.; Barton, C.C.; Liu, Z.-J.; Hey, R.N.

    1997-01-01

    We investigate the morphology and distribution of a seamount population on a section of seafloor influenced by both superfast seafloor spreading and hotspot volcanism. The population under investigation is part of a broad chain of seamounts extending eastward from the East Pacific Rise, near Easter Island. In order to define the morphological variability of the seamounts, basal shape, cross-sectional area, volume, flatness, and flank slope are plotted against height for 383 seamounts with heights greater than 200 m, based on bathymetry data collected by GLORI-B and SeaBeam 2000, during three cruises onboard the R/V Melville in the spring of 1993. Nearly complete swath mapping coverage of the seamounts is available for the analysis of size and shape distribution. We quantitatively describe the seamount population of this active region, in which seamounts cover ???27% of the seafloor, and account for ???4.2% of the total crustal volume. Over 50% of the total volume (61,000 km3) of seamounts used in this study is made up by the 14 largest seamounts, and the remaining volume is made up by the 369 smaller seamounts (>200 m in height). Our analysis indicates there are at least two seamount populations in the Easter Island-Salas y Gomez Island (25??-29??S, 113??-104??W) study area. One population of seamounts is composed of short seamounts (1200 m), shield-like, pointy cones (flatness ???1200 m) originate exclusively from a hotspot source, but only a portion of the smaller volcanoes (

  12. The Seamount Catalog in EarthRef.org

    NASA Astrophysics Data System (ADS)

    Keizer, P.; Koppers, A.; Staudigel, H.; Helly, J.

    2001-12-01

    Seamounts are prominent features on the ocean floor that provide us with important insights to geology, geochemistry, geophysics and paleoclimate. To make accessible a diverse set of seamount data we developed the Seamount Catalog on the EarthRef.org web site that is accessible via http://earthref.org/databases/SC/. The goal of our effort is to provide simple access to the widest possible variety in digital data files as related to seamount research in a geospatial context. Each seamount is described in terms of its location, basic morphological features, and the types of data available in the catalog. The Seamount Catalog includes a series of basic bathymetry maps, processed grid files and original multibeam data. At least one screen-optimized JPEG file is available for online viewing and the remaining (higher resolution) files are directly downloadable from the EarthRef.org web site. The grid files are based on multibeam bathymetry data merged with the predicted bathymetry database of Smith and Sandwell (1996; 1997). The Seamount Catalog data objects are extensively described in terms of metadata allowing for searches by location (lat/lon), region name, seamount name, sample name or reference. We hope to further develop the Seamount Catalog by adding geophysical and other seamount data, expanding its metadata catalog, working towards a metadata interchange format (*.mif) and establishing interoperability with other data bases. The geospatial character of the Seamount Catalog would allow for interoperability between existing geochemistry, paleomagnetic and biological (biota) databases. Data files available for downloading will be stored using the Storage Resource Broker technology (SRB) while the generated metadata will be stored in the Seamount Catalog itself. Such developments represent the first steps towards the creation of a digital seamount research environment that includes electronic access to data and ultimately also the tools for working with the data.

  13. Big data era in meteor science

    NASA Astrophysics Data System (ADS)

    Vinković, D.; Gritsevich, M.; Srećković, V.; Pečnik, B.; Szabó, G.; Debattista, V.; Škoda, P.; Mahabal, A.; Peltoniemi, J.; Mönkölä, S.; Mickaelian, A.; Turunen, E.; Kákona, J.; Koskinen, J.; Grokhovsky, V.

    2016-01-01

    Over the last couple of decades technological advancements in observational techniques in meteor science have yielded drastic improvements in the quality, quantity and diversity of meteor data, while even more ambitious instruments are about to become operational. This empowers meteor science to boost its experimental and theoretical horizons and seek more advanced science goals. We review some of the developments that push meteor science into the big data era that requires more complex methodological approaches through interdisciplinary collaborations with other branches of physics and computer science. We argue that meteor science should become an integral part of large surveys in astronomy, aeronomy and space physics, and tackle the complexity of micro-physics of meteor plasma and its interaction with the atmosphere.

  14. Meteor Beliefs Project: Meteoric Imagery in SF, Part V: This Island Earth

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair; Gheorghe, Andrei Dorian

    2007-04-01

    The classic 1950s science fiction film This Island Earth is discussed for its meteoric elements, along with a more recent movie which pokes fun at it, by way of celebrating the Meteor Beliefs Project's fourth anniversary.

  15. The NIWA seamount sled: An effective epibenthic sledge for sampling epifauna on seamounts and rough seafloor

    NASA Astrophysics Data System (ADS)

    Clark, Malcolm R.; Stewart, Rob

    2016-02-01

    Epibenthic sleds, sledges and dredges have been widely used for sampling deep-sea macro and megafaunal communities, providing extensive information on benthic biodiversity and distribution patterns. Different countries and institutes have developed a variety of gear types, but these are often unsuitable for sampling rough seafloor, such as seamount and ridge topography. The NIWA seamount sled, a form of epibenthic sledge, is an inexpensive yet robust and versatile sampling device used to obtain invertebrate and rock samples. It incorporates features from a number of existing designs that have produced a versatile sled that can be used on all habitats from mud through to steep and rocky seamounts. It has been used for many research surveys around New Zealand, where it has proven an efficient sampler of target fauna (large macro- and mega-benthic epifauna). Its design has also been adopted by institutes in France and China for surveying seamounts, and it is suggested it could be used as a simple standardised design for sampling seamounts internationally.

  16. The origin of the Canary Island Seamount Province - new ages of old seamounts.

    PubMed

    van den Bogaard, Paul

    2013-01-01

    The Canary Island Seamount Province forms a scattered hotspot track on the Atlantic ocean floor ~1300 km long and ~350 km wide, perpendicular to lithospheric fractures, and parallel to the NW African continental margin. New (40)Ar/(39)Ar datings show that seamount ages vary from 133 Ma to 0.2 Ma in the central archipelago, and from 142 Ma to 91 Ma in the southwest. Combining (40)Ar/(39)Ar ages with plate tectonic reconstructions, I find that the temporal and spatial distribution of seamounts is irreconcilable with a deep fixed mantle plume origin, or derivation from passive mantle upwelling beneath a mid-ocean ridge. I conclude that shallow mantle upwelling beneath the Atlantic Ocean basin off the NW African continental lithosphere flanks produced recurrent melting anomalies and seamounts from the Late Jurassic to Recent, nominating the Canary Island Seamount Province as oldest hotspot track in the Atlantic Ocean, and most long-lived preserved on earth. PMID:23838703

  17. The origin of the Canary Island Seamount Province - new ages of old seamounts.

    PubMed

    van den Bogaard, Paul

    2013-01-01

    The Canary Island Seamount Province forms a scattered hotspot track on the Atlantic ocean floor ~1300 km long and ~350 km wide, perpendicular to lithospheric fractures, and parallel to the NW African continental margin. New (40)Ar/(39)Ar datings show that seamount ages vary from 133 Ma to 0.2 Ma in the central archipelago, and from 142 Ma to 91 Ma in the southwest. Combining (40)Ar/(39)Ar ages with plate tectonic reconstructions, I find that the temporal and spatial distribution of seamounts is irreconcilable with a deep fixed mantle plume origin, or derivation from passive mantle upwelling beneath a mid-ocean ridge. I conclude that shallow mantle upwelling beneath the Atlantic Ocean basin off the NW African continental lithosphere flanks produced recurrent melting anomalies and seamounts from the Late Jurassic to Recent, nominating the Canary Island Seamount Province as oldest hotspot track in the Atlantic Ocean, and most long-lived preserved on earth.

  18. The origin of the Canary Island Seamount Province - New ages of old seamounts

    PubMed Central

    van den Bogaard, Paul

    2013-01-01

    The Canary Island Seamount Province forms a scattered hotspot track on the Atlantic ocean floor ~1300 km long and ~350 km wide, perpendicular to lithospheric fractures, and parallel to the NW African continental margin. New 40Ar/39Ar datings show that seamount ages vary from 133 Ma to 0.2 Ma in the central archipelago, and from 142 Ma to 91 Ma in the southwest. Combining 40Ar/39Ar ages with plate tectonic reconstructions, I find that the temporal and spatial distribution of seamounts is irreconcilable with a deep fixed mantle plume origin, or derivation from passive mantle upwelling beneath a mid-ocean ridge. I conclude that shallow mantle upwelling beneath the Atlantic Ocean basin off the NW African continental lithosphere flanks produced recurrent melting anomalies and seamounts from the Late Jurassic to Recent, nominating the Canary Island Seamount Province as oldest hotspot track in the Atlantic Ocean, and most long-lived preserved on earth. PMID:23838703

  19. Bi-telescopic, deep, simultaneous meteor observations

    NASA Technical Reports Server (NTRS)

    Taff, L. G.

    1986-01-01

    A statistical summary is presented of 10 hours of observing sporadic meteors and two meteor showers using the Experimental Test System of the Lincoln Laboratory. The observatory is briefly described along with the real-time and post-processing hardware, the analysis, and the data reduction. The principal observational results are given for the sporadic meteor zenithal hourly rates. The unique properties of the observatory include twin telescopes to allow the discrimination of meteors by parallax, deep limiting magnitude, good time resolution, and sophisticated real-time and post-observing video processing.

  20. The 25th International Meteor Conference

    NASA Astrophysics Data System (ADS)

    Roggemans, Paul

    2006-08-01

    Since the founding of the International Meteor Organization, the International Meteor Conferences guaranteed the vital personal contacts between its members. In recent years IMCs were sometimes assumed to have started with IMO. However, the IMCs grew out of a much older initiative, the Meteor Seminars that started in 1979, later also called International Meteor Weekends. These events played a crucial role in the making of the IMO. The 2006 IMC in Roden, the Netherlands later this year is in fact a jubilee edition as it is the 25th edition since the very beginning in 1979!

  1. Zooplankton distribution around four eastern North Pacific seamounts

    NASA Astrophysics Data System (ADS)

    Haury, Loren; Fey, Connie; Newland, Carol; Genin, Amatzia

    2000-01-01

    The effects of seamounts on the distribution of zooplankton were investigated at four seamounts in the northeastern Pacific. The following hypotheses were tested: (1) mesoscale gaps of reduced abundance of migrating zooplankton develop over seamounts every night; (2) fine-scale patchiness is augmented within these gaps and in the region downstream of seamounts; and (3) increased numbers of crustacean carcasses occur over seamounts. Gaps are expected because most zooplankton that descend over shallow topography at dawn are either eaten by resident predators or are advected off the summit, while fine-scale patchiness should result from lateral shear between the gap and the surrounding zooplankton-rich waters. Copepod carcasses should be more abundant over seamounts than the surrounding water because of the increased predation at seamounts. Zooplankton distributions were determined from net samples and acoustic records. Water column properties were measured with a CTD and hydrocasts, and currents by moored current meters, acoustic current profilers and drifter drogues. Zooplankton gaps were found over three of the four seamounts surveyed, but not on every survey of each seamount. Only three of the surveys provided the information necessary to test the patchiness hypothesis; on two of these increased patchiness and carcass abundance were found associated with gaps. When no gap was observed over a seamount, there was no evidence of increased carcass abundance or enhanced patchiness, indicating that the three phenomena are temporally and spatially linked. Copepod carcasses were found in the intestines of small fish sampled at the same time as the zooplankton. The fish, along with crustacean predators like euphausiids, are the likely source for the carcasses. Seamounts appear to be an important cause of enhanced zooplankton patchiness on scales ranging from 100s of meters to areas larger than the seamounts themselves.

  2. Geophysical Age Dating of Seamounts using Dense Core Flexure Model

    NASA Astrophysics Data System (ADS)

    Hwang, Gyuha; Kim, Seung-Sep

    2016-04-01

    Lithospheric flexure of oceanic plate is thermo-mechanical response of an elastic plate to the given volcanic construct (e.g., seamounts and ocean islands). If the shape and mass of such volcanic loads are known, the flexural response is governed by the thickness of elastic plate, Te. As the age of oceanic plate increases, the elastic thickness of oceanic lithosphere becomes thicker. Thus, we can relate Te with the age of plate at the time of loading. To estimate the amount of the driving force due to seamounts on elastic plate, one needs to approximate their density structure. The most common choice is uniform density model, which utilizes constant density value for a seamount. This approach simplifies computational processes for gravity prediction and error estimates. However, the uniform density model tends to overestimate the total mass of the seamount and hence produces more positive gravitational contributions from the load. Minimization of gravity misfits using uniform density, therefore, favors thinner Te in order to increase negative contributions from the lithospheric flexure, which can compensate for the excessive positives from the seamount. An alternative approach is dense core model, which approximate the heterogeneity nature of seamount density as three bodies of infill sediment, edifice, and dense core. In this study, we apply the dense core model to the Louisville Seamount Chain for constraining flexural deformation. We compare Te estimates with the loading time of the examined seamounts to redefine empirical geophysical age dating of seamounts.

  3. Uncertainties in MARS Meteor Orbit Radar Data

    NASA Astrophysics Data System (ADS)

    Kolomiyets, S. V.

    2015-03-01

    The uncertainties in meteor radar data and the problem of hyperbolic meteors are interconnected. Meteor orbital data, obtained by the Meteor Automatic Radar System (MARS) at the Kharkiv Institute of Radio Electronics, Ukraine, was used to develop the algorithm to determine the uncertainties of the orbital elements obtained by radar systems such as MARS. We have constructed the empirical model of the distribution of uncertainties in the orbital elements of meteor radar data. MARS had a high effective sensitivity (the limiting magnitude of observed meteors was close to 12 ^ M) and was capable to carry out comprehensive geophysical and astronomical studies of meteors. When we register meteor numbers, radiants, meteoroid velocities, we can talk about astronomical observations. The main objective of meteor astronomy research is to determine the orbit of the meteoroid, in other words, to study a meteoroid as an astronomical object of the Solar System. Sometimes meteoroids may have an interstellar origin. Such meteoroids usually have hyperbolic orbits (i.e. with eccentricities e>1). However, hyperbolic orbits of meteoroids may have another origin, e.g. arise due to errors of observations (primarily due to the errors of eccentricities - σe). To correctly interpret the astronomical data, it is necessary to know how the errors are calculated. In this paper, we estimated the uncertainties in the Kharkiv meteor radar data (the average σe ~0.2) and discussed their connection to the problem of hyperbolic meteors. We obtained ~0.8% of total number of meteoroid orbits in 1975, which we named "real" hyperboles, i.e. with eccentricities more or equal 1+2σe.

  4. Croatian Meteor Network: ongoing work 2014 - 2015

    NASA Astrophysics Data System (ADS)

    Šegon, D.; Andreić, Ž.; Korlević, K.; Vida, D.

    2015-01-01

    Ongoing work mainly between 2014-2015 International Meteor Conferences (IMC) has been presented. Current sky coverage, software updates, orbit catalogues updates, shower search updates, international collaboration as well as new fields of research and educational efforts made by the Croatian Meteor Network are described.

  5. The Makings of Meteor Astronomy: Part XIII

    NASA Astrophysics Data System (ADS)

    Beech, M.

    1996-10-01

    In 1848, Sir John Lubbock advanced the hypothesis that meteors shine by reflected sunlight. He developed a set of equations describing the geometry of meteor encounters, and for a decade or so, his idea was at least marginally supported by other observers.

  6. Models of sporadic meteor body distributions

    NASA Technical Reports Server (NTRS)

    Andreev, V. V.; Belkovich, O. I.

    1987-01-01

    The distribution of orbital elements and flux density over the celestial sphere are the most common forms of representation of the meteor body distribution in the vicinity of the Earth's orbit. The determination of flux density distribution of sporadic meteor bodies was worked out. The method and its results are discussed.

  7. Activity of the Lyrid meteor stream

    NASA Technical Reports Server (NTRS)

    Lindblad, Bertil A.; Porubcan, V.

    1992-01-01

    The activity of the Lyrid meteor stream is in most years fairly low with a visual rate at maximum (21-22 April) of 5-10 meteors per hour. Short bursts of very high Lyrid activity, with visual hourly rates of 100 or more, have sometimes been reported. These observations generally refer to faint visual meteors. The reported bursts of high activity have occurred in a very narrow interval of solar longitudes (deg 31.24 to 31.38 equinox 1950.0), while the recurrent or 'normal' maximum for bright meteors occurs at solar longitude deg 31.6, or slightly later. A mass separation of the meteors in the shower is thus indicated.

  8. Sporadic E-Layers and Meteor Activity

    NASA Astrophysics Data System (ADS)

    Alimov, Obid

    2016-07-01

    In average width it is difficult to explain variety of particularities of the behavior sporadic layer Es ionospheres without attraction long-lived metallic ion of the meteoric origin. Mass spectrometric measurements of ion composition using rockets indicate the presence of metal ions Fe+, Mg+, Si+, Na+, Ca+, K+, Al+ and others in the E-region of the ionosphere. The most common are the ions Fe+, Mg+, Si+, which are primarily concentrated in the narrow sporadic layers of the ionosphere at altitudes of 90-130 km. The entry of meteoric matter into the Earth's atmosphere is a source of meteor atoms (M) and ions (M +) that later, together with wind shear, produce midlatitude sporadic Es layer of the ionosphere. To establish the link between sporadic Es layer and meteoroid streams, we proceeded from the dependence of the ionization coefficient of meteors b on the velocity of meteor particles in different meteoroid streams. We investigated the dependence of the critical frequency f0Es of sporadic E on the particle velocity V of meteor streams and associations. It was established that the average values of f0Es are directly proportional to the velocity V of meteor streams and associations, with the correlation coefficient of 0.53 < R < 0.74. Thus, the critical frequency of the sporadic layer Es increases with the increase of particle velocity V in meteor streams, which indicates the direct influence of meteor particles on ionization of the lower ionosphere and formation of long-lived metal atoms M and ions M+ of meteoric origin.

  9. Geochemistry of hydrothermal plume in the Suiyo Seamount Caldera.

    NASA Astrophysics Data System (ADS)

    Shitashima, K.; Maeda, Y.

    2002-12-01

    Chemical compounds of the hot basalt origin are discharged into the deep ocean via hydrothermal plume by the deep-sea hydrothermal activity. The hydrothermal plume is widely diffused to the ocean by mixing with ambient seawater. Chemical reactions and interactions with microorganisms in the diffusion process of the hydrothermal plume are important to comprehend the oceanic geochemical cycles. Recently, it has been clarified that the variation of hydrothermal activity is greatly controlled in the tidal current. Not only geochemical observation but also physical observation, such as water current measurement, are necessary for the understanding of the deep-sea hydrothermal systems including the behavior of hydrothermal plume. In order to observe the diffusion process of hydrothermal plumes, sampling and chemical mapping of the hydrothermal plume and measurement of water current were carried out at the Suiyo Seamount Caldera during research cruises under the ?Archaean Park? project funded by MEXT. The three-dimensional acoustic current meters were moored at the height of 13m and 125m above the bottom in the Suiyo Seamount Caldera. At the 13m height, average water current speed and current direction were 10.46 cm/second and 228.1 degrees, respectively, and maximum water current speed was over 40.46 cm/second. On the other hand, average water current speed and current direction at the 125m height were 3.87 cm/second and 57.8 degrees, respectively. The strong water current of the southwest direction in 24 hours periods existed near bottom of the caldera. In addition, downward current and water temperature depreciation were observed, when there was the strong current in 24 hours periods. These results suggest that the low-temperature ocean water around the Suiyo Seamount flows toward the bottom of caldera periodically. The mini CTDT-RMS mounted twelve 1.2L Niskin bottles and the in-situ pH sensor were installed on the ROV or manned submersible. The hydrothermal plume

  10. Emplacement and Growth of Serpentinite Seamounts on the Mariana Forearc

    NASA Astrophysics Data System (ADS)

    Oakley, A. J.; Taylor, B.; Moore, G. F.; Fryer, P.; Morgan, J. K.; Goodliffe, A. M.

    2004-12-01

    Seamounts comprised primarily of serpentinite muds are found on the outer forearc of the Izu-Bonin-Mariana subduction system. They represent some of the first material outputs of the recycling process that takes place in subduction zones. Therefore, understanding their evolution is necessary to correctly quantify the flux of material through the subduction system. Serpentinite seamounts have been described as mud diapirs, mud volcanoes, uplifted blocks of mantle material, and a composite of the latter two. Multi-channel seismic (MCS) data collected in 2002 from the outer Mariana forearc imaged, for the first time, the large-scale internal structure of these seamounts. These data, combined with new bathymetry, have provided insight into how the seamounts grow and deform with time and have allowed us to evaluate proposed models for their formation. The serpentinite seamounts rest on faulted and sedimented Mariana forearc basement. Flank flows of serpentinite muds downlap existing forearc substrate, leaving the underlying stratigraphy largely undisturbed. Reflections located 3.5-5 km beneath forearc basement may represent Moho, suggesting that the seamounts are built on anomalously thin forearc crust. A strong reflection at the summit of Big Blue, the largest serpentinite seamount in the Mariana Forearc, represents a collapse structure that has been partially in-filled by younger muds, supporting the idea that serpentinite seamount growth is episodic. Basal thrusts that incorporate forearc sediments at the toe of Turquoise Seamount provide evidence for seamount settling and lateral growth. We are conducting numerical simulations of seamount growth and evolution using the discrete element method (DEM), previously used to examine gravity spreading phenomena in magmatic volcanoes. Simulations employing distinctly low basal and internal friction coefficients provide a good match to the overall morphology of the serpentinite seamounts, and offer insight into their internal

  11. Microbial Ecology of Subseafloor Communities at Deep-sea Hydrothermal Seamounts of the Pacific Ocean

    NASA Astrophysics Data System (ADS)

    Huber, J. A.; Bolton, S.; Butterfield, D. A.; Baross, J. A.; Sogin, M. L.

    2006-12-01

    Circulation of hydrothermal fluids and seawater occurs within the upper 500 m of porous oceanic crust and provides a rich environment for microbial growth in the subseafloor. Enrichment cultures, geochemical indicators, and sequence analyses of PCR amplicons of ribosomal RNA genes demonstrate that these crustal fluids host a microbial community composed of organisms indigenous to the subseafloor and organisms from other deep-sea habitats, such as seawater. However, the subseafloor microbial communities remain undersampled and our knowledge of what microbes are present and how they are distributed in this dynamic environment over time and space is fragmentary. This work focuses on determining the microbial diversity and genomic content of the subseafloor microbial community at geographically and geochemically distinct deep- sea hydrothermal seamounts. The approach uses a combination of methods, including DNA-based, culturing, and geochemical methods applied to diffuse fluids from two locations: Axial Seamount on the Juan de Fuca Ridge in the northeast Pacific Ocean (45.92° N, 130° W) and seamounts along the Mariana Arc (14-22° N, 143-146° E) in the western Pacific. Both locations host recently eruptive seamounts located above 2000 m with diffusely venting fluids that contain high concentrations of carbon dioxide. However, their geological and chemical setting differs greatly; Axial is a mid-ocean ridge seamount with fluids dominated by high concentrations of hydrogen sulfide, and the Mariana seamounts are at a convergent plate boundary and host a variety of fluids, including those with very low pH and high concentrations of particulate sulfur. Initial studies reveal bacterial communities at both sites consist mainly of epsilon-proteobacteria, a physiologically and phylogenetically diverse group known to have a widespread distribution and dominance in many deep-sea vent habitats. However, while subseafloor archaeal communities at Axial are composed of autotrophic

  12. Quantitative Study of Seismogenic Potential Along Manila Trench: Effects of Scaborough Seamount Chain Subduction

    NASA Astrophysics Data System (ADS)

    Yu, H.; Liu, Y.; Li, D.; Ning, J.; Matsuzawa, T.; Shibazaki, B.; Hsu, Y. J.

    2014-12-01

    Modern seismicity record along the Manila Trench shows only infrequent Mw7 earthquakes, the lack of great earthquakes may indicate the subduction fault is either aseismically slipping or is accumulating strain energy toward rapid release in a megathrust earthquake. We conduct numerical simulations of the plate coupling, earthquake nucleation and dynamic rupture propagation processes along the Manila subduction fault (15-19.5ºN), taking into consideration the effects of plate geometry (including subducted seamounts), fault strength, rate-state frictional properties and pore pressure variations. Specifically, we use the bathymetry to depict the outline of Manila trench along its strike, 2681 background seismicity (1970/02/13 to 2013/09/06) from Chinese Earthquake Network Center and 540 focal mechanism solutions (1976/01/01 to 2013/01/27) from Global CMT project to constrain the geometry of the subducting Sunda/Eurasian slab. The compilation of seismicity and focal mechanism indicates the plate dipping angle gradually changes from 28º (south of the Scaborough Seamount Chain) to 12º (north of it). This geometric anomaly may due to the subducted part of the seamount chain. Preliminary modeling results using gabbro gouge friction data show that the Scaborough Seamount Chain could be a barrier to earthquake rupture propagation. Only earthquakes larger than Mw7 can overcome the barrier to rupture the entire Manila trench. Smaller earthquakes would cease rupturing when it encounters the seamount chain. Moreover, we propose that Manila trench subduction zone has the potential of rupturing in a Mw8 megathrust earthquake, if the simulation period is long enough for an Mw8 earthquake cycle and dynamic rupture overcomes the subducted Scaborough Seamount Chain. Our model parameters will be further constrained by laboratory rock mechanics experiments conducted on IODP Expedition 349, South China Sea (SCS), drilling samples (work in progress at China Earthquake Administration

  13. Diversity of microbial communities in ocean crust below ancient hotspot seamounts along the Louisville Seamount Chain

    NASA Astrophysics Data System (ADS)

    Sylvan, J. B.; Edwards, K. J.

    2012-12-01

    The goal of Integrated Ocean Drilling Expedition 330, Louisville Seamount Trail, was to understand the motion of the Louisville hotspot during 50-80 Ma. As such, >1 km of volcanic basement was collected from five sites on four seamounts, providing an excellent chance to study how microbial populations are effected by different lithologies, different seamounts and age of basement rock along the Louisville Seamount Chain (LSC). Analysis of bacteria growing in enrichment incubations that targeted oligotrophs (with 1% or 10% Marine Broth 2216 diluted with 3% NaCl) and sulfur oxidizers reveals the presence of a diverse array of bacteria, including ɛ-proteobacteria closely related to Sulfurimonas autotrophica, β-proteobacterial methylotrophs, ζ-proteobacteria and Bacteroidetes most closely related to organisms cultured from sediments. Many of these sequences are <97% similar to the closest cultured relatives, indicating the subsurface LSC may be home to unique new species. One isolate recently obtained in pure culture from the original enrichments is 99% similar to Halomonas sulfidaeris str. Esulfude1, a bacterium originally isolated from a hydrothermal sulfide chimney. A second isolate may be a new species of Bacillus. Initial molecular analysis of bacterial communities by pyrosequencing of the 16S rRNA gene as part of the Census of Deep Life (CoDL) supports the data from the culturing work; in one sample collected 174 meters below seafloor, the most abundant bacteria detected include species from the genera Pseudomonas, Sulfurimonas, Methyloversatilis and Desulfocapsa. More CoDL samples will be analyzed in the near future. We will describe results to date on subsurface microbial diversity along the Louisville Seamount Chain from the culturing work and CoDL project and draw comparisons to data derived from younger crustal sites to try to understand how the LSC ecosystem fits into our global picture of life in ocean crust.

  14. SPA Meteor Section Results: 2007

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair

    2013-08-01

    Information extracted from analyses carried out by the SPA Meteor Section from 2007 is presented and discussed. Events covered include: the radio Quadrantid maximum on January 4; a bright fireball seen from parts of England and imaged from the Netherlands at 19h56m UT on February 6, for which an approximate trajectory was established; radio results from the Lyrids in late April; the Perseid near-peak activity from August and a note on some daylight Perseid observing from Britain using thermal imagers; the radio α-Aurigid maximum on September 1; the Orionid return, which again provided enhanced activity over several consecutive dates in October for visual and radio observers; the radio Leonids, although the probably main peak found visually on November 19 was not recorded thus due to its timing; the typically protracted Geminid maximum period around December 13-15 as observed visually and by radio; and the Ursid outburst, primarily as detected by radio on December 22.

  15. Oceanic sharks clean at coastal seamount.

    PubMed

    Oliver, Simon P; Hussey, Nigel E; Turner, John R; Beckett, Alison J

    2011-01-01

    Interactions between pelagic thresher sharks (Alopias pelagicus) and cleaner wrasse were investigated at a seamount in the Philippines. Cleaning associations between sharks and teleosts are poorly understood, but the observable interactions seen at this site may explain why these mainly oceanic sharks regularly venture into shallow coastal waters where they are vulnerable to disturbance from human activity. From 1,230 hours of observations recorded by remote video camera between July 2005 and December 2009, 97 cleaner-thresher shark events were analyzed, 19 of which were interrupted. Observations of pelagic thresher sharks interacting with cleaners at the seamount were recorded at all times of day but their frequency declined gradually from morning until evening. Cleaners showed preferences for foraging on specific areas of a thresher shark's body. For all events combined, cleaners were observed to conduct 2,757 inspections, of which 33.9% took place on the shark's pelvis, 23.3% on the pectoral fins, 22.3% on the caudal fin, 8.6% on the body, 8.3% on the head, 2.1% on the dorsal fin, and 1.5% on the gills respectively. Cleaners did not preferentially inspect thresher sharks by time of day or by shark sex, but there was a direct correlation between the amount of time a thresher shark spent at a cleaning station and the number of inspections it received. Thresher shark clients modified their behavior by "circular-stance-swimming," presumably to facilitate cleaner inspections. The cleaner-thresher shark association reflected some of the known behavioral trends in the cleaner-reef teleost system since cleaners appeared to forage selectively on shark clients. Evidence is mounting that in addition to acting as social refuges and foraging grounds for large visiting marine predators, seamounts may also support pelagic ecology by functioning as cleaning stations for oceanic sharks and rays. PMID:21423796

  16. Oceanic sharks clean at coastal seamount.

    PubMed

    Oliver, Simon P; Hussey, Nigel E; Turner, John R; Beckett, Alison J

    2011-03-14

    Interactions between pelagic thresher sharks (Alopias pelagicus) and cleaner wrasse were investigated at a seamount in the Philippines. Cleaning associations between sharks and teleosts are poorly understood, but the observable interactions seen at this site may explain why these mainly oceanic sharks regularly venture into shallow coastal waters where they are vulnerable to disturbance from human activity. From 1,230 hours of observations recorded by remote video camera between July 2005 and December 2009, 97 cleaner-thresher shark events were analyzed, 19 of which were interrupted. Observations of pelagic thresher sharks interacting with cleaners at the seamount were recorded at all times of day but their frequency declined gradually from morning until evening. Cleaners showed preferences for foraging on specific areas of a thresher shark's body. For all events combined, cleaners were observed to conduct 2,757 inspections, of which 33.9% took place on the shark's pelvis, 23.3% on the pectoral fins, 22.3% on the caudal fin, 8.6% on the body, 8.3% on the head, 2.1% on the dorsal fin, and 1.5% on the gills respectively. Cleaners did not preferentially inspect thresher sharks by time of day or by shark sex, but there was a direct correlation between the amount of time a thresher shark spent at a cleaning station and the number of inspections it received. Thresher shark clients modified their behavior by "circular-stance-swimming," presumably to facilitate cleaner inspections. The cleaner-thresher shark association reflected some of the known behavioral trends in the cleaner-reef teleost system since cleaners appeared to forage selectively on shark clients. Evidence is mounting that in addition to acting as social refuges and foraging grounds for large visiting marine predators, seamounts may also support pelagic ecology by functioning as cleaning stations for oceanic sharks and rays.

  17. Oceanic Sharks Clean at Coastal Seamount

    PubMed Central

    Oliver, Simon P.; Hussey, Nigel E.; Turner, John R.; Beckett, Alison J.

    2011-01-01

    Interactions between pelagic thresher sharks (Alopias pelagicus) and cleaner wrasse were investigated at a seamount in the Philippines. Cleaning associations between sharks and teleosts are poorly understood, but the observable interactions seen at this site may explain why these mainly oceanic sharks regularly venture into shallow coastal waters where they are vulnerable to disturbance from human activity. From 1,230 hours of observations recorded by remote video camera between July 2005 and December 2009, 97 cleaner-thresher shark events were analyzed, 19 of which were interrupted. Observations of pelagic thresher sharks interacting with cleaners at the seamount were recorded at all times of day but their frequency declined gradually from morning until evening. Cleaners showed preferences for foraging on specific areas of a thresher shark's body. For all events combined, cleaners were observed to conduct 2,757 inspections, of which 33.9% took place on the shark's pelvis, 23.3% on the pectoral fins, 22.3% on the caudal fin, 8.6% on the body, 8.3% on the head, 2.1% on the dorsal fin, and 1.5% on the gills respectively. Cleaners did not preferentially inspect thresher sharks by time of day or by shark sex, but there was a direct correlation between the amount of time a thresher shark spent at a cleaning station and the number of inspections it received. Thresher shark clients modified their behavior by “circular-stance-swimming,” presumably to facilitate cleaner inspections. The cleaner-thresher shark association reflected some of the known behavioral trends in the cleaner-reef teleost system since cleaners appeared to forage selectively on shark clients. Evidence is mounting that in addition to acting as social refuges and foraging grounds for large visiting marine predators, seamounts may also support pelagic ecology by functioning as cleaning stations for oceanic sharks and rays. PMID:21423796

  18. Geochemical characteristics of Cocos Plate seamount lavas

    NASA Astrophysics Data System (ADS)

    Allan, James F.; Batiza, Rodey; Sack, Richard O.

    1994-03-01

    A wide compositional continuum of basalts has been erupted from near-ridge seamounts constructed on the Cocos Plate between the Clipperton and Orozco Francture Zones. They range from highly evolved to moderately primitive (3.0 7.8% MgO), LREE-enriched alkali basalts, to moderately evolved to near-primary (5.2 9.5% MgO) tholeiites indistinguishable from N-type MORB. The data set of 159 quench glass analyses exhibits a remarkably consistent variation in both major and trace element composition that is keyed to variations in (La/Sm). Modeling of potential liquid lines of descent at pressures ranging from 1 bar to 8 kbar shows that this covariation is partially due to systematic differences in liquid lines of descent, where the alkaline lavas have undergone substantially more high pressure clinopyroxene fractionation and substantially less low pressure plagioclase fractionation than the tholeiites. In addition, systematic variation in the composition of the more primitive glasses indicates that they were derived from mixing of discrete enriched and depleted melts in the heterogenous seamount mantle source at pressures of 8 10 kbar and greater, and that clinopyroxene may be a residual phase during partial melting. These results show that porous media flow in the seamount mantle source is minor and that melt transport is accomplished primarily through cracking and diking. This study supports suggestions that the general homogeneity of basalt along the EPR is due to mixing in sub-axial magma chambers and mush zones, with additional mixing during partial mantle melting and melt segregation.

  19. Radio Meteors Observations Techniques at RI NAO

    NASA Astrophysics Data System (ADS)

    Vovk, Vasyl; Kaliuzhnyi, Mykola

    2016-07-01

    The Solar system is inhabited with large number of celestial bodies. Some of them are well studied, such as planets and vast majority of big asteroids and comets. There is one group of objects which has received little attention. That is meteoroids with related to them meteors. Nowadays enough low-technology high-efficiency radio-technical solutions are appeared which allow to observe meteors daily. At RI NAO three methodologies for meteor observation are developed: single-station method using FM-receiver, correlation method using FM-receiver and Internet resources, and single-station method using low-cost SDR-receiver.

  20. Diffusion of long-period meteor streams

    NASA Astrophysics Data System (ADS)

    Emel'Ianenko, V. V.

    1992-10-01

    The diffusion of long-period meteor streams is considered on the basis of mappings for the description of planetary perturbations. Formulas for the dispersion of orbital elements under the conditions of limiting stochasticity are obtained. A statistical study of the evolution of meteor streams in the orbits of the Comets Thatcher, P/Swift-Tuttle, P/Halley, and P/Tempel-Tuttle is carried out. It is shown that the dispersion of orbital elements exhibits complex behavior due to the random distribution of meteor particles in the resonant zones.

  1. The 2014 May Camelopardalid Meteor Shower

    NASA Technical Reports Server (NTRS)

    Cooke, Bill; Moser, Danielle

    2014-01-01

    On May 24, 2014 Earth will encounter multiple streams of debris laid down by Comet 209P LINEAR. This will likely produce a new meteor shower, never before seen. Rates predicted to be from 100 to 1000 meteors per hour between 2 and 4 AM EDT, so we are dealing with a meteor outburst, potentially a storm. Peak rate of 200 per hour best current estimate. Difficult to calibrate models due to lack of past observations. Models indicate mm size particles in stream, so potential risk to Earth orbiting spacecraft.

  2. Visual data of minor meteor showers limits of the method

    NASA Technical Reports Server (NTRS)

    Rendtel, Jurgen; Koschack, R.

    1992-01-01

    Visual meteor observations are carried out on a regular basis by many experienced observers worldwide, thus supplying information about activity of meteor showers. The limits of the method are determined by the accuracy of the detection of the meteor trail. This study shows that visual meteor observations provide reliable data for an observable hourly rate of greater than or equal to 3.

  3. The First Confirmed Videorecordings of Lunar Meteor Impacts

    NASA Technical Reports Server (NTRS)

    Dunham, D. W.; Cudnik, B.; Palmer, D. M.; Sada, P. V.; Melosh, J.; Beech, M.; Pellerin, L.; Asher, D.; Frankenberger R.; Venable R.

    2000-01-01

    North American observers recorded at least six meteors striking the Moon's surface during the Leonid meteor shower on 1999 Nov. 18. Each meteor produced a flash that was recorded from at least two separate locations, marking the first confirmed lunar meteor impacts.

  4. Construction of a meteor orbit calculation system for comprehensive meteor observation

    NASA Astrophysics Data System (ADS)

    Mizumoto, S.; Madkour, W.; Yamamoto, M.

    2016-01-01

    At Kochi University of Technology (KUT), the development of an HRO (Ham-band Radio meteor Observation) -Interferometer (IF) was started in 2003, and we realized the meteor orbit calculation system by multiple-site radio observation with GPS time-keeping combining with the 5 channel (5ch) HRO-IF in 2012. Here, we introduce a future plan of comprehensive meteor observation by Radio, Optical and Infrasound observation.

  5. Jasper Seamount: seven million years of volcanism

    USGS Publications Warehouse

    Pringle, M.S.; Staudigel, H.; Gee, J.

    1991-01-01

    Jasper Seamount is a young, mid-sized (690 km3) oceanic intraplate volcano located about 500 km west-southwest of San Diego, California. Reliable 40Ar/39Ar age data were obtained for several milligram-sized samples of 4 to 10 Ma plagioclase by using a defocused laser beam to clean the samples before fusion. Gee and Staudigel suggested that Jasper Seamount consists of a transitional to tholeiitic shield volcano formed by flank transitional series lavas, overlain by flank alkalic series lavas and summit alkalic series lavas. Twenty-nine individual 40Ar/39Ar laser fusion analyses on nine samples confirm the stratigraphy: 10.3-10.0 Ma for the flank transitional series, 8.7-7.5 Ma for the flank alkalic series, and 4.8-4.1 Ma for the summit alkalic series. The alkalinity of the lavas clearly increases with time, and there appear to be 1 to 3 m.y. hiatuses between each series. -from Authors

  6. The KUT meteor radar: An educational low cost meteor observation system by radio forward scattering

    NASA Astrophysics Data System (ADS)

    Madkour, W.; Yamamoto, M.

    2016-01-01

    The Kochi University of Technology (KUT) meteor radar is an educational low cost observation system built at Kochi, Japan by successive graduate students since 2004. The system takes advantage of the continuous VHF- band beacon signal emitted from Fukui National College of Technology (FNCT) for scientific usage all over Japan by receiving the forward scattered signals. The system uses the classical forward scattering setup similar to the setup described by the international meteor organization (IMO), gradually developed from the most basic single antenna setup to the multi-site meteor path determination setup. The primary objective is to automate the observation of the meteor parameters continuously to provide amounts of data sufficient for statistical analysis. The developed software system automates the observation of the astronomical meteor parameters such as meteor direction, velocity and trajectory. Also, automated counting of meteor echoes and their durations are used to observe mesospheric ozone concentration by analyzing the duration distribution of different meteor showers. The meteor parameters observed and the methodology used for each are briefly summarized.

  7. Meteor radar response function: Application to the interpretation of meteor backscatter at medium frequency

    NASA Astrophysics Data System (ADS)

    Cervera, M. A.; Holdsworth, D. A.; Reid, I. M.; Tsutsumi, M.

    2004-11-01

    Recently, Cervera and Elford (2004) extended earlier work on the development of the meteor radar response function (Elford, 1964; Thomas et al., 1988) to include a nonuniform meteor ionization profile. This approach has the advantage that the height distribution of meteors expected to be observed by a radar meteor system is able to be accurately modeled and insights into the meteoroid chemistry to be gained. The meteor radar response function is also an important tool with regard to the interpretation of meteor backscatter in other areas, e.g., modeling the expected diurnal variation of sporadic meteors, investigating the expected echo distribution over the sky, and the calculation of the expected rate curves of meteor showers. We exemplify each of these techniques from the analysis of meteor data collected by the Buckland Park 2 MHz system during October 1997. In addition, we show that the response function may be used to quantify the echo rate of a given shower relative to the sporadic background and thus determine if that shower is able to be detected by the radar.

  8. Seamounts are hotspots of pelagic biodiversity in the open ocean.

    PubMed

    Morato, Telmo; Hoyle, Simon D; Allain, Valerie; Nicol, Simon J

    2010-05-25

    The identification of biodiversity hotspots and their management for conservation have been hypothesized as effective ways to protect many species. There has been a significant effort to identify and map these areas at a global scale, but the coarse resolution of most datasets masks the small-scale patterns associated with coastal habitats or seamounts. Here we used tuna longline observer data to investigate the role of seamounts in aggregating large pelagic biodiversity and to identify which pelagic species are associated with seamounts. Our analysis indicates that seamounts are hotspots of pelagic biodiversity. Higher species richness was detected in association with seamounts than with coastal or oceanic areas. Seamounts were found to have higher species diversity within 30-40 km of the summit, whereas for sets close to coastal habitat the diversity was lower and fairly constant with distance. Higher probability of capture and higher number of fish caught were detected for some shark, billfish, tuna, and other by-catch species. The study supports hypotheses that seamounts may be areas of special interest for management for marine pelagic predators. PMID:20448197

  9. Seamounts are hotspots of pelagic biodiversity in the open ocean.

    PubMed

    Morato, Telmo; Hoyle, Simon D; Allain, Valerie; Nicol, Simon J

    2010-05-25

    The identification of biodiversity hotspots and their management for conservation have been hypothesized as effective ways to protect many species. There has been a significant effort to identify and map these areas at a global scale, but the coarse resolution of most datasets masks the small-scale patterns associated with coastal habitats or seamounts. Here we used tuna longline observer data to investigate the role of seamounts in aggregating large pelagic biodiversity and to identify which pelagic species are associated with seamounts. Our analysis indicates that seamounts are hotspots of pelagic biodiversity. Higher species richness was detected in association with seamounts than with coastal or oceanic areas. Seamounts were found to have higher species diversity within 30-40 km of the summit, whereas for sets close to coastal habitat the diversity was lower and fairly constant with distance. Higher probability of capture and higher number of fish caught were detected for some shark, billfish, tuna, and other by-catch species. The study supports hypotheses that seamounts may be areas of special interest for management for marine pelagic predators.

  10. SAGE III/Meteor - 3M

    NASA Technical Reports Server (NTRS)

    1999-01-01

    Full view of the SAGE III Bench Checkout Unit, Collimated Source Bench (CSB), Portable Image Generator (PIG) on tripod, and Stratospheric Aerosol Gastropheric Experiment (SAGE)/Meteor - 3M flight instrument. Photographed in building 1250, 40 foot clean room.

  11. SAGE III/Meteor - 3M

    NASA Technical Reports Server (NTRS)

    1999-01-01

    Back view of the SAGE III Bench Checkout Unit, Portable Image Generator (PIG) on tripod, and the Stratospheric Aerosol Gastropheric Experiment (SAGE)/Meteor - 3M flight instrument. Photographed in building 1250, 40 foot clean room.

  12. SAGE III/Meteor - 3M

    NASA Technical Reports Server (NTRS)

    1999-01-01

    From left to right: Richard Rawls, Chip Holloway, and Art Hayhurst standing next to the Stratospheric Aerosol Gastropheric Experiment (SAGE)/Meteor - 3M flight instrument. Photographed in building 1250, 40 foot clean room.

  13. Meteor showers associated with 2003EH1

    NASA Astrophysics Data System (ADS)

    Babadzhanov, P. B.; Williams, I. P.; Kokhirova, G. I.

    2008-06-01

    Using the Everhart RADAU19 numerical integration method, the orbital evolution of the near-Earth asteroid 2003EH1 is investigated. This asteroid belongs to the Amor group and is moving on a comet-like orbit. The integrations are performed over one cycle of variation of the perihelion argument ω. Over such a cycle, the orbit intersect that of the Earth at eight different values of ω. The orbital parameters are different at each of these intersections and so a meteoroid stream surrounding such an orbit can produce eight different meteor showers, one at each crossing. The geocentric radiants and velocities of the eight theoretical meteor showers associated with these crossing points are determined. Using published data, observed meteor showers are identified with each of the theoretically predicted showers. The character of the orbit and the existence of observed meteor showers associated with 2003EH1 confirm the supposition that this object is an extinct comet.

  14. Monte Carlo modeling and meteor showers

    NASA Technical Reports Server (NTRS)

    Kulikova, N. V.

    1987-01-01

    Prediction of short lived increases in the cosmic dust influx, the concentration in lower thermosphere of atoms and ions of meteor origin and the determination of the frequency of micrometeor impacts on spacecraft are all of scientific and practical interest and all require adequate models of meteor showers at an early stage of their existence. A Monte Carlo model of meteor matter ejection from a parent body at any point of space was worked out by other researchers. This scheme is described. According to the scheme, the formation of ten well known meteor streams was simulated and the possibility of genetic affinity of each of them with the most probable parent comet was analyzed. Some of the results are presented.

  15. Man-Sized Meteor Over Macon

    NASA Video Gallery

    Astronomers at NASA's Marshall Space Flight Center have recorded the brightest meteor ever seen by their network. On May 20, 2011, six-foot diameter fragment of an unknown comet entered the atmosph...

  16. Large Meteor Tracked over Northeast Alabama

    NASA Video Gallery

    On the evening of May 18, NASA all-sky meteor cameras located at NASA’s Marshall Space Flight Center and at the Walker County Science Center near Chickamauga, Ga. tracked the entry of a large meteo...

  17. Comparison with Russian analyses of meteor impact

    SciTech Connect

    Canavan, G.H.

    1997-06-01

    The inversion model for meteor impacts is used to discuss Russian analyses and compare principal results. For common input parameters, the models produce consistent estimates of impactor parameters. Directions for future research are discussed and prioritized.

  18. Analysis of ALTAIR 1998 Meteor Radar Data

    NASA Technical Reports Server (NTRS)

    Zinn, J.; Close, S.; Colestock, P. L.; MacDonell, A.; Loveland, R.

    2011-01-01

    We describe a new analysis of a set of 32 UHF meteor radar traces recorded with the 422 MHz ALTAIR radar facility in November 1998. Emphasis is on the velocity measurements, and on inferences that can be drawn from them regarding the meteor masses and mass densities. We find that the velocity vs altitude data can be fitted as quadratic functions of the path integrals of the atmospheric densities vs distance, and deceleration rates derived from those fits all show the expected behavior of increasing with decreasing altitude. We also describe a computer model of the coupled processes of collisional heating, radiative cooling, evaporative cooling and ablation, and deceleration - for meteors composed of defined mixtures of mineral constituents. For each of the cases in the data set we ran the model starting with the measured initial velocity and trajectory inclination, and with various trial values of the quantity mPs 2 (the initial mass times the mass density squared), and then compared the computed deceleration vs altitude curves vs the measured ones. In this way we arrived at the best-fit values of the mPs 2 for each of the measured meteor traces. Then further, assuming various trial values of the density Ps, we compared the computed mass vs altitude curves with similar curves for the same set of meteors determined previously from the measured radar cross sections and an electrostatic scattering model. In this way we arrived at estimates of the best-fit mass densities Ps for each of the cases. Keywords meteor ALTAIR radar analysis 1 Introduction This paper describes a new analysis of a set of 422 MHz meteor scatter radar data recorded with the ALTAIR High-Power-Large-Aperture radar facility at Kwajalein Atoll on 18 November 1998. The exceptional accuracy/precision of the ALTAIR tracking data allow us to determine quite accurate meteor trajectories, velocities and deceleration rates. The measurements and velocity/deceleration data analysis are described in Sections

  19. An ecosystem evaluation framework for global seamount conservation and management.

    PubMed

    Taranto, Gerald H; Kvile, Kristina Ø; Pitcher, Tony J; Morato, Telmo

    2012-01-01

    In the last twenty years, several global targets for protection of marine biodiversity have been adopted but have failed. The Convention on Biological Diversity (CBD) aims at preserving 10% of all the marine biomes by 2020. For achieving this goal, ecologically or biologically significant areas (EBSA) have to be identified in all biogeographic regions. However, the methodologies for identifying the best suitable areas are still to be agreed. Here, we propose a framework for applying the CBD criteria to locate potential ecologically or biologically significant seamount areas based on the best information currently available. The framework combines the likelihood of a seamount constituting an EBSA and its level of human impact and can be used at global, regional and local scales. This methodology allows the classification of individual seamounts into four major portfolio conservation categories which can help optimize management efforts toward the protection of the most suitable areas. The framework was tested against 1000 dummy seamounts and satisfactorily assigned seamounts to proper EBSA and threats categories. Additionally, the framework was applied to eight case study seamounts that were included in three out of four portfolio categories: areas highly likely to be identified as EBSA with high degree of threat; areas highly likely to be EBSA with low degree of threat; and areas with a low likelihood of being EBSA with high degree of threat. This framework will allow managers to identify seamount EBSAs and to prioritize their policies in terms of protecting undisturbed areas, disturbed areas for recovery of habitats and species, or both based on their management objectives. It also identifies seamount EBSAs and threats considering different ecological groups in both pelagic and benthic communities. Therefore, this framework may represent an important tool to mitigate seamount biodiversity loss and to achieve the 2020 CBD goals. PMID:22905190

  20. An ecosystem evaluation framework for global seamount conservation and management.

    PubMed

    Taranto, Gerald H; Kvile, Kristina Ø; Pitcher, Tony J; Morato, Telmo

    2012-01-01

    In the last twenty years, several global targets for protection of marine biodiversity have been adopted but have failed. The Convention on Biological Diversity (CBD) aims at preserving 10% of all the marine biomes by 2020. For achieving this goal, ecologically or biologically significant areas (EBSA) have to be identified in all biogeographic regions. However, the methodologies for identifying the best suitable areas are still to be agreed. Here, we propose a framework for applying the CBD criteria to locate potential ecologically or biologically significant seamount areas based on the best information currently available. The framework combines the likelihood of a seamount constituting an EBSA and its level of human impact and can be used at global, regional and local scales. This methodology allows the classification of individual seamounts into four major portfolio conservation categories which can help optimize management efforts toward the protection of the most suitable areas. The framework was tested against 1000 dummy seamounts and satisfactorily assigned seamounts to proper EBSA and threats categories. Additionally, the framework was applied to eight case study seamounts that were included in three out of four portfolio categories: areas highly likely to be identified as EBSA with high degree of threat; areas highly likely to be EBSA with low degree of threat; and areas with a low likelihood of being EBSA with high degree of threat. This framework will allow managers to identify seamount EBSAs and to prioritize their policies in terms of protecting undisturbed areas, disturbed areas for recovery of habitats and species, or both based on their management objectives. It also identifies seamount EBSAs and threats considering different ecological groups in both pelagic and benthic communities. Therefore, this framework may represent an important tool to mitigate seamount biodiversity loss and to achieve the 2020 CBD goals.

  1. An Ecosystem Evaluation Framework for Global Seamount Conservation and Management

    PubMed Central

    Taranto, Gerald H.; Kvile, Kristina Ø.; Pitcher, Tony J.; Morato, Telmo

    2012-01-01

    In the last twenty years, several global targets for protection of marine biodiversity have been adopted but have failed. The Convention on Biological Diversity (CBD) aims at preserving 10% of all the marine biomes by 2020. For achieving this goal, ecologically or biologically significant areas (EBSA) have to be identified in all biogeographic regions. However, the methodologies for identifying the best suitable areas are still to be agreed. Here, we propose a framework for applying the CBD criteria to locate potential ecologically or biologically significant seamount areas based on the best information currently available. The framework combines the likelihood of a seamount constituting an EBSA and its level of human impact and can be used at global, regional and local scales. This methodology allows the classification of individual seamounts into four major portfolio conservation categories which can help optimize management efforts toward the protection of the most suitable areas. The framework was tested against 1000 dummy seamounts and satisfactorily assigned seamounts to proper EBSA and threats categories. Additionally, the framework was applied to eight case study seamounts that were included in three out of four portfolio categories: areas highly likely to be identified as EBSA with high degree of threat; areas highly likely to be EBSA with low degree of threat; and areas with a low likelihood of being EBSA with high degree of threat. This framework will allow managers to identify seamount EBSAs and to prioritize their policies in terms of protecting undisturbed areas, disturbed areas for recovery of habitats and species, or both based on their management objectives. It also identifies seamount EBSAs and threats considering different ecological groups in both pelagic and benthic communities. Therefore, this framework may represent an important tool to mitigate seamount biodiversity loss and to achieve the 2020 CBD goals. PMID:22905190

  2. Nonhydrostatic tidal dynamics in the area of a seamount

    NASA Astrophysics Data System (ADS)

    Voltzinger, N. E.; Androsov, A. A.

    2016-07-01

    The nonhydrostatic boundary problem for an arbitrary three-dimensional domain with a seamount is considered. The problem is integrated into curvilinear boundary-fitted coordinates on a nonuniform grid. In order to identify nonhydrostatic effects the grid is condensed on the slopes of the seamount preserving a coarse resolution in the rest of the domain, where the problem is solved in the hydrostatic approximation. Calculation results for the nonhydrostatic tidal dynamics and hydrology of the Strait of Messina in the area of a seamount are presented.

  3. SEC Vidicon spectra of Geminid meteors, 1972

    NASA Technical Reports Server (NTRS)

    Millman, P. M.; Clifton, K. S.

    1975-01-01

    The SEC Vidicon, a low light level closed circuit television system, was used to obtain 137 spectrographic records of meteors at Mt. Hopkins, Arizona, during the Geminid meteor shower in December 1972. Seven of the best Geminid meteor spectra are studied here in detail. The near infrared, out to wavelengths near 9000 A, is recorded for the first time for Geminids. The spectra, in general, exhibit the elements previously found in photographic records of this shower but show a surprising frequency of occurrence of the forbidden green line of O I at 5577 A. This line is normally absent from meteors moving as slowly as the Geminids (36 km/sec) and its presence in these records may be due to the added sensitivity available with the SEC Vidicon. The average green line duration in Geminid meteors with a luminosity near zero absolute visual magnitude is 0.73 sec at a mean height of 95 km, 11 km lower than the green line peak in Perseid meteors of the same luminosity.

  4. Meteoric Ions in Planetary Ionospheres

    NASA Technical Reports Server (NTRS)

    Pesnell, W. D.; Grebowsky, Joseph M.; Vondrak, Richard R. (Technical Monitor)

    2001-01-01

    Solar system debris, in the form of meteoroids, impacts every planet. The flux, relative composition and speed of the debris at each planet depends on the planet's size and location in the solar system. Ablation in the atmosphere evaporates the meteoric material and leaves behind metal atoms. During the ablation process metallic ions are formed by impact ionization. For small inner solar system planets, including Earth, this source of ionization is typically small compared to either photoionization or charge exchange with ambient molecular ions. For Earth, the atmosphere above the main deposition region absorbs the spectral lines capable of ionizing the major metallic atoms (Fe and Mg) so that charge exchange with ambient ions is the dominant source. Within the carbon dioxide atmosphere of Mars (and possibly Venus), photoionization is important in determining the ion density. For a heavy planet like Jupiter, far from the sun, impact ionization of ablated neutral atoms by impacts with molecules becomes a prominent source of ionization due to the gravitational acceleration to high incident speeds. We will describe the processes and location and extent of metal ion layers for Mars, Earth and Jupiter, concentrating on flagging the uncertainties in the models at the present time. This is an important problem, because low altitude ionosphere layers for the planets, particularly at night, probably consist predominantly of metallic ions. Comparisons with Earth will be used to illustrate the differing processes in the three planetary atmospheres.

  5. January and February Meteor Showers Detected by CAMS: the Cameras for Allsky Meteor Surveillance

    NASA Astrophysics Data System (ADS)

    Johnson, Beth; Jenniskens, P. M.

    2014-01-01

    Many meteor showers are in need of validation. Of 493 meteor showers listed in the IAU Working List of Mete-or Showers, only 95 are established. Of the rest, it is uncertain whether they exist or not. The goal of the Cameras for Allsky Meteor Surveillance (CAMS) project in California is to validate or remove the remaining 325 showers. CAMS scales up the use of low-light-level video for meteor triangulation, by deploying 60 video cameras spread over three sites. Once the video data has been analyzed, showers can be confirmed by comparing arrival time, direc-tion of the radiant, and speed of the individual meteors. Once established, showers can be linked to their parent bod-ies and meteoroid streams. The CAMS stations are located in Sunnyvale, at Fremont Peak Observatory, and at Lick Observatory, to the south and east of Sunnyvale, respectively. Each station contains 20 low-light-level security cameras arrayed to view the entire sky above 30°. During the night, the video data from the cameras is written to disk and analysed in day-time with the MeteorScan software package to find moving objects. Eight-second video sequences are saved for all detections. The video sequences are combined at the SETI Institute, where astrometric calibration files are generated and meteors detected from at least two stations simultaneously are found interactively using the Coincidence program. Coincidence also calculates the radiant and velocity of each meteor. Here, we discuss results obtained in January and February 2013. Over 7,500 meteor orbits were cataloged in this period. This outcome doubled the detection rate from the previous two years of CAMS data.We will present graphs of the detected meteor showers and discuss their parent body sources.

  6. Mesospheric temperature estimation from meteor decay times during Geminids meteor shower

    NASA Astrophysics Data System (ADS)

    Kozlovsky, Alexander; Lukianova, Renata; Shalimov, Sergey; Lester, Mark

    2016-02-01

    Meteor radar observations at the Sodankylä Geophysical Observatory (67° 22'N, 26° 38'E, Finland) indicate that the mesospheric temperature derived from meteor decay times is systematically underestimated by 20-50 K during the Geminids meteor shower which has peak on 13 December. A very good coincidence of the minimum of routinely calculated temperature and maximum of meteor flux (the number of meteors detected per day) was observed regularly on that day in December 2008-2014. These observations are for a specific height-lifetime distribution of the Geminids meteor trails and indicate a larger percentage of overdense trails compared to that for sporadic meteors. A consequence of this is that the routine estimates of mesospheric temperature during the Geminids are in fact underestimates. The observations do, however, indicate unusual properties (e.g., mass, speed, or chemical composition) of the Geminids meteoroids. Similar properties were found also for Quadrantids in January 2009-2015, which like the Geminids has as a parent body an asteroid, but not for other meteor showers.

  7. Lagrangian observations of surface circulation at the Emperor Seamount chain

    NASA Technical Reports Server (NTRS)

    Vastano, A. C.; Hagan, D. E.; Mcnally, G. J.

    1985-01-01

    In a Kuroshio tracking experiment initiated in February 1977, two satellite-reporting buoys, drogued to 100-m depth, were released southeast of Kuyshu Island, Japan. These drifters crossed the Shatskiy Rise in the Kuroshio extension during May and October and then traversed the Emperor Seamount Chain. Although they reached the chain 117 days apart, their movements near the seamounts display remarkably similar patterns, demonstrating upstream meanders in the surface flow; cyclonic eddy activity immediately west of the chain; passage through the same gap associated with the Jingu and Nintoku seamounts; and a wavelike pattern present over the Hess Rise east of the chain. One drifter exhibited cyclonic eddy motion east of the chain in the lee of the Kinmei Seamount.

  8. Search for seamounts in the southern Cook and Austral region

    SciTech Connect

    Lambeck, K.; Coleman, R.

    1982-04-01

    The existence of uncharted seamounts in the Cook-Austral region of the South Pacific has been investigated using GEOS 3 and SEASAT radar altimeter observations. Three previously uncharted submarine seamounts, provisionally named GEOS A to GEOS C, have been located between Mauke and Rimatara and a fourth, GEOS D, has been located east of Rurutu. This confirms that the Aitutaki-Mauke islands of the Southern Cooks are a continuation of the Austral chain. A second group of uncharted seamounts has been provisionally located some 200 km south of Rimatara and Maria and this is suggestive of a second seamount chain, south of the first, that includes Raratonga and Mangaia. Fabert Bank, to the south of Mangaia, appears to be mislocated by about 2/sup 0/ in longitude.

  9. Seismic detections of the 15 February 2013 Chelyabinsk meteor from the dense ChinArray

    NASA Astrophysics Data System (ADS)

    Li, Lu; Wang, Baoshan; Peng, Zhigang; Wang, Weitao

    2016-07-01

    ChinArray is a dense portable broadband seismic network to cover the entire continental China, and the Phase I is deployed along the north-south seismic belt in southwest China. In this study, we analyze seismic data recorded on the ChinArray following the February 15, 2013 Chelyabinsk (Russia) meteor. This was the largest known object entering the Earth's atmosphere since the 1908 Tunguska meteor. The seismic energy radiated from this event was recorded by seismic stations worldwide including the dense ChinArray that are more than 4000 km away. The weak signal from the meteor event was contaminated by a magnitude 5.8 Tonga earthquake occurred ~20 min earlier. To test the feasibility of detecting the weak seismic signals from the meteor event, we compute vespagram and perform F-K analysis to the surface-wave data. We identify a seismic phase with back azimuth (BAZ) of 329.7° and slowness of 34.73 s/deg, corresponding to the surface wave from the Russian meteor event (BAZ ~325.97°). The surface magnitude (M S) of the meteor event is 3.94 ± 0.18. We also perform similar analysis on the data from the broadband array F-net in Japan, and find the BAZ of the surface waves to be 316.61°. With the different BAZs of ChinArray and F-net, we locate the Russian meteor event at 58.80°N, 58.72°E. The relatively large mislocation (~438 km as compared with 55.15°N, 61.41°E by others) may be a result of the bending propagation path of surface waves, which deviates from the great circle path. Our results suggest that the dense ChinArray and its subarrays could be used to detect weak signals at teleseismic distances.

  10. Seismic detections of the 15 February 2013 Chelyabinsk meteor from the dense ChinArray

    NASA Astrophysics Data System (ADS)

    Li, Lu; Wang, Baoshan; Peng, Zhigang; Wang, Weitao

    2016-08-01

    ChinArray is a dense portable broadband seismic network to cover the entire continental China, and the Phase I is deployed along the north-south seismic belt in southwest China. In this study, we analyze seismic data recorded on the ChinArray following the February 15, 2013 Chelyabinsk (Russia) meteor. This was the largest known object entering the Earth's atmosphere since the 1908 Tunguska meteor. The seismic energy radiated from this event was recorded by seismic stations worldwide including the dense ChinArray that are more than 4000 km away. The weak signal from the meteor event was contaminated by a magnitude 5.8 Tonga earthquake occurred ~20 min earlier. To test the feasibility of detecting the weak seismic signals from the meteor event, we compute vespagram and perform F-K analysis to the surface-wave data. We identify a seismic phase with back azimuth (BAZ) of 329.7° and slowness of 34.73 s/deg, corresponding to the surface wave from the Russian meteor event (BAZ ~325.97°). The surface magnitude ( M S) of the meteor event is 3.94 ± 0.18. We also perform similar analysis on the data from the broadband array F-net in Japan, and find the BAZ of the surface waves to be 316.61°. With the different BAZs of ChinArray and F-net, we locate the Russian meteor event at 58.80°N, 58.72°E. The relatively large mislocation (~438 km as compared with 55.15°N, 61.41°E by others) may be a result of the bending propagation path of surface waves, which deviates from the great circle path. Our results suggest that the dense ChinArray and its subarrays could be used to detect weak signals at teleseismic distances.

  11. A characterization of the megafauna on Davidson Seamount

    NASA Astrophysics Data System (ADS)

    Lundsten, L.; Devogelaere, A. P.; Barry, J. P.; Clague, D. A.

    2006-12-01

    Seamounts offer hard substrate, complex habitat, elevated current velocities, and other features that allow for the existence of unique assemblages of organisms, often dominated by long-lived and fragile corals and sponges. Seamount faunas have high rates of endemism with biogeographic patterns analogous to land-based island faunas. Seamount organisms, particularly long-lived deep-sea corals, are particularly vulnerable to bottom trawling and other resource extraction techniques. Davidson Seamount, located 120 km southwest of Monterey, CA, USA, is an example of a relatively undisturbed and pristine seamount habitat. Volcanic in origin, Davidson Seamount was formed 12-16 million years ago atop a fossil spreading center, which produced a unique pattern of northeast trending ridges on the seamount. Remotely Operated Vehicle (ROV) dives at Davidson Seamount were conducted in 2000 and 2006 by a collaboration of scientists, resource managers and educators. Sixteen dives were annotated in detail using MBARI's Video Annotation Reference System (VARS), yielding more than 60,000 biological observations. Over 170 organisms were identified to the lowest possible taxon. The distribution of organisms in relation to the bathymetric complexity of the seamount were analyzed using ArcGIS 9.1 and NOAA's Benthic Terrain Modeler (BTM) to relate faunal distributions to slope, aspect, and bathymetric position. Video transects completed in 2006 were analyzed to quantify species' density and richness. Several new species were observed and collected, and are currently being described by taxonomists. Results of this study indicate that corals and sponges may have species-specific depth distributions with little overlap of large habitat forming phyla. Moreover, substratum type, slope, and aspect are important in determining the distribution of some coral species. This baseline survey is valuable in describing the fauna of Davidson Seamount, has been used in developing essential fish habitat

  12. Topographically induced circulation patterns and mixing over Condor seamount

    NASA Astrophysics Data System (ADS)

    Bashmachnikov, I.; Loureiro, C. M.; Martins, A.

    2013-12-01

    Analysis of mean and oscillatory circulation patterns over Condor seamount, situated near the central group of the Azores islands, was performed. During 1.5 years of observations, at least half of the time an anticyclonic cap was established over the summit. The vortex was characterised by a strong asymmetry: it was shifted to the south of the summit and strongly stretched along the gentle eastern and western slopes of the seamount.

  13. New Application of Finite Element Method to Seamount Magnetism

    NASA Astrophysics Data System (ADS)

    HA, G.; Kim, S. S.; So, B. D.

    2015-12-01

    Geomagnetic method can be utilized in a wide range of applications, including investigation of small-scale near-surface targets and characterization of large-scale geologic structures. In particular, marine magnetic studies involve with various interpretation approaches to constrain geophysical information regarding the depth of a particular seamount, its size and shape, and the orientation and magnitude of its magnetization. The accuracy of the estimated information is normally governed by the quality and amount of available data and by the sophistication of the employed modeling techniques. Here we aim to advance geomagnetic modeling approaches using the interactive finite element solver, COMSOL Multiphysics, and improve the degree of detail that can be obtained from the measured magnetic field. First, we carried out benchmark tests by comparing the computed results using the analytic solutions for simple bodies. We built two types of synthetic models with rectangular and sphere shaped ore bodies having high intensity of magnetization and we changed magnetized direction in each calculation. Comparisons of FEM-based results with the analytic ones exhibited good agreement in general. Second, marine magnetic data obtained at seamounts can be very crucial to determine the age and location of seamount formation. Traditional magnetic methods often assume the uniformly magnetized seamounts to simplify computational efforts. However, the inner structures of seamounts constrained by seismic data show a clear distinction between the dense core and edifice layers. Here we divide the seamount into the dense core and edifice layers in a synthetic model, assign different magnetization direction and intensity to them, and optimize these parameters by minimizing differences between the observed and numerical computed data. These examined results will be valuable to understand seamount formation processes in detail. In addition, we discuss FEM-based magnetic models to mimic the

  14. Microbial community on oceanic ferro-manganese crusts from Takuyo-Daigo Seamount and Ryusei Seamount

    NASA Astrophysics Data System (ADS)

    Nitahara, S.; Kato, S.; Yamagishi, A.

    2012-12-01

    Background and Purpose Iron and manganese oxide deposits are often found on deep seafloor. Rocks covered with these oxides are called ferro-manganese crusts (Mn crusts), and are ubiquitously distributed on deep seafloor (Rona 2003). Because Mn crusts contain rare metals such as Co, Pt and rare earth element, it can be resources in the future. Mn crusts and microbes on Mn crusts may contribute to material, especially carbon and nitrogen circulation between hydrosphere and lithosphere. Mechanism of Mn crust formation is not completely understood. Wang et al. propose a model that microorganisms associate with initial Mn mineral deposition (Wang et al., 2011). There is a possibility that microbes may contribute to formation of Mn crust relying on their ability to oxidize Fe and Mn. However, there is limited information about diversity, spatial distribution and abundance of microbes on Mn crust surface. Our purpose is to clarify microbial community composition, spatial distribution, diversity and abundance of microbes on Mn crusts collected from Takuyo-Daigo seamount and Ryusei seamount. Method We collected Mn crusts, sediments and ambient seawater from Takuyo-Daigo seamount at the depth of 1200 m, 1419 m, 2209 m and 2991 m during NT09-02 cruise in Feb 2009 and Ryusei seamount at the depth of 1194 m, 2079 m during KY11-02 in Feb 2011 with remotely operated vehicle Hyper-Dolphin (JAMSTEC). Genomic DNA was extracted from each sample using Fast DNA kit for soil (Qbiogene). Partial 16S rRNA gene and amoA gene were amplified by PCR with prokaryote-universal primer set (Uni516F-Uni1407R) and bacterial and archaeal amoA specific primer sets. PCR products were cloned. The nucleotide sequences of randomly selected clones were determined. We performed phylogenetic and statistical analysis to determine microbial community compositions, and estimated diversity indices. We also estimated the copy numbers of 16S rRNA and amoA genes of Bacteria and Archaea by quantitative PCR. Results

  15. Trophodynamic studies on the Condor seamount (Azores, Portugal, North Atlantic)

    NASA Astrophysics Data System (ADS)

    Colaço, A.; Giacomello, E.; Porteiro, F.; Menezes, G. M.

    2013-12-01

    Compared to the surrounding ocean waters, seamounts are commonly considered habitats where biological productivity is higher and consumers proliferate. Despite their high productivity, studies of seamount trophic webs are still scarce and fragmentary, and little is known about the connections between the different compartments. What are the trophic interactions of seamount fauna? How do the pelagic and benthic environment couple? In order to answer these questions, stable isotopes δ15N and δ13C were measured in the organisms collected during the course of numerous campaigns at the Condor seamount in the North Atlantic. The Condor seamount food chain is composed of five trophic levels. Mesopelagic organisms are the link between the epipelagic environment and the benthic and benthopelagic organisms, bridging the gap between primary consumers and the 4th and 5th trophic chain levels. Our results demonstrate, through stable isotope analysis, the important role of mesopelagic organisms in the transfer of energy within the seamount food web, as modeling/theoretical studies have previously suggested.

  16. Asteroid 1620 Geographos: II. Associated Meteor Streams

    NASA Astrophysics Data System (ADS)

    Ryabova, G. O.

    2002-05-01

    This study attempts to answer the following questions. Are there meteor streams genetically related to asteroid 1620 Geographos? When and how were they generated? Can we find any of them in the catalogs of orbits of meteors that have been observed? Numerous model streams, varying in particle-ejection scheme and in the moment of generation, have been considered. It has been found that the meteor streams observed from the Earth were most likely produced as a result of a collision with a small body. However, the generation of the meteor stream under the combined effect of rotation and tidal forces during the asteroid's close approach to the Earth cannot also be ruled out. Meteoroid streams formed at high ejection velocities (up to 1 km/s) can approach the Earth's orbit twice per orbital period: once before perihelion (in February-March) and once after perihelion (in August). The 44 orbits close to the model ones were found in the catalogs of meteoroid orbits. A taxonomic structure has been built for them. The distribution of ejection velocities for the models of Earth-approaching meteoroids points to the impact of an overtaking body, but the moment of collision remains unknown. Thus, it is quite possible that asteroid Geographos is the parent body for twin meteor showers observed at the Earth: Spring and Autumn Geographids.

  17. CAMS confirmation of previously reported meteor showers

    NASA Astrophysics Data System (ADS)

    Jenniskens, P.; Nénon, Q.; Gural, P. S.; Albers, J.; Haberman, B.; Johnson, B.; Holman, D.; Morales, R.; Grigsby, B. J.; Samuels, D.; Johannink, C.

    2016-03-01

    Leading up to the 2015 IAU General Assembly, the International Astronomical Union's Working List of Meteor Showers included 486 unconfirmed showers, showers that are not certain to exist. If confirmed, each shower would provide a record of past comet or asteroid activity. Now, we report that 41 of these are detected in the Cameras for Allsky Meteor Surveillance (CAMS) video-based meteor shower survey. They manifest as meteoroids arriving at Earth from a similar direction and orbit, after removing the daily radiant drift due to Earth's motion around the Sun. These showers do exist and, therefore, can be moved to the IAU List of Established Meteor Showers. This adds to 31 previously confirmed showers from CAMS data. For each shower, finding charts are presented based on 230,000 meteors observed up to March of 2015, calculated by re-projecting the drift-corrected Sun-centered ecliptic coordinates into more familiar equatorial coordinates. Showers that are not detected, but should have, and duplicate showers that project to the same Sun-centered ecliptic coordinates, are recommended for removal from the Working List.

  18. BRAMS: The Belgian RAdio Meteor Stations

    NASA Technical Reports Server (NTRS)

    Lamy, H.; Ranvier, S.; De Keyser, J.; Calders, S.; Gamby, E.; Verbeeck, C.

    2011-01-01

    In the last months, the Belgian Institute for Space Aeronomy has been developing a Belgian network for observing radio meteors using forward scattering technique. This network is called BRAMS for Belgian RAdio Meteor Stations. Two beacons emitting a circularly polarized pure sine wave toward the zenith act as the transmitters at frequencies of 49.97 and 49.99 MHz. The first one located in Dourbes (Southern Belgium) emits a constant power of 150 Watts while the one located in Ieper (Western Belgium) emits a constant power of 50 Watts. The receiving network consists of about 20 stations hosted mainly by radio amateurs. Two stations have crossed-Yagi antennas measuring horizontal and vertical polarizations of the waves reflected off meteor trails. This will enable a detailed analysis of the meteor power profiles from which physical parameters of the meteoroids can be obtained. An interferometer consisting of 5 Yagi-antennas will be installed at the site of Humain in order to determine the angular detection of one reflection point, allowing us to determine meteoroid trajectories. We describe this new meteor observing facility and present the goals we expect to achieve with the network.

  19. Optical Meteor Systems Used by the NASA Meteoroid Environment Office

    NASA Technical Reports Server (NTRS)

    Kingery, A. M.; Blaauw, R. C.; Cooke, W. J.; Moser, D. E.

    2015-01-01

    The NASA Meteoroid Environment Office (MEO) uses two main meteor camera networks to characterize the meteoroid environment: an all sky system and a wide field system to study cm and mm size meteors respectively. The NASA All Sky Fireball Network consists of fifteen meteor video cameras in the United States, with plans to expand to eighteen cameras by the end of 2015. The camera design and All-Sky Guided and Real-time Detection (ASGARD) meteor detection software [1, 2] were adopted from the University of Western Ontario's Southern Ontario Meteor Network (SOMN). After seven years of operation, the network has detected over 12,000 multi-station meteors, including meteors from at least 53 different meteor showers. The network is used for speed distribution determination, characterization of meteor showers and sporadic sources, and for informing the public on bright meteor events. The NASA Wide Field Meteor Network was established in December of 2012 with two cameras and expanded to eight cameras in December of 2014. The two camera configuration saw 5470 meteors over two years of operation with two cameras, and has detected 3423 meteors in the first five months of operation (Dec 12, 2014 - May 12, 2015) with eight cameras. We expect to see over 10,000 meteors per year with the expanded system. The cameras have a 20 degree field of view and an approximate limiting meteor magnitude of +5. The network's primary goal is determining the nightly shower and sporadic meteor fluxes. Both camera networks function almost fully autonomously with little human interaction required for upkeep and analysis. The cameras send their data to a central server for storage and automatic analysis. Every morning the servers automatically generates an e-mail and web page containing an analysis of the previous night's events. The current status of the networks will be described, alongside with preliminary results. In addition, future projects, CCD photometry and broadband meteor color camera

  20. Great Minds? Great Lakes!

    ERIC Educational Resources Information Center

    Environmental Protection Agency, Chicago, IL. Great Lakes National Program Office.

    This book contains lesson plans that provide an integrated approach to incorporating Great Lakes environmental issues into elementary subjects. The book is divided into three subject areas: (1) History, which includes the origins of the Great Lakes, Great Lakes people, and shipwrecks; (2) Social Studies, which covers government, acid rain as a…

  1. Atmospheric trajectories and light curves of shower meteors

    NASA Astrophysics Data System (ADS)

    Koten, P.; Borovička, J.; Spurný, P.; Betlem, H.; Evans, S.

    2004-12-01

    Double station data on 496 meteors belonging to several meteor showers were obtained within the program of the video meteor observations during years 1998-2001. Analyzed meteors cover a range of photometric masses from 10-7 to 10-4 kg with a corresponding range of maximum brightness from +4.7 to -2.1 absolute magnitude. Atmospheric trajectories of Perseid, Orionid and Leonid meteors are analysed. These typical cometary high velocity meteors are compared to Geminid meteors with probable asteroidal origin and Taurid meteors - another cometary shower with significantly lower entry velocity. The light curves of the studied meteors vary widely, but generally are nearly symmetrical with the point of maximum brightness located close the to middle of the luminous trajectory. Small differences between showers are reported. We found that the height data are in good agreement with the dust-ball model predictions. The only difference is the beginning height behaviour. The beginning heights of cometary meteors increase with increasing photometric mass. These meteoroids probably contain a volatile part which starts to ablate before we are able to detect the meteors. The Geminid meteors are a different case. They start to ablate suddenly and their beginning height is almost constant in the whole range of studied meteoroid masses. In this case we observe real beginnings of meteor ablation.

  2. Models for Near-Ridge Seamounts Constrained by Gravity Observations

    NASA Astrophysics Data System (ADS)

    Kostlan, M.; McClain, J. S.

    2009-12-01

    In an analysis of the seamount chain centered at 105°20’W, 9°05’N, west of the East Pacific Rise and south of the Clipperton transform fault, we compared measured free air gravity anomaly values with modeled gravity anomaly values. The seamount chain contains approximately ten seamounts trending roughly east-west, perpendicular to the mid-ocean ridge axis. They lie on lithosphere between 1.5 and 2.7 Ma in age. Based on its position and age, the seamount chain appears to be associated with the 9°03’N overlapping spreading center (OSC). This OSC includes several associated seamount chains, aligned generally east-west, and of varying ages. The observed data include both free air gravity anomalies and bathymetry of the seamount chain, provided by the National Geophysical Data Center (NGDC), and was selected because the gravity measurements are relatively well covered. We used a series of different structural models of the oceanic crust and mantle to generate gravity anomalies associated with the sea mounts. The models utilize Parker’s algorithm to generate these free air gravity anomalies. We compute a gravity residual by subtracting the calculated anomalies from the observed anomalies. The models include one with a crust of a constant thickness (6 km), while another introduces a constant-thickness Layer 2A. In contrast, a third model included a variable thickness crust, where the thickness is governed by Airy compensation. The calculations show that the seamounts must be partly compensated, because the constant-thickness models predict a high negative residual (or they produce an anomaly which is too high). In contrast, the Airy compensation model produces an anomaly that is too low at the longer wavelengths, indicating that the lithosphere must have some strength, and that flexure must be supporting part of the load of the seamount chain. This contrasts with earlier studies that indicate young, near-ridge seamounts do not result in flexure of the thin

  3. ROAN Remote radio meteor detection sensor

    NASA Astrophysics Data System (ADS)

    Lesanu, C. E.

    2016-01-01

    Only few meteor enthusiasts across the world today, approaches systematically the radio meteor detection technique, one of the reasons being the difficulty to build and install proper permanent antennas, especially when low-VHF frequency opportunity transmitters are used as illuminators. Other reasons were in the past the relatively high cost of the entire system, receivers and computers, and not ultimately the high power consumption of the system in a 24/7 operation, when using regular personal computers. The situation changed in the recent years with the advent of the low cost software defined radio SDR receivers and low consumption/cost single board computers SBC. A commercial off-the-shelf hardware based remote radio meteor detection sensor is presented.

  4. Observation of meteors by MST radar

    NASA Technical Reports Server (NTRS)

    Jones, William; Kingsley, S. P.

    1992-01-01

    The observation of meteor trails by a vertical mesosphere - stratosphere - troposphere (MST) radar beam has the advantage of good height resolution and an approximate knowledge of the zenith angle since the trails are horizontal or near-horizontal. An extension of the ablation theory of meteors was developed for near horizontal trails which takes into account the curvature of the earth. Observations of the Geminid meteor shower by MST radar reveal the 'diffusion heights' to be in fair agreement with the true height, but with some discrepancies that can amount to 4 km. The true heights are almost entirely confined to the range 87-91 km, although the upper limit is attributed to the coherent integration time of the existing MST radar processing.

  5. Various meteor scenes I: the perception and the conception of a 'meteor shower'

    NASA Astrophysics Data System (ADS)

    Koseki, Masahiro

    2014-10-01

    Not all 'established showers' are recognisable by every method. Some might be lost ('dead') or have recurrent (periodic) nature and are not observable annually. Some are dominated by faint meteors and not observable visually but by radar systems. Other showers are rich in fireballs and their low meteor rates make them a good target for video and photographic observations, while visual observers may not notice their activity because of the low rates. The perception limit in magnitude differs between the observing methods on the one hand, but depends on the magnitude ratios of shower meteors on the other hand. Differences in the definition of a 'meteor shower'/'meteoroid stream' work important roles composing the shower list and we need to know how much various researchers' definitions differ. Depending whether we use observational raw data of the visible meteor shower or orbital elements of the meteoroid stream this may lead to either an obvious meteor showers or an undetectable stream. This paper (paper I) describes the reasons why we can see a meteor shower and why not, Paper II proves the condition by the example of Cygnid-Draconid complex, especially for the κ-Cygnids, and Paper III looks at the different views of several minor showers from the different kind observations.

  6. All-sky Meteor Orbit System AMOS and preliminary analysis of three unusual meteor showers

    NASA Astrophysics Data System (ADS)

    Tóth, Juraj; Kornoš, Leonard; Zigo, Pavol; Gajdoš, Štefan; Kalmančok, Dušan; Világi, Jozef; Šimon, Jaroslav; Vereš, Peter; Šilha, Jiří; Buček, Marek; Galád, Adrián; Rusňák, Patrik; Hrábek, Peter; Ďuriš, František; Rudawska, Regina

    2015-12-01

    All-sky Meteor Orbit System (AMOS) is a semi-autonomous video observatory for detection of transient events on the sky, mostly the meteors. Its hardware and software development and permanent placement on several locations in Slovakia allowed the establishment of Slovak Video Meteor Network (SVMN) monitoring meteor activity above the Central Europe. The data reduction, orbital determination and additional results from AMOS cameras - the SVMN database - as well as from observational expeditions on Canary Islands and in Canada provided dynamical and physical data for better understanding of mutual connections between parent bodies of asteroids and comets and their meteoroid streams. We present preliminary results on exceptional and rare meteor streams such as September ɛ Perseids (SPE) originated from unknown long periodic comet on a retrograde orbit, suspected asteroidal meteor stream of April α Comae Berenicids (ACO) in the orbit of meteorites Příbram and Neuschwanstein and newly observed meteor stream Camelopardalids (CAM) originated from Jupiter family comet 209P/Linear.

  7. Analysis of historical meteor and meteor shower records: Korea, China, and Japan

    NASA Astrophysics Data System (ADS)

    Yang, Hong-Jin; Park, Changbom; Park, Myeong-Gu

    2005-05-01

    We have compiled and analyzed historical Korean meteor and meteor shower records in three Korean official history books, Samguksagi which covers the three Kingdoms period (57 B.C.-A.D. 935), Goryeosa of Goryeo dynasty (A.D. 918-1392), and Joseonwangjosillok of Joseon dynasty (A.D. 1392-1910). We have found 3861 meteor and 31 meteor shower records. We have confirmed the peaks of Perseids and an excess due to the mixture of Orionids, north-Taurids, or Leonids through the Monte Carlo test. The peaks persist from the period of Goryeo dynasty to that of Joseon dynasty, for almost one thousand years. Korean records show a decrease of Perseids activity and an increase of Orionids/north-Taurids/Leonids activity. We have also analyzed seasonal variation of sporadic meteors from Korean records. We confirm the seasonal variation of sporadic meteors from the records of Joseon dynasty with the maximum number of events being roughly 1.7 times the minimum. The Korean records are compared with Chinese and Japanese records for the same periods. Major features in Chinese meteor shower records are quite consistent with those of Korean records, particularly for the last millennium. Japanese records also show Perseids feature and Orionids/north-Taurids/Leonids feature, although they are less prominent compared to those of Korean or Chinese records.

  8. Knut Lundmark, meteors and an early Swedish crowdsourcing experiment.

    PubMed

    Kärnfelt, Johan

    2014-10-01

    Mid twentieth century meteor astronomy demanded the long-term compilation of observations made by numerous individuals over an extensive geographical area. Such a massive undertaking obviously required the participation of more than just professional astronomers, who often sought to expand their ranks through the use of amateurs that had a basic grasp of astronomy as well as the night sky, and were thus capable of generating first-rate astronomical reports. When, in the 1920s, renowned Swedish astronomer Knut Lundmark turned his attention to meteor astronomy, he was unable to rely even upon this solution. In contrast to many other countries at the time, Sweden lacked an organized amateur astronomy and thus contained only a handful of competent amateurs. Given this situation, Lundmark had to develop ways of engaging the general public in assisting his efforts. To his advantage, he was already a well-established public figure who had published numerous popular science articles and held talks from time to time on the radio. During the 1930s, this prominence greatly facilitated his launching of a crowdsourcing initiative for the gathering of meteor observations. This paper consists of a detailed discussion concerning the means by which Lundmark's initiative disseminated astronomical knowledge to the general public and encouraged a response that might directly contribute to the advancement of science. More precisely, the article explores the manner in which he approached the Swedish public, the degree to which that public responded and the extent to which his efforts were successful. The primary aim of this exercise is to show that the apparently recent Internet phenomenon of 'crowdsourcing', especially as it relates to scientific research, actually has a pre-Internet history that is worth studying. Apart from the fact that this history is interesting in its own right, knowing it can provide us with a fresh vantage point from which to better comprehend and appreciate

  9. Knut Lundmark, meteors and an early Swedish crowdsourcing experiment.

    PubMed

    Kärnfelt, Johan

    2014-10-01

    Mid twentieth century meteor astronomy demanded the long-term compilation of observations made by numerous individuals over an extensive geographical area. Such a massive undertaking obviously required the participation of more than just professional astronomers, who often sought to expand their ranks through the use of amateurs that had a basic grasp of astronomy as well as the night sky, and were thus capable of generating first-rate astronomical reports. When, in the 1920s, renowned Swedish astronomer Knut Lundmark turned his attention to meteor astronomy, he was unable to rely even upon this solution. In contrast to many other countries at the time, Sweden lacked an organized amateur astronomy and thus contained only a handful of competent amateurs. Given this situation, Lundmark had to develop ways of engaging the general public in assisting his efforts. To his advantage, he was already a well-established public figure who had published numerous popular science articles and held talks from time to time on the radio. During the 1930s, this prominence greatly facilitated his launching of a crowdsourcing initiative for the gathering of meteor observations. This paper consists of a detailed discussion concerning the means by which Lundmark's initiative disseminated astronomical knowledge to the general public and encouraged a response that might directly contribute to the advancement of science. More precisely, the article explores the manner in which he approached the Swedish public, the degree to which that public responded and the extent to which his efforts were successful. The primary aim of this exercise is to show that the apparently recent Internet phenomenon of 'crowdsourcing', especially as it relates to scientific research, actually has a pre-Internet history that is worth studying. Apart from the fact that this history is interesting in its own right, knowing it can provide us with a fresh vantage point from which to better comprehend and appreciate

  10. Knut Lundmark, meteors and an early Swedish crowdsourcing experiment.

    PubMed

    Kärnfelt, Johan

    2014-10-01

    Mid twentieth century meteor astronomy demanded the long-term compilation of observations made by numerous individuals over an extensive geographical area. Such a massive undertaking obviously required the participation of more than just professional astronomers, who often sought to expand their ranks through the use of amateurs that had a basic grasp of astronomy as well as the night sky, and were thus capable of generating first-rate astronomical reports. When, in the 1920s, renowned Swedish astronomer Knut Lundmark turned his attention to meteor astronomy, he was unable to rely even upon this solution. In contrast to many other countries at the time, Sweden lacked an organized amateur astronomy and thus contained only a handful of competent amateurs. Given this situation, Lundmark had to develop ways of engaging the general public in assisting his efforts. To his advantage, he was already a well-established public figure who had published numerous popular science articles and held talks from time to time on the radio. During the 1930s, this prominence greatly facilitated his launching of a crowdsourcing initiative for the gathering of meteor observations. This paper consists of a detailed discussion concerning the means by which Lundmark's initiative disseminated astronomical knowledge to the general public and encouraged a response that might directly contribute to the advancement of science. More precisely, the article explores the manner in which he approached the Swedish public, the degree to which that public responded and the extent to which his efforts were successful. The primary aim of this exercise is to show that the apparently recent Internet phenomenon of 'crowdsourcing', especially as it relates to scientific research, actually has a pre-Internet history that is worth studying. Apart from the fact that this history is interesting in its own right, knowing it can provide us with a fresh vantage point from which to better comprehend and appreciate

  11. The First Year of Croatian Meteor Network

    NASA Astrophysics Data System (ADS)

    Andreic, Zeljko; Segon, Damir

    2010-08-01

    The idea and a short history of Croatian Meteor Network (CMN) is described. Based on use of cheap surveillance cameras, standard PC-TV cards and old PCs, the Network allows schools, amateur societies and individuals to participate in photographic meteor patrol program. The network has a strong educational component and many cameras are located at or around teaching facilities. Data obtained by these cameras are collected and processed by the scientific team of the network. Currently 14 cameras are operable, covering a large part of the croatian sky, data gathering is fully functional, and data reduction software is in testing phase.

  12. Electrophonic sounds from large meteor fireballs

    NASA Astrophysics Data System (ADS)

    Keay, Colin S. L.

    1992-06-01

    Anomalous sounds from large meteor fireballs, anomalous because they are audible simultaneously with the sighting, have been a matter for debate for over two centuries. Only a minority of observers perceive them. Ten years ago a viable physical explanation was developed (Keay, 1980) which accounts for the phenomenon in terms of ELF/VLF radiation from the fireball plasma being transduced into acoustic waves whenever appropriate objects happen to be in the vicinity of an observer. This explanation has now been verified observationally and supported by other evidence including the study of meteor fireball light curves reported here.

  13. An Investigation of Meteors in Early April

    NASA Astrophysics Data System (ADS)

    Arter, Terrance R.; Williams, Iwan P.

    1995-01-01

    In conducting a search through the IAU Meteor Catalogue at Lund, a peak in activity on April 8th, not corresponding to any known shower was discovered. Analysis of the orbit shows that a subset of those meteors originated on very coherent orbits. It is suggested that there could either represent a hither to unidentified stream or that they are meteoroids which, like the April Lyrids, were ejected from Comet Thatcher but have arrived onto their current orbits as a consequence primarily of Poynting - Robertson drag.

  14. Antarctic ozone - Meteoric control of HNO3

    NASA Astrophysics Data System (ADS)

    Prather, Michael J.; Rodriguez, Jose M.

    1988-01-01

    Atmospheric circulation leads to an accumulation of debris from meteors in the Antarctic stratosphere at the beginning of austral spring. The major component of meteoric material is alkaline, comprised predominantly of the oxides of magnesium and iron. These metals may neutralize the natural acidity of stratospheric aerosols, remove nitric acid from the gas phase, and bond it as metal nitrates in the aerosol phase. Removal of nitric acid vapor has been previously shown to be a critical link in the photochemical depletion of ozone in the Antarctic spring, by allowing for increased catalytic loss from chlorine and bromine.

  15. Meteor spectra from AMOS video system

    NASA Astrophysics Data System (ADS)

    Gajdoš, Š.; Tóth, J.; Kornoš, L.

    2015-01-01

    We present a report on the observation of enhanced activity from the Ursids meteor shower using the all-sky camera, at the AGO Modra, on Dec. 22-23, 2014. The time of maximum is in good accordance with the predictions of some authors. We derived a single-station meteor radiant, RA = 217.9° ± 0.1°, DEC = +76.4° ± 0.1° at solar longitude S.L. = 270.9°, along with the activity profile of the Ursid outburst with the maximum occurring at Dec. 23th, 00h40m UT ± 30 min.

  16. Meteor spectra from AMOS video system

    NASA Astrophysics Data System (ADS)

    Rudawska, Regina; Tóth, Juraj; Kalmančok, Dušan; Zigo, Pavol; Matlovič, Pavol

    2016-04-01

    Here we demonstrate the capability of the updated All-Sky Meteor Orbit System (AMOS) (called AMOS-Spec) to measure the main element abundances of meteors. The AMOS-Spec program has been created with the intention of carrying out regular systematic spectroscopic observations. At the same time, the meteoroid trajectory and pre-atmospheric orbit are independently measured from data collected by the AMOS camera network. This, together with spectral information, allows us to find the link between the meteoroid and its parent body, from both dynamical and physical consideration. Here we report results for 35 selected cases.

  17. In Situ Measurements of Meteoric Ions

    NASA Technical Reports Server (NTRS)

    Grebowsky, Joseph M.; Aiken, Arthur C.; Einaudi, Franco (Technical Monitor)

    2001-01-01

    Extraterrestrial material is the source of metal ions in the Earth's atmosphere, Each year approx. 10(exp 8) kg of material is intercepted by the Earth. The origin of this material is predominantly solar orbiting interplanetary debris from comets or asteroids that crosses the Earth's orbit. It contains a very small amount of interstellar material. On occasion the Earth passes through enhanced amounts of debris associated with the orbit of a decaying comet. This leads to enhanced meteor shower displays for up to several days. The number flux of shower material is typically several times the average sporadic background influx of material. Meteoric material is some of the earliest material formed in the solar system. By studying the relative elemental abundances of atmospheric metal ions, information can be gained on the chemical composition of cometary debris and the chemical makeup of the early solar system. Using in situ sampling with rocket-borne ion mass spectrometers; there have been approximately 50 flights that made measurements of the metal ion abundances at attitudes between 80 and 130 km. It is this altitude range where incoming meteoric particles am ablated, the larger ones giving rise to visible meteor. displays. In several rocket measurements isotopic ratios of different atomic ion mass components and metal molecular ion concentrations have been determined and used to identify unambiguously the measured species and to investigate the processes controlling the metal ion distributions The composition of the Earth's ionosphere was first sampled by an ion mass spectrometer flown an a rocket in 1956. In 1958 a rocket-borne ion spectrometer identified, fbr the first time, a layer of metal ions near 95 km. These data were interpreted as evidence of an extraterrestrial rather than a terrestrial source. Istomin predicted: "It seems probable that with some improvement in the method that analysis of the ion composition in the E-region may be used for determining

  18. The Radio Meteor Zoo: a citizen science project

    NASA Astrophysics Data System (ADS)

    Calders, S.; Verbeeck, C.; Lamy, H.; Martínez Picar, A.

    2016-01-01

    Scientists from the BRAMS radio meteor network have started a citizen science project called Radio Meteor Zoo in collaboration with Zooniverse in order to identify meteor reflections in BRAMS spectrograms. First, a small-scale version of the Radio Meteor Zoo was carried out with a sample of meteor identifications in 12 spectrograms by 35 volunteers. Results are presented here and allowed us to define a method that reliably detects meteor reflections based on the identifications by the volunteers. It turns out that, if each spectrogram is inspected by 10 volunteers, hit and false detection percentages of 95% respectively 6% are expected. The Radio Meteor Zoo is online at https://www.zooniverse.org/projects/zooniverse/radio-meteor-zoo. Citizen scientists are kindly invited to inspect spectrograms.

  19. Exploring the relationship between meteor parameters based on photographic data

    NASA Astrophysics Data System (ADS)

    Yancheva, Y.; Hristova, S.; Bojurova, E.

    2016-01-01

    The paper presents an attempt to investigate the relationship between the luminosity and the linear length of the meteors, based on photographic observations of the Geminid meteor shower during the night of maximum in December 2015.

  20. Independent identification of meteor showers in EDMOND database

    NASA Astrophysics Data System (ADS)

    Rudawska, R.; Matlovič, P.; Tóth, J.; Kornoš, L.

    2015-12-01

    Cooperation and data sharing among national networks and International Meteor Organization Video Meteor Database (IMO VMDB) resulted in European viDeo MeteOr Network Database (EDMOND). The current version of the database (EDMOND 5.0) contains 144 749 orbits collected from 2001 to 2014. This paper presents the results obtained by a proposed new independent method of meteor showers identification, which is applied to the current version of the database (EDMOND 5.0). In the first step of the survey we used the DSH criterion to find groups around each meteor within the similarity threshold. Mean parameters of the groups were calculated and compared using a new function DX based on geocentric parameters (λ⊙, α, δ, and Vg). Similar groups were merged into final clusters (representing meteor showers), and compared with the IAU Meteor Data Center list of meteor showers.

  1. Optical studies of meteors at Mount Hopkins Observatory

    NASA Technical Reports Server (NTRS)

    Weekes, T. C.; Williams, J. T.

    1974-01-01

    The 10-m optical reflector and an array of phototubes are used to extend the optical measurements beyond the present limit achieved by the Vidicon system. The first detection of optical meteors with M sub v = + 12 is reported. It is hoped that this system can be used to determine intermediate points in the meteor frequency mass curve for sporadic meteors and to study in detail the faint components of meteor showers. Preliminary observations made on three nights in September 1974 are presented.

  2. On associations of Apollo asteroids with meteor streams

    NASA Technical Reports Server (NTRS)

    Porubcan, V.; Stohl, Jan; Vana, R.

    1992-01-01

    Potential associations of Apollo asteroids with meteor streams are searched on the basis of the orbital parameters comparison. From all Apollo asteroids discovered through 1991 June those are only selected for further analysis whose orbits approach to less than 0.1 AU to the Earth's orbit. Their orbits are compared with precise photographic orbits of individual meteors from the Meteor Data Center in Lund. Results on the associations of asteroids with meteor streams are presented and discussed.

  3. Meteor Search by Spirit, Sol 668

    NASA Technical Reports Server (NTRS)

    2005-01-01

    [figure removed for brevity, see original site] Annotated Meteor Search by Spirit, Sol 668

    The panoramic cameras on NASA's Mars Exploration Rovers are about as sensitive as the human eye at night. The cameras can see the same bright stars that we can see from Earth, and the same patterns of constellations dot the night sky. Scientists on the rover team have been taking images of some of these bright stars as part of several different projects. One project is designed to try to capture 'shooting stars,' or meteors, in the martian night sky. 'Meteoroids' are small pieces of comets and asteroids that travel through space and eventually run into a planet. On Earth, we can sometimes see meteoroids become brilliant, long 'meteors' streaking across the night sky as they burn up from the friction in our atmosphere. Some of these meteors survive their fiery flight and land on the surface (or in the ocean) where, if found, they are called 'meteorites.' The same thing happens in the martian atmosphere, and Spirit even accidentally discovered a meteor while attempting to obtain images of Earth in the pre-dawn sky back in March, 2004 (see http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20040311a.html, and Selsis et al. (2005) Nature, vol 435, p. 581). On Earth, some meteors come in 'storms' or 'showers' at predictable times of the year, like the famous Perseid meteor shower in August or the Leonid meteor shower in November. These 'storms' happen when Earth passes through the same parts of space where comets sometimes pass. The meteors we see at these times are from leftover debris that was shed off of these comets.

    The same kind of thing is predicted for Mars, as well. Inspired by calculations about Martian meteor storms by meteor scientists from the University of Western Ontario in Canada and the Centre de Recherche en Astrophysique de Lyon in France, and also aided by other meteor research colleagues from NASA's Marshall Space Flight Center, scientists on

  4. Results of the IMO Video Meteor Network - June 2015

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Crivello, Stefano; Stomeo, Enrico; Barentsen, Geert; Goncalves, Rui; Saraiva, Carlos; Maciejewski, Maciej; Maslov, Mikhail

    2015-10-01

    Observations of the IMO Video Meteor Network are presented for 2015 June. Activity profile is presented for the Daytime Arietids, based on 28 shower meteors. The meteor rate of the Daytime Arietids between June 5 and 11, normalized for the limiting magnitude and angular velocity, is found to be about one quarter of that of the eta-Aquariids during their maximum.

  5. Determination of meteor flux distribution over the celestial sphere

    NASA Technical Reports Server (NTRS)

    Andreev, V. V.; Belkovich, O. I.; Filimonova, T. K.; Sidorov, V. V.

    1992-01-01

    A new method of determination of meteor flux density distribution over the celestial sphere is discussed. The flux density was derived from observations by radar together with measurements of angles of arrival of radio waves reflected from meteor trails. The role of small meteor showers over the sporadic background is shown.

  6. Results of the IMO Video Meteor Network - October 2014

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Crivello, Stefano; Stomeo, Enrico; Barentsen, Geert; Goncalves, Rui; Saraiva, Carlos; Maciewski, Maciej; Maslov, Mikhail

    2015-02-01

    A record number of 86 cameras of the IMO Video Meteor Network collected over 11 000 hours worth of data in 2014 October, recording almost 52 000 meteors. Yearly flux density profiles are presented for the Orionids, Leonis Minorids, October Camelopardalids, and October Ursae Majorids, covering the period from 2011 to 2014. Population indexes are calculated for all four meteor showers.

  7. Easy way to estimate meteor brightness on TV frames

    NASA Astrophysics Data System (ADS)

    Leonov, V. A.; Bagrov, A. V.

    2016-01-01

    The traditional method of the meteor brightness measurements claims that the meteor brightness is equal to the stellar magnitude of a star that looks like a meteor in the brightest point of its track. This rule was convenient for the comparison of meteor observations by different observers and for the analysis of the brightness distributions of meteors from observed showers. This traditional method suffers from systematic errors, particularly those that arise from using stellar brightness measured in specific spectral wave bands different from the observer's ones, but mainly due to neglecting the influence of the meteor angular velocity on the real meteor brightness. To get a proper estimate of the meteor brightness that is a measure of the ground meteor illumination in the non-systematic units, an observer must take into account that the effective exposition of a meteor image in any resolution element of its track is a few times shorter than the corresponding exposition of a star image in the same frame. We propose a very simple method for improved estimations of meteor brightness by applying a correction to the meteor stellar magnitude obtained within the traditional framework.

  8. The activity of autumn meteor showers in 2006-2008

    NASA Astrophysics Data System (ADS)

    Kartashova, Anna

    2015-03-01

    The purpose of meteor observations in INASAN is the study of meteor showers, as the elements of the migrant substance of the Solar System, and estimation of risk of hazardous collisions of spacecrafts with the particles of streams. Therefore we need to analyze the meteor events with brightness of up to 8 m, which stay in meteoroid streams for a long time and can be a hazardous for the spacecraft. The results of our single station TV observations of autumn meteor showers for the period from 2006 to 2008 are presented. The high-sensitive hybrid camera (the system with coupled of the Image Intensifier) FAVOR with limiting magnitude for meteors about 9m. . .10m in the field of view 20 × 18 was used for observations. In 2006-2008 from October to November more than 3 thousand of meteors were detected, 65% from them have the brightness from 6m to 9m. The identification with autumn meteor showers (Orionids, Taurids, Draconids, Leonids) was carried out. In order to estimate the density of the influx of meteor matter to the Earth for these meteor showers the Index of meteor activity (IMA) was calculated. The IMA distribution for the period 2006 - 2008 is given. The distributions of autumn meteor showers (the meteors with brightness of up to 8 m) by stellar magnitude from 2006 to 2008 are also presented.

  9. 47 CFR 90.250 - Meteor burst communications.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 47 Telecommunication 5 2012-10-01 2012-10-01 false Meteor burst communications. 90.250 Section 90... PRIVATE LAND MOBILE RADIO SERVICES Non-Voice and Other Specialized Operations § 90.250 Meteor burst communications. Meteor burst communications may be authorized for the use of private radio stations subject...

  10. 47 CFR 90.250 - Meteor burst communications.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 47 Telecommunication 5 2011-10-01 2011-10-01 false Meteor burst communications. 90.250 Section 90... PRIVATE LAND MOBILE RADIO SERVICES Non-Voice and Other Specialized Operations § 90.250 Meteor burst communications. Meteor burst communications may be authorized for the use of private radio stations subject...

  11. 47 CFR 90.250 - Meteor burst communications.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 47 Telecommunication 5 2010-10-01 2010-10-01 false Meteor burst communications. 90.250 Section 90... PRIVATE LAND MOBILE RADIO SERVICES Non-Voice and Other Specialized Operations § 90.250 Meteor burst communications. Meteor burst communications may be authorized for the use of private radio stations subject...

  12. 47 CFR 90.250 - Meteor burst communications.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 47 Telecommunication 5 2013-10-01 2013-10-01 false Meteor burst communications. 90.250 Section 90... PRIVATE LAND MOBILE RADIO SERVICES Non-Voice and Other Specialized Operations § 90.250 Meteor burst communications. Meteor burst communications may be authorized for the use of private radio stations subject...

  13. 47 CFR 90.250 - Meteor burst communications.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 47 Telecommunication 5 2014-10-01 2014-10-01 false Meteor burst communications. 90.250 Section 90... PRIVATE LAND MOBILE RADIO SERVICES Non-Voice and Other Specialized Operations § 90.250 Meteor burst communications. Meteor burst communications may be authorized for the use of private radio stations subject...

  14. The Census of Marine Life on Seamounts: results from a global science program

    NASA Astrophysics Data System (ADS)

    Stocks, K.; Clark, M.; Rowden, A.; Consalvey, M.

    2010-12-01

    CenSeam (a Global Census of Marine Life on Seamounts) is a network of more than 500 scientists, policy makers and conservationists around the world. These participants are collaborating to increase our understanding of the factors driving seamount community composition and diversity, such that we can better understand and manage the effects of human activities. The major scientific outcomes of the CenSeam community include the findings that 1) Seamount community composition is often similar to surrounding habitats; however, community structure can be different. 2) Contrary to conventional wisdom, few seamounts follow island biogeography predictions. 3) Seamounts can support a higher benthic biomass than surrounding habitats. 4) Seamounts can support species and communities new to science, and represent range extensions for known species, which are being described from CenSeam voyages. 5) For the first time, the extent of the vulnerability and risk to seamount benthic communities from fishing has been quantified. 6) Whilst long assumed, CenSeam researchers have demonstrated that seamount communities are disturbed by fishing and are slow to recover. And 7) Seamounts might act as repositories of biodiversity during future periods of extreme environmental change, as they have likely done in the past. The major products of Censeam include 1) a book synthesizing seamount knowledge: Seamounts: Ecology, Fisheries and Conservation (from Blackwell Publishing); 2) a recent review of the structure and function of seamount benthic communities, human impacts, and seamount management and conservation (Ann Rev Mar Sci); 3) hundreds of scientific publications, including Special Issues in Marine Ecology and Oceanography (in collaboration with the Seamount Biogeogsciences Network), and a Special Collection in PLoSONE; 4) guidance documents and formal advising for seamount management communities, including the United Nations Environment Program, International Seabed Authority

  15. Dredged trachyte and basalt from kodiak seamount and the adjacent aleutian trench, alaska.

    PubMed

    Forbes, R B; Hoskin, C M

    1969-10-24

    Blocky fragments of aegirine-augite trachyte (with accompanying icerafted gravels.) were recovered from the upper slopes of Kodiak Seamount in several dredge hauls. An alkali basalt pillow segment was also dredged from a moatlike depression, at a depth of 5000 meters, near the west base of the seamount. These retrievals confirm the volcanic origin of Kodiak Seamount and further support the view of Engel, Engel, and Havens that the higher elevations of seamounts are composed of alkali basalts or related variants.

  16. Time-Dependent Flexural Deformation Beneath the Emperor Seamounts

    NASA Astrophysics Data System (ADS)

    Wessel, P.; Watts, A. B.; Kim, S. S.

    2014-12-01

    The Hawaii-Emperor seamount chain stretches over 6000 km from the Big Island of Hawaii to the subduction cusp off Kamchatka and represents a near-continuous record of hotspot volcanism since the Late Cretaceous. The load of these seamounts and islands has caused the underlying lithosphere to deform, developing a flexural flanking moat that is now largely filled with volcanoclastic sediments. Because the age differences between the seafloor and the seamounts vary by an order of magnitude or more along the chain, the Hawaii-Emperor chain and surrounding area is considered a natural laboratory for lithospheric flexure and has been studied extensively in order to infer the rheology of the oceanic lithosphere. While most investigations have focused on the Hawaiian Islands and proximal seamounts (where data sets are more complete, including seismic reflection and refraction, swath bathymetry and even mapping and dating of drowned reef terraces), far fewer studies have examined the flexural deformation beneath the remote Emperor chain. Preliminary analysis of satellite altimetry data shows the flexural moats to be associated with very large negative gravity anomalies relative to the magnitudes of the positive anomalies over the loads, suggesting considerable viscous or viscoelastic relaxation since the loads were emplaced 50-80 Myr ago. In our study, we will attempt to model the Emperor seamount chain load as a superposition of individual elliptical Gaussian seamounts with separate loading histories. We use Optimal Robust Separation (ORS) techniques to extract the seamount load from the regional background bathymetry and partition the residual load into a set of individual volcanoes. The crustal age grid and available seamount dates are used to construct a temporal loading model and evaluate the flexural response of the lithosphere beneath the Emperor seamounts. We explore a variety of rheological models and loading scenarios that are compatible with the inferred load

  17. Observed deep energetic eddies by seamount wake

    NASA Astrophysics Data System (ADS)

    Chen, Gengxin; Wang, Dongxiao; Dong, Changming; Zu, Tingting; Xue, Huijie; Shu, Yeqiang; Chu, Xiaoqing; Qi, Yiquan; Chen, Hui

    2015-11-01

    Despite numerous surface eddies are observed in the ocean, deep eddies (a type of eddies which have no footprints at the sea surface) are much less reported in the literature due to the scarcity of their observation. In this letter, from recently collected current and temperature data by mooring arrays, a deep energetic and baroclinic eddy is detected in the northwestern South China Sea (SCS) with its intensity, size, polarity and structure being characterized. It remarkably deepens isotherm at deep layers by the amplitude of ~120 m and induces a maximal velocity amplitude about 0.18 m/s, which is far larger than the median velocity (0.02 m/s). The deep eddy is generated in a wake when a steering flow in the upper layer passes a seamount, induced by a surface cyclonic eddy. More observations suggest that the deep eddy should not be an episode in the area. Deep eddies significantly increase the velocity intensity and enhance the mixing in the deep ocean, also have potential implication for deep-sea sediments transport.

  18. Observed deep energetic eddies by seamount wake

    PubMed Central

    Chen, Gengxin; Wang, Dongxiao; Dong, Changming; Zu, Tingting; Xue, Huijie; Shu, Yeqiang; Chu, Xiaoqing; Qi, Yiquan; Chen, Hui

    2015-01-01

    Despite numerous surface eddies are observed in the ocean, deep eddies (a type of eddies which have no footprints at the sea surface) are much less reported in the literature due to the scarcity of their observation. In this letter, from recently collected current and temperature data by mooring arrays, a deep energetic and baroclinic eddy is detected in the northwestern South China Sea (SCS) with its intensity, size, polarity and structure being characterized. It remarkably deepens isotherm at deep layers by the amplitude of ~120 m and induces a maximal velocity amplitude about 0.18 m/s, which is far larger than the median velocity (0.02 m/s). The deep eddy is generated in a wake when a steering flow in the upper layer passes a seamount, induced by a surface cyclonic eddy. More observations suggest that the deep eddy should not be an episode in the area. Deep eddies significantly increase the velocity intensity and enhance the mixing in the deep ocean, also have potential implication for deep-sea sediments transport. PMID:26617343

  19. Observed deep energetic eddies by seamount wake.

    PubMed

    Chen, Gengxin; Wang, Dongxiao; Dong, Changming; Zu, Tingting; Xue, Huijie; Shu, Yeqiang; Chu, Xiaoqing; Qi, Yiquan; Chen, Hui

    2015-01-01

    Despite numerous surface eddies are observed in the ocean, deep eddies (a type of eddies which have no footprints at the sea surface) are much less reported in the literature due to the scarcity of their observation. In this letter, from recently collected current and temperature data by mooring arrays, a deep energetic and baroclinic eddy is detected in the northwestern South China Sea (SCS) with its intensity, size, polarity and structure being characterized. It remarkably deepens isotherm at deep layers by the amplitude of ~120 m and induces a maximal velocity amplitude about 0.18 m/s, which is far larger than the median velocity (0.02 m/s). The deep eddy is generated in a wake when a steering flow in the upper layer passes a seamount, induced by a surface cyclonic eddy. More observations suggest that the deep eddy should not be an episode in the area. Deep eddies significantly increase the velocity intensity and enhance the mixing in the deep ocean, also have potential implication for deep-sea sediments transport.

  20. Meteor Shower Activity Derived from "Meteor Watching Public-Campaign" in Japan

    NASA Technical Reports Server (NTRS)

    Sato, M.; Watanabe, J.

    2011-01-01

    We tried to analyze activities of meteor showers from accumulated data collected by public campaigns for meteor showers which were performed as outreach programs. The analyzed campaigns are Geminids (in 2007 and 2009), Perseids (in 2008 and 2009), Quadrantids (in 2009) and Orionids (in 2009). Thanks to the huge number of reports, the derived time variations of the activities of meteor showers is very similar to those obtained by skilled visual observers. The values of hourly rates are about one-fifth (Geminids 2007) or about one-fourth (Perseids 2008) compared with the data of skilled observers, mainly due to poor observational sites such as large cities and urban areas, together with the immature skill of participants in the campaign. It was shown to be highly possible to estimate time variation in the meteor shower activity from our campaign.

  1. Automated Meteor Fluxes with a Wide-Field Meteor Camera Network

    NASA Technical Reports Server (NTRS)

    Blaauw, R. C.; Campbell-Brown, M. D.; Cooke, W.; Weryk, R. J.; Gill, J.; Musci, R.

    2013-01-01

    Within NASA, the Meteoroid Environment Office (MEO) is charged to monitor the meteoroid environment in near ]earth space for the protection of satellites and spacecraft. The MEO has recently established a two ]station system to calculate automated meteor fluxes in the millimeter ]size ]range. The cameras each consist of a 17 mm focal length Schneider lens on a Watec 902H2 Ultimate CCD video camera, producing a 21.7 x 16.3 degree field of view. This configuration has a red ]sensitive limiting meteor magnitude of about +5. The stations are located in the South Eastern USA, 31.8 kilometers apart, and are aimed at a location 90 km above a point 50 km equidistant from each station, which optimizes the common volume. Both single station and double station fluxes are found, each having benefits; more meteors will be detected in a single camera than will be seen in both cameras, producing a better determined flux, but double station detections allow for non ]ambiguous shower associations and permit speed/orbit determinations. Video from the cameras are fed into Linux computers running the ASGARD (All Sky and Guided Automatic Real ]time Detection) software, created by Rob Weryk of the University of Western Ontario Meteor Physics Group. ASGARD performs the meteor detection/photometry, and invokes the MILIG and MORB codes to determine the trajectory, speed, and orbit of the meteor. A subroutine in ASGARD allows for the approximate shower identification in single station meteors. The ASGARD output is used in routines to calculate the flux in units of #/sq km/hour. The flux algorithm employed here differs from others currently in use in that it does not assume a single height for all meteors observed in the common camera volume. In the MEO system, the volume is broken up into a set of height intervals, with the collecting areas determined by the radiant of active shower or sporadic source. The flux per height interval is summed to obtain the total meteor flux. As ASGARD also

  2. Meteor Search by Spirit, Sol 668

    NASA Technical Reports Server (NTRS)

    2005-01-01

    [figure removed for brevity, see original site] Annotated Meteor Search by Spirit, Sol 668

    The panoramic cameras on NASA's Mars Exploration Rovers are about as sensitive as the human eye at night. The cameras can see the same bright stars that we can see from Earth, and the same patterns of constellations dot the night sky. Scientists on the rover team have been taking images of some of these bright stars as part of several different projects. One project is designed to try to capture 'shooting stars,' or meteors, in the martian night sky. 'Meteoroids' are small pieces of comets and asteroids that travel through space and eventually run into a planet. On Earth, we can sometimes see meteoroids become brilliant, long 'meteors' streaking across the night sky as they burn up from the friction in our atmosphere. Some of these meteors survive their fiery flight and land on the surface (or in the ocean) where, if found, they are called 'meteorites.' The same thing happens in the martian atmosphere, and Spirit even accidentally discovered a meteor while attempting to obtain images of Earth in the pre-dawn sky back in March, 2004 (see http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20040311a.html, and Selsis et al. (2005) Nature, vol 435, p. 581). On Earth, some meteors come in 'storms' or 'showers' at predictable times of the year, like the famous Perseid meteor shower in August or the Leonid meteor shower in November. These 'storms' happen when Earth passes through the same parts of space where comets sometimes pass. The meteors we see at these times are from leftover debris that was shed off of these comets.

    The same kind of thing is predicted for Mars, as well. Inspired by calculations about Martian meteor storms by meteor scientists from the University of Western Ontario in Canada and the Centre de Recherche en Astrophysique de Lyon in France, and also aided by other meteor research colleagues from NASA's Marshall Space Flight Center, scientists on

  3. Bright Meteor Lights Up Atlanta Skies

    NASA Video Gallery

    This video shows a very bright meteor that streaked over the skies of Atlanta, Ga., on the night of Aug. 28, 2011. The view is from an all sky camera in Cartersville, Ga., operated by NASA’s Mars...

  4. Lake Erie Fireball Meteor, Tavistock View

    NASA Video Gallery

    This brief video shows a view of the Aug 8 fireball meteor that entered the atmosphere 54 miles above Lake Erie and moved SSE at 25 km/s, or 55,900 mph. This view is from the all sky camera in Tavi...

  5. Lake Erie Fireball Meteor, Orangeville View

    NASA Video Gallery

    This brief video shows a view of the Aug 8 fireball meteor that entered the atmosphere 54 miles above Lake Erie and moved SSE at 25 km/s, or 55,900 mph. This view is from the all sky camera in Oran...

  6. The radiant distribution of AMOR radar meteors

    NASA Astrophysics Data System (ADS)

    Galligan, D. P.; Baggaley, W. J.

    2005-05-01

    A large data set provided by the highly sensitive Advanced Meteor Orbit Radar (AMOR) facility is used to investigate the structure of the sporadic meteor complex. The helion, antihelion and apex apparent sources are clearly found. Observational bias is then removed to reveal the true source distributions as observed on Earth. A long-standing problem in meteor science has been the difference in observed meteor flux between the helion and antihelion source directions. Consideration of the effects of atmospheric interference and Faraday rotation is found to lead to a closer balance between these. The orbital distributions present within the different regions are also discussed. The apex region is found to have a strong retrograde component and a weaker prograde component that exists at high southerly latitudes and that contains orbits with particularly high inclinations. The retrograde component reduces substantially after inclusion of observational bias corrections. Care should be taken in comparing the results presented here with those from other radar systems: AMOR is sensitive to dust as small in diameter as ~40μm, while the limiting sensitivity of most contemporary systems is an order of magnitude larger.

  7. Lake Erie Fireball Meteor, Mcmaster View

    NASA Video Gallery

    This brief video shows a view of the Aug 8 fireball meteor that entered the atmosphere 54 miles above Lake Erie and moved SSE at 25 km/s, or 55,900 mph. This view is from the all sky camera in Mcma...

  8. Great Lakes: Great Gardening.

    ERIC Educational Resources Information Center

    New York Sea Grant Inst., Albany, NY.

    This folder contains 12 fact sheets designed to improve the quality of gardens near the Great Lakes. The titles are: (1) "Your Garden and the Great Lakes"; (2) "Organic Gardening"; (3) "Fruit and Vegetable Gardening"; (4) "Composting Yard Wastes"; (5) "Herbicides and Water Quality"; (6) "Watering"; (7) "Soil Erosion by Water"; (8) "Soil…

  9. 75 FR 51237 - Fisheries in the Western Pacific; Hawaii Bottomfish and Seamount Groundfish; Management Measures...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-08-19

    .... SUPPLEMENTARY INFORMATION: This document is also available at www.gpoaccess.gov/fr . Fishing for pelagic... Pacific; Hawaii Bottomfish and Seamount Groundfish; Management Measures for Hancock Seamounts to Rebuild...), Amendment 2 would continue a moratorium on fishing at Hancock Seamounts for armorhead...

  10. Residency and spatial use by reef sharks of an isolated seamount and its implications for conservation.

    PubMed

    Barnett, Adam; Abrantes, Kátya G; Seymour, Jamie; Fitzpatrick, Richard

    2012-01-01

    Although marine protected areas (MPAs) are a common conservation strategy, these areas are often designed with little prior knowledge of the spatial behaviour of the species they are designed to protect. Currently, the Coral Sea area and its seamounts (north-east Australia) are under review to determine if MPAs are warranted. The protection of sharks at these seamounts should be an integral component of conservation plans. Therefore, knowledge on the spatial ecology of sharks at the Coral Sea seamounts is essential for the appropriate implementation of management and conservation plans. Acoustic telemetry was used to determine residency, site fidelity and spatial use of three shark species at Osprey Reef: whitetip reef sharks Triaenodon obesus, grey reef sharks Carcharhinus amblyrhynchos and silvertip sharks Carcharhinus albimarginatus. Most individuals showed year round residency at Osprey Reef, although five of the 49 individuals tagged moved to the neighbouring Shark Reef (~14 km away) and one grey reef shark completed a round trip of ~250 km to the Great Barrier Reef. Additionally, individuals of white tip and grey reef sharks showed strong site fidelity to the areas they were tagged, and there was low spatial overlap between groups of sharks tagged at different locations. Spatial use at Osprey Reef by adult sharks is generally restricted to the north-west corner. The high residency and limited spatial use of Osprey Reef suggests that reef sharks would be highly vulnerable to targeted fishing pressure and that MPAs incorporating no-take of sharks would be effective in protecting reef shark populations at Osprey and Shark Reef. PMID:22615782

  11. Residency and spatial use by reef sharks of an isolated seamount and its implications for conservation.

    PubMed

    Barnett, Adam; Abrantes, Kátya G; Seymour, Jamie; Fitzpatrick, Richard

    2012-01-01

    Although marine protected areas (MPAs) are a common conservation strategy, these areas are often designed with little prior knowledge of the spatial behaviour of the species they are designed to protect. Currently, the Coral Sea area and its seamounts (north-east Australia) are under review to determine if MPAs are warranted. The protection of sharks at these seamounts should be an integral component of conservation plans. Therefore, knowledge on the spatial ecology of sharks at the Coral Sea seamounts is essential for the appropriate implementation of management and conservation plans. Acoustic telemetry was used to determine residency, site fidelity and spatial use of three shark species at Osprey Reef: whitetip reef sharks Triaenodon obesus, grey reef sharks Carcharhinus amblyrhynchos and silvertip sharks Carcharhinus albimarginatus. Most individuals showed year round residency at Osprey Reef, although five of the 49 individuals tagged moved to the neighbouring Shark Reef (~14 km away) and one grey reef shark completed a round trip of ~250 km to the Great Barrier Reef. Additionally, individuals of white tip and grey reef sharks showed strong site fidelity to the areas they were tagged, and there was low spatial overlap between groups of sharks tagged at different locations. Spatial use at Osprey Reef by adult sharks is generally restricted to the north-west corner. The high residency and limited spatial use of Osprey Reef suggests that reef sharks would be highly vulnerable to targeted fishing pressure and that MPAs incorporating no-take of sharks would be effective in protecting reef shark populations at Osprey and Shark Reef.

  12. Residency and Spatial Use by Reef Sharks of an Isolated Seamount and Its Implications for Conservation

    PubMed Central

    Barnett, Adam; Abrantes, Kátya G.; Seymour, Jamie; Fitzpatrick, Richard

    2012-01-01

    Although marine protected areas (MPAs) are a common conservation strategy, these areas are often designed with little prior knowledge of the spatial behaviour of the species they are designed to protect. Currently, the Coral Sea area and its seamounts (north-east Australia) are under review to determine if MPAs are warranted. The protection of sharks at these seamounts should be an integral component of conservation plans. Therefore, knowledge on the spatial ecology of sharks at the Coral Sea seamounts is essential for the appropriate implementation of management and conservation plans. Acoustic telemetry was used to determine residency, site fidelity and spatial use of three shark species at Osprey Reef: whitetip reef sharks Triaenodon obesus, grey reef sharks Carcharhinus amblyrhynchos and silvertip sharks Carcharhinus albimarginatus. Most individuals showed year round residency at Osprey Reef, although five of the 49 individuals tagged moved to the neighbouring Shark Reef (∼14 km away) and one grey reef shark completed a round trip of ∼250 km to the Great Barrier Reef. Additionally, individuals of white tip and grey reef sharks showed strong site fidelity to the areas they were tagged, and there was low spatial overlap between groups of sharks tagged at different locations. Spatial use at Osprey Reef by adult sharks is generally restricted to the north-west corner. The high residency and limited spatial use of Osprey Reef suggests that reef sharks would be highly vulnerable to targeted fishing pressure and that MPAs incorporating no-take of sharks would be effective in protecting reef shark populations at Osprey and Shark Reef. PMID:22615782

  13. The Temporary factor in the Physical theory of meteor

    NASA Astrophysics Data System (ADS)

    Smirnov, V. A.

    The physical processes accompanying development of the meteor phenomenon, proceed in various temporary scales. For example, frequently meeting double final flares at meteors of a flow Perseid's occur in time, smaller 0,05 seconds. However, care of heat at the expense of energy of a driven meteor 1 gramme of substance for his evaporation needs time, on the order greater. Thus is explained significant inertness in movement of meteors and independence of light flares of meteor plasma of mechanical changes of structure of meteoroid's.

  14. Internal tidal currents over the summit of cross seamount

    USGS Publications Warehouse

    Noble, M.; Mullineaux, L.S.

    1989-01-01

    Spectral analysis of 46 days of record from a current meter deployed above the summit of Cross Seamount (approximately 300 km west of the Hawaiian Islands) indicates that the strongest current fluctuations were driven by the semidiurnal tide. The tides accounted for 28% of the variance in the current spectrum, were mainly baroclinic in character, and were propagated towards the west-northwest. The amplitude of the S2 current flowing parallel to the major axis of the current ellipse ranged between 4 and 9 cm-1 s. The S2 current was 1.5 times larger than the M2 current. This ratio is 4 times larger than is expected for this region of the Pacific and is not a general characteristics of flows over seamounts. Instantaneous current speeds over the seamount often exceeded 20 cm s-1 and were probably responsible for the small ripples observed on the sediment-covered regions of the summit. ?? 1990.

  15. Geophysical exploration of the Southeast Tyrrhenian Sea (Italy): Seamounts batimetries

    NASA Astrophysics Data System (ADS)

    Passaro, Salvatore; Milano, Girolamo

    2010-05-01

    The Tyrrhenian Sea is a young extensional basin in the Central Mediterranean that formed within a complex convergent boundary between Africa and Eurasian Plates. Its opening, associated to the west dipping subduction of the Ionian lithosphere, started about 11 My ago and was marked first by an EW and successively by an ESE directed extension. This last mainly affected the Southeast Tyrrhenian Sea and led to the formation of the Marsili ocean-like basin. This large-scale extension produced the onset of volcanism throughout the Tyrrhenian Sea and the formation of several seamounts. High values of heat flow (>150 mW m-2) and the thin crust (7 km on average) and lithosphere (30 km on average) testify the young age of formation of oceanic crust in the Southeast Tyrrhenian Sea. On November 2007, a multidisciplinary oceanographic survey was carried out in the Southeast Tyrrhenian Sea by a group of researchers of the IAMC-CNR (Naples), Osservatorio Vesuviano (INGV, Naples), NOAA (Seattle) and GNS (New Zealand) on board of the R/V Urania. The main aim of the survey was the identification and the exploration of potential active volcanic and/or hydrothermal vents on the seamounts located in the Southeast Tyrrhenian Sea. Twelve Tyrrhenian seamounts have been explored with a modified CTD system, in order to acquire "tow-yo" profiles in dynamic mode (real time monitoring of physical and chemical parameters of seawater along vertical/horizontal profiles). In addiction, Multibeam swath bathymetry was carried out over fifteen seamounts. The strategy for the achieving of the aim consisted in two phases: i) row multibeam acquisition of the sea floor morphology to verify, confirm or review all available data, ii) tow-yo activity and seawater sampling. Here, we show the main results of bathymetric data acquisition carried out over fifteen seamounts with the use of the Reson Seabat 8160 multibeam sonar system mounted on keel of the R/V Urania. The most interesting morphostructural

  16. Comparison of TV magnitudes and visual magnitudes of meteors

    NASA Astrophysics Data System (ADS)

    Shigeno, Yoshihiko; Toda, Masayuki

    2008-08-01

    The generally accepted belief is that a meteor, with a large amount of infrared rays, can be captured brighter than it actually is by infrared-sensitive image intensifiers (I.I.) or CCD. We conducted observations of meteors using three methodologies: 1) I.I. with an attached filter that has the same spectral response as the human eye at night vision, 2) I.I. without the filter and 3) visually to determine meteor magnitudes. A total of 31 members of the astronomical club at Meiji University observed 50 Perseid meteors, 19 Geminid meteors as well as 44 sporadic meteors and the results were tabulated. The results helped us understand that on average I.I. can record meteors as brighter than visual observation by the magnitude equivalent of 0.5 for Perseids, 1.0 for Geminids and 0.5 for sporadic meteors. For I.I. with a filter that has the same spectral response the human eye at night vision, it turned out that we could obtain almost the same magnitude with observation by the human eye. We learned that a bright meteor with negative magnitude can be observed by I.I. brighter than the human eye. From several examples, we found I.I. could record a meteor with about -1 visual magnitude as brighter by about three magnitudes. We could probably do so because a bright meteor with negative magnitude may contain more infrared rays and the brightness could be amplified.

  17. Physical and dynamical studies of meteors. [radar observation of fragmentation

    NASA Technical Reports Server (NTRS)

    Southworth, R. B.; Sekanina, Z.

    1974-01-01

    Distribution of meteors in streams detected in the synoptic-year meteor sample plus a study of the fragmentation characteristics of the synoptic-year meteor sample are presented. Population coefficients and dispersion coefficients were determined for each meteor stream. These two parameters serve to determine the number of definite members of the stream in the sample used, and to estimate the actual space density of meteor streams. From results of the fragmentation study, it appears that the main body of most radar meteors does not ablate fragments layer by layer, but collapses rather suddenly under dynamic pressures on the order of 0,0002 dynes/cm. Furthermore, it is believed that fragmentation does not cause a serious selection effect in the radar meteor data.

  18. Results of Lunar Impact Observations During Geminid Meteor Shower Events

    NASA Technical Reports Server (NTRS)

    Suggs, R. J.; Suggs, R. M.

    2015-01-01

    the lunar environment associated with larger lunar impactors, but also provides statistical data for verification and improving meteoroid prediction models. Current meteoroid models indicate that the Moon is struck by a sporadic meteoroid with a mass greater than 1 kg over 260 times per year. This number is very uncertain since observations for objects in this mass range are few. Factors of several times, higher or lower, are easily possible. Meteor showers are also present to varying degrees at certain times of the year. The Earth experiences meteor showers when encountering the debris left behind by comets, which is also the case with 2 the Moon. During such times, the rate of shower meteoroids can greatly exceed that of the sporadic background rate for larger meteoroids. Looking for meteor shower impacts on the Moon at about the same time as they occur on Earth will yield important data that can be fed into meteor shower forecasting models, which can then be used to predict times of greater meteoroid hazard on the Moon. The Geminids are one such meteor shower of interest. The Geminids are a major meteor shower that occur in December with a peak intensity occurring usually during the 13th and 14th of the month and appearing to come from a radiant in the constellation Gemini. The Geminids are interesting in that the parent body of the debris stream is an asteroid, which along with the Quadrantids, are the only major meteor showers not originating from a comet. The Geminids parent body, 3200 Phaethon, is about 5 km in diameter and has an orbit that has a 22deg inclination which intersects the main asteroid belt and has a perihelion less than half of Mercury's perihelion distance. Thus, its orbit crosses those of Mars, Earth, Venus, and Mercury. The Geminid debris stream is by far the most massive as compared to the others. When the Earth passes through the stream in mid-December, a peak intensity of approx. equal 120 meteors per hour can be seen. Because of the

  19. The global distribution of seamounts based on 30 arc seconds bathymetry data

    NASA Astrophysics Data System (ADS)

    Yesson, Chris; Clark, Malcolm R.; Taylor, Michelle L.; Rogers, Alex D.

    2011-04-01

    Seamounts and knolls are 'undersea mountains', the former rising more than 1000 m from the seafloor. These features provide important habitats for aquatic predators, demersal deep-sea fish and benthic invertebrates. However most seamounts have not been surveyed and their numbers and locations are not well known. Previous efforts to locate and quantify seamounts have used relatively coarse bathymetry grids. Here we use global bathymetric data at 30 arc-sec resolution to identify seamounts and knolls. We identify 33,452 seamounts and 138,412 knolls, representing the largest global set of identified seamounts and knolls to date. We compare estimated seamount numbers, locations, and depths with validation sets of seamount data from New Zealand and Azores. This comparison indicates the method we apply finds 94% of seamounts, but may overestimate seamount numbers along ridges and in areas where faulting and seafloor spreading creates highly complex topography. The seamounts and knolls identified herein are significantly geographically biased towards areas surveyed with ship-based soundings. As only 6.5% of the ocean floor has been surveyed with soundings it is likely that new seamounts will be uncovered as surveying improves. Seamount habitats constitute approximately 4.7% of the ocean floor, whilst knolls cover 16.3%. Regional distribution of these features is examined, and we find a disproportionate number of productive knolls, with a summit depth of <1.5 km, located in the Southern Ocean. Less than 2% of seamounts are within marine protected areas and the majority of these are located within exclusive economic zones with few on the High Seas. The database of seamounts and knolls resulting from this study will be a useful resource for researchers and conservation planners.

  20. Interferometric Meteor Head Echo Observations using the Southern Argentina Agile Meteor Radar (SAAMER)

    NASA Technical Reports Server (NTRS)

    Janches, D.; Hocking, W.; Pifko, S.; Hormaechea, J. L.; Fritts, D. C.; Brunini, C; Michell, R.; Samara, M.

    2013-01-01

    A radar meteor echo is the radar scattering signature from the free-electrons in a plasma trail generated by entry of extraterrestrial particles into the atmosphere. Three categories of scattering mechanisms exist: specular, nonspecular trails, and head-echoes. Generally, there are two types of radars utilized to detect meteors. Traditional VHF meteor radars (often called all-sky1radars) primarily detect the specular reflection of meteor trails traveling perpendicular to the line of sight of the scattering trail, while High Power and Large Aperture (HPLA) radars efficiently detect meteor head-echoes and, in some cases, non-specular trails. The fact that head-echo measurements can be performed only with HPLA radars limits these studies in several ways. HPLA radars are very sensitive instruments constraining the studies to the lower masses, and these observations cannot be performed continuously because they take place at national observatories with limited allocated observing time. These drawbacks can be addressed by developing head echo observing techniques with modified all-sky meteor radars. In addition, the fact that the simultaneous detection of all different scattering mechanisms can be made with the same instrument, rather than requiring assorted different classes of radars, can help clarify observed differences between the different methodologies. In this study, we demonstrate that such concurrent observations are now possible, enabled by the enhanced design of the Southern Argentina Agile Meteor Radar (SAAMER) deployed at the Estacion Astronomica Rio Grande (EARG) in Tierra del Fuego, Argentina. The results presented here are derived from observations performed over a period of 12 days in August 2011, and include meteoroid dynamical parameter distributions, radiants and estimated masses. Overall, the SAAMER's head echo detections appear to be produced by larger particles than those which have been studied thus far using this technique.

  1. CAMS: Cameras for Allsky Meteor Surveillance to establish minor meteor showers

    NASA Astrophysics Data System (ADS)

    Jenniskens, P.; Gural, P. S.; Dynneson, L.; Grigsby, B. J.; Newman, K. E.; Borden, M.; Koop, M.; Holman, D.

    2011-11-01

    First results are presented from a newly developed meteoroid orbit survey, called CAMS - Cameras for Allsky Meteor Surveillance, which combines meteor detection algorithms for low-light video observations with traditional video surveillance tools. Sixty video cameras at three stations monitor the sky above 31° elevation. Goal of CAMS is to verify meteor showers in search of their parent comets among newly discovered near-Earth objects. This paper outlines the concept of operations, the hardware, and software methods used during operation and in the data reduction pipeline, and accompanies the data release of the first batch of meteoroid orbits. During the month of November 2010, 2169 precisely reduced meteoroid trajectories from 17 nights have an error in the apparent radiant of the trajectory <2° and error in speed <10%. Median values of the error are 0.31° and 0.53 km/s, respectively, sufficient to resolve the intrinsic dispersion of annual meteor showers and resolve minor showers from the sporadic background. The limiting visual magnitude of the cameras is +5.4, recording meteors of +4 magnitude and brighter, bright enough to stand out from the mostly fainter sporadic meteors detected as under dense radar echoes. CAMS readily detected all established showers (6) active during the clear nights in November. Of the showers that needed confirmation, we confirm the theta Aurigids (THA, IAU#390), the chi Taurids (CTA, IAU#388), and the omicron Eridanids (OER, IAU#338). We conclude that the iota November Aurigids (IAR, IAU#248) are in fact the combined activity of the theta Aurigids and chi Taurids, and this shower should be dismissed from the list. Finally, there is also a clustering consistent with the zeta Cancrids (ZCN, IAU#243), but we cannot exclude that this is lower perihelion dust belonging to the Orionid shower. Data are submitted to the IAU Meteor Data Center on a semi-regular basis, and can be accessed also at http://cams.seti.org.

  2. DYNAMICS OF DUST PARTICLES RELEASED FROM OORT CLOUD COMETS AND THEIR CONTRIBUTION TO RADAR METEORS

    SciTech Connect

    Nesvorny, David; Vokrouhlicky, David; Pokorny, Petr; Janches, Diego

    2011-12-10

    The Oort Cloud Comets (OCCs), exemplified by the Great Comet of 1997 (Hale-Bopp), are occasional visitors from the heatless periphery of the solar system. Previous works hypothesized that a great majority of OCCs must physically disrupt after one or two passages through the inner solar system, where strong thermal gradients can cause phase transitions or volatile pressure buildup. Here we study the fate of small debris particles produced by OCC disruptions to determine whether the imprints of a hypothetical population of OCC meteoroids can be found in the existing meteor radar data. We find that OCC particles with diameters D {approx}< 10 {mu}m are blown out from the solar system by radiation pressure, while those with D {approx}> 1 mm have a very low Earth-impact probability. The intermediate particle sizes, D {approx} 100 {mu}m, represent a sweet spot. About 1% of these particles orbitally evolve by Poynting-Robertson drag to reach orbits with semimajor axis a {approx} 1 AU. They are expected to produce meteors with radiants near the apex of Earth's orbital motion. We find that the model distributions of their impact speeds and orbits provide a good match to radar observations of apex meteors, except for the eccentricity distribution, which is more skewed toward e {approx} 1 in our model. Finally, we propose an explanation for the long-standing problem in meteor science related to the relative strength of apex and helion/antihelion sources. As we show in detail, the observed trend, with the apex meteors being more prominent in observations of highly sensitive radars, can be related to orbital dynamics of particles released on the long-period orbits.

  3. Dynamics of Dust Particles Released from Oort Cloud Comets and Their Contribution to Radar Meteors

    NASA Technical Reports Server (NTRS)

    Nesvorny, David; Vokrouhlicky, David; Pokorny, Petr; Janches, Diego

    2012-01-01

    The Oort Cloud Comets (OCCs), exemplified by the Great Comet of 1997 (Hale-Bopp), are occasional visitors from the heatless periphery of the solar system. Previous works hypothesized that a great majority of OCCs must physically disrupt after one or two passages through the inner solar system, where strong thermal gradients can cause phase transitions or volatile pressure buildup. Here we study the fate of small debris particles produced by OCC disruptions to determine whether the imprints of a hypothetical population of OCC meteoroids can be found in the existing meteor radar data. We find that OCC particles with diameters D < or approx. 10 microns are blown out from the solar system by radiation pressure, while those with D > or approx. 1 mm have a very low Earth-impact probability. The intermediate particle sizes, D approx. 100 microns represent a sweet spot. About 1% of these particles orbitally evolve by Poynting-Robertson drag to reach orbits with semimajor axis a approx. 1 AU. They are expected to produce meteors with radiants near the apex of the Earth s orbital motion. We find that the model distributions of their impact speeds and orbits provide a good match to radar observations of apex meteors, except for the eccentricity distribution, which is more skewed toward e approx. 1 in our model. Finally, we propose an explanation for the long-standing problem in meteor science related to the relative strength of apex and helion/antihelion sources. As we show in detail, the observed trend, with the apex meteors being more prominent in observations of highly sensitive radars, can be related to orbital dynamics of particles released on the long-period orbits.

  4. Lava bubble-wall fragments formed by submarine hydrovolcanic explosions on Lo'ihi Seamount and Kilauea Volcano

    USGS Publications Warehouse

    Clague, D.A.; Davis, A.S.; Bischoff, J.L.; Dixon, J.E.; Geyer, R.

    2000-01-01

    Glassy bubble-wall fragments, morphologically similar to littoral limu o Pele, have been found in volcanic sands erupted on Lo'ihi Seamount and along the submarine east rift zone of Kilauea Volcano. The limu o Pele fragments are undegassed with respect to H2O and S and formed by mild steam explosions. Angular glass sand fragments apparently form at similar, and greater, depths by cooling-contraction granulation. The limu o Pele fragments from Lo'ihi Seamount are dominantly tholeiitic basalt containing 6.25-7.25% MgO. None of the limu o Pele samples from Lo'ihi Seamount contains less than 5.57% MgO, suggesting that higher viscosity magmas do not form lava bubbles. The dissolved CO2 and H2O contents of 7 of the limu o Pele fragments indicate eruption at 1200??300 m depth (120??30 bar). These pressures exceed that generally thought to limit steam explosions. We conclude that hydrovolcanic eruptions are possible, with appropriate pre-mixing conditions, at pressures as great as 120 bar.

  5. Frictional Constitutive Parameters for Serpentine Mud from South Chamorro Seamount

    NASA Astrophysics Data System (ADS)

    Noda, H.; Shimamoto, T.; Ishii, T.

    2005-12-01

    The lack of great earthquakes in Izu-Ogasawara and Mariana subduction zones may be associated with low-temperature serpentinite (M. Kasahara, 2003). We have thus started experimental studies on fault constitutive properties of serpentinite gouge, using a biaxial frictional testing machine at Kyoto University. Many conically-shaped serpentine seamounts are developed behind those subduction zones. They are consisted mainly of serpentinite mud with clasts of mantle rocks and high-pressure metamorphic rocks. Previous studies imply that the serpentinite is likely to have formed at depths around 30km. We have used serpentine mud, consisted mainly of chrysotile, in the drill core from South Chamorro Seamount (ODP Leg195). Double shear frictional experiments have been conducted on about 0.3 mm thick gouge at 30 MPa normal stress, at room temperature and under wet conditions (but without pore pressure). A series of velocity-step tests were performed in velocity range from 0.015 to 150 μm/s. Rate-and-state constitutive laws were fit to experimental data, by solving specimen-apparatus interaction numerically searching for the optimum constitutive parameters. Determination of stiffness of the apparatus is essential for accurate estimate of constitutive parameters. Careful measurements have revealed that the total stiffness (9.00×107 N/m) fluctuates by up to about 10 % probably owing to loose alignment of machine elements. This induces errors in constitutive parameters depending on dc}. If dc is in the order of 10 μm or larger, the error in b value is in the order of percent or less. But if the dc is around 1 μm, it becomes tens of percents or larger. The absolute value of frictional coefficient is around 0.2, very low and consistent with that of pure chrysotile (Moore et al., 1997). a- σb value is about 0.005 for velocity steps at 0.015-0.15 μm/s, decreases with increasing slip rate down to about -0.01 for the velocity steps at 15-150 μm/s. It changes from positive to

  6. Subducting seamounts control interplate coupling and seismic rupture in the 2014 Iquique earthquake area.

    PubMed

    Geersen, Jacob; Ranero, César R; Barckhausen, Udo; Reichert, Christian

    2015-01-01

    To date, the parameters that determine the rupture area of great subduction zone earthquakes remain contentious. On 1 April 2014, the Mw 8.1 Iquique earthquake ruptured a portion of the well-recognized northern Chile seismic gap but left large highly coupled areas un-ruptured. Marine seismic reflection and swath bathymetric data indicate that structural variations in the subducting Nazca Plate control regional-scale plate-coupling variations, and the limited extent of the 2014 earthquake. Several under-thrusting seamounts correlate to the southward and up-dip arrest of seismic rupture during the 2014 Iquique earthquake, thus supporting a causal link. By fracturing of the overriding plate, the subducting seamounts are likely further responsible for reduced plate-coupling in the shallow subduction zone and in a lowly coupled region around 20.5°S. Our data support that structural variations in the lower plate influence coupling and seismic rupture offshore Northern Chile, whereas the structure of the upper plate plays a minor role. PMID:26419949

  7. Subducting seamounts control interplate coupling and seismic rupture in the 2014 Iquique earthquake area

    PubMed Central

    Geersen, Jacob; Ranero, César R.; Barckhausen, Udo; Reichert, Christian

    2015-01-01

    To date, the parameters that determine the rupture area of great subduction zone earthquakes remain contentious. On 1 April 2014, the Mw 8.1 Iquique earthquake ruptured a portion of the well-recognized northern Chile seismic gap but left large highly coupled areas un-ruptured. Marine seismic reflection and swath bathymetric data indicate that structural variations in the subducting Nazca Plate control regional-scale plate-coupling variations, and the limited extent of the 2014 earthquake. Several under-thrusting seamounts correlate to the southward and up-dip arrest of seismic rupture during the 2014 Iquique earthquake, thus supporting a causal link. By fracturing of the overriding plate, the subducting seamounts are likely further responsible for reduced plate-coupling in the shallow subduction zone and in a lowly coupled region around 20.5°S. Our data support that structural variations in the lower plate influence coupling and seismic rupture offshore Northern Chile, whereas the structure of the upper plate plays a minor role. PMID:26419949

  8. Subducting seamounts control interplate coupling and seismic rupture in the 2014 Iquique earthquake area.

    PubMed

    Geersen, Jacob; Ranero, César R; Barckhausen, Udo; Reichert, Christian

    2015-09-30

    To date, the parameters that determine the rupture area of great subduction zone earthquakes remain contentious. On 1 April 2014, the Mw 8.1 Iquique earthquake ruptured a portion of the well-recognized northern Chile seismic gap but left large highly coupled areas un-ruptured. Marine seismic reflection and swath bathymetric data indicate that structural variations in the subducting Nazca Plate control regional-scale plate-coupling variations, and the limited extent of the 2014 earthquake. Several under-thrusting seamounts correlate to the southward and up-dip arrest of seismic rupture during the 2014 Iquique earthquake, thus supporting a causal link. By fracturing of the overriding plate, the subducting seamounts are likely further responsible for reduced plate-coupling in the shallow subduction zone and in a lowly coupled region around 20.5°S. Our data support that structural variations in the lower plate influence coupling and seismic rupture offshore Northern Chile, whereas the structure of the upper plate plays a minor role.

  9. Endemicity, biogeograhy, composition, and community structure on a northeast pacific seamount.

    PubMed

    McClain, Craig R; Lundsten, Lonny; Ream, Micki; Barry, James; DeVogelaere, Andrew

    2009-01-01

    The deep ocean greater than 1 km covers the majority of the earth's surface. Interspersed on the abyssal plains and continental slope are an estimated 14000 seamounts, topographic features extending 1000 m off the seafloor. A variety of hypotheses are posited that suggest the ecological, evolutionary, and oceanographic processes on seamounts differ from those governing the surrounding deep sea. The most prominent and oldest of these hypotheses, the seamount endemicity hypothesis (SMEH), states that seamounts possess a set of isolating mechanisms that produce highly endemic faunas. Here, we constructed a faunal inventory for Davidson Seamount, the first bathymetric feature to be characterized as a 'seamount', residing 120 km off the central California coast in approximately 3600 m of water (Fig 1). We find little support for the SMEH among megafauna of a Northeast Pacific seamount; instead, finding an assemblage of species that also occurs on adjacent continental margins. A large percentage of these species are also cosmopolitan with ranges extending over much of the Pacific Ocean Basin. Despite the similarity in composition between the seamount and non-seamount communities, we provide preliminary evidence that seamount communities may be structured differently and potentially serve as source of larvae for suboptimal, non-seamount habitats. PMID:19127302

  10. Endemicity, biogeograhy, composition, and community structure on a northeast pacific seamount.

    PubMed

    McClain, Craig R; Lundsten, Lonny; Ream, Micki; Barry, James; DeVogelaere, Andrew

    2009-01-01

    The deep ocean greater than 1 km covers the majority of the earth's surface. Interspersed on the abyssal plains and continental slope are an estimated 14000 seamounts, topographic features extending 1000 m off the seafloor. A variety of hypotheses are posited that suggest the ecological, evolutionary, and oceanographic processes on seamounts differ from those governing the surrounding deep sea. The most prominent and oldest of these hypotheses, the seamount endemicity hypothesis (SMEH), states that seamounts possess a set of isolating mechanisms that produce highly endemic faunas. Here, we constructed a faunal inventory for Davidson Seamount, the first bathymetric feature to be characterized as a 'seamount', residing 120 km off the central California coast in approximately 3600 m of water (Fig 1). We find little support for the SMEH among megafauna of a Northeast Pacific seamount; instead, finding an assemblage of species that also occurs on adjacent continental margins. A large percentage of these species are also cosmopolitan with ranges extending over much of the Pacific Ocean Basin. Despite the similarity in composition between the seamount and non-seamount communities, we provide preliminary evidence that seamount communities may be structured differently and potentially serve as source of larvae for suboptimal, non-seamount habitats.

  11. Diversity and endemism of the benthic seamount fauna in the southwest Pacific.

    PubMed

    de Forges, B R; Koslow, J A; Poore, G C

    2000-06-22

    Seamounts comprise a unique deep-sea environment, characterized by substantially enhanced currents and a fauna that is dominated by suspension feeders, such as corals. The potential importance of these steep-sided undersea mountains, which are generally of volcanic origin, to ocean biogeography and diversity was recognized over 40 years ago, but this environment has remained very poorly explored. A review of seamount biota and biogeography reported a total of 597 invertebrate species recorded from seamounts worldwide since the Challenger expedition of 1872. Most reports, based on a single taxonomic group, were extremely limited: 5 seamounts of the estimated more than 30,000 seamounts in the world's oceans accounted for 72% of the species recorded. Only 15% of the species occurring on seamounts were considered potential seamount endemics. Here we report the discovery of more than 850 macro- and megafaunal species from seamounts in the Tasman Sea and southeast Coral Sea, of which 29-34% are new to science and potential seamount endemics. Low species overlap between seamounts in different portions of the region indicates that the seamounts in clusters or along ridge systems function as 'island groups' or 'chains' leading to highly localized species distributions and apparent speciation between groups or ridge systems that is exceptional for the deep sea. These results have substantial implications for the conservation of this fauna, which is threatened by fishing activity.

  12. Diversity and endemism of the benthic seamount fauna in the southwest Pacific.

    PubMed

    de Forges, B R; Koslow, J A; Poore, G C

    2000-06-22

    Seamounts comprise a unique deep-sea environment, characterized by substantially enhanced currents and a fauna that is dominated by suspension feeders, such as corals. The potential importance of these steep-sided undersea mountains, which are generally of volcanic origin, to ocean biogeography and diversity was recognized over 40 years ago, but this environment has remained very poorly explored. A review of seamount biota and biogeography reported a total of 597 invertebrate species recorded from seamounts worldwide since the Challenger expedition of 1872. Most reports, based on a single taxonomic group, were extremely limited: 5 seamounts of the estimated more than 30,000 seamounts in the world's oceans accounted for 72% of the species recorded. Only 15% of the species occurring on seamounts were considered potential seamount endemics. Here we report the discovery of more than 850 macro- and megafaunal species from seamounts in the Tasman Sea and southeast Coral Sea, of which 29-34% are new to science and potential seamount endemics. Low species overlap between seamounts in different portions of the region indicates that the seamounts in clusters or along ridge systems function as 'island groups' or 'chains' leading to highly localized species distributions and apparent speciation between groups or ridge systems that is exceptional for the deep sea. These results have substantial implications for the conservation of this fauna, which is threatened by fishing activity. PMID:10879534

  13. Deep subsurface microbiology of 64-71 million year old inactive seamounts along the Louisville Seamount Chain

    NASA Astrophysics Data System (ADS)

    Sylvan, J. B.; Morono, Y.; Grim, S.; Inagaki, F.; Edwards, K. J.

    2013-12-01

    One of the objectives of IODP Expedition 330, Louisville Seamount Trail, was to sample and learn about the subsurface biosphere in the Louisville Seamount Chain (LSC). Seamounts are volcanic constructs that are ubiquitous along the seafloor - models suggest there are >100,000 seamounts of >1 km in height globally (Wessel et al., 2010). Therefore, knowledge about microbiology in the LSC subsurface can broadly be interpreted as representative of much the seafloor. In addition, despite the fact that the vast majority of the sea floor is comprised of crust >10 Ma, the majority of work to date has focused on young sites with active hydrology. Our presentation summarizes work focusing on subsurface microbiology from two different LSC seamounts: holes U1374A (65-71 Ma) and U1376A (64 Ma). We here present data for microbial biomass in the LSC subsurface using a method we developed to quantify microbial biomass in subseafloor ocean crust. We also present results from pyrotag analysis of 15 samples from holes U1374A and holes U1376A, representing several different lithologies from 40-491 meters below seafloor (mbsf) in hole U1374A and from 29-174 mbsf in hole U1376A. Finally, we present preliminary analysis of metagenomic sequencing from three of the samples from Hole U1376A. Biomass was low in the subsurface of both seamounts, ranging from below detection to ~104 cells cm-3. Bacteria comprised >99% of the prokaryotic community in LSC subsurface samples, therefore, bacterial diversity was assessed through 454 pyrosequencing of the V4V6 region of the 16S rRNA gene. Rarefaction analysis indicates that bacterial communities from the LSC subsurface are low diversity, on the order of a few hundred operational taxonomic units per sample. The phyla Actinobacteria, Bacteroidetes, Firmicutes and the classes α-, β- and γ-Proteobacteria are most abundant in the LSC subsurface. Within these, the orders Actinomycetales, Sphingobacteriales, Bacillales and Burkholderiales are the most

  14. Weak interplate coupling by seamounts and repeating M approximately 7 earthquakes.

    PubMed

    Mochizuki, Kimihiro; Yamada, Tomoaki; Shinohara, Masanao; Yamanaka, Yoshiko; Kanazawa, Toshihiko

    2008-08-29

    Subducting seamounts are thought to increase the normal stress between subducting and overriding plates. However, recent seismic surveys and laboratory experiments suggest that interplate coupling is weak. A seismic survey in the Japan Trench shows that a large seamount is being subducted near a region of repeating earthquakes of magnitude M approximately 7. Both observed seismicity and the pattern of rupture propagation during the 1982 M 7.0 event imply that interplate coupling was weak over the seamount. A large rupture area with small slip occurred in front of the seamount. Its northern bound could be determined by a trace of multiple subducted seamounts. Whereas a subducted seamount itself may not define the rupture area, its width may be influenced by that of the seamount. PMID:18755973

  15. Weak interplate coupling by seamounts and repeating M approximately 7 earthquakes.

    PubMed

    Mochizuki, Kimihiro; Yamada, Tomoaki; Shinohara, Masanao; Yamanaka, Yoshiko; Kanazawa, Toshihiko

    2008-08-29

    Subducting seamounts are thought to increase the normal stress between subducting and overriding plates. However, recent seismic surveys and laboratory experiments suggest that interplate coupling is weak. A seismic survey in the Japan Trench shows that a large seamount is being subducted near a region of repeating earthquakes of magnitude M approximately 7. Both observed seismicity and the pattern of rupture propagation during the 1982 M 7.0 event imply that interplate coupling was weak over the seamount. A large rupture area with small slip occurred in front of the seamount. Its northern bound could be determined by a trace of multiple subducted seamounts. Whereas a subducted seamount itself may not define the rupture area, its width may be influenced by that of the seamount.

  16. Double station observation of Draconid meteor outburst from two moving aircraft

    NASA Astrophysics Data System (ADS)

    Koten, Pavel; Vaubaillon, Jeremie; Margonis, Anastasios; Tóth, Juraj; Ďuriš, František; McAulliffe, Jonathan; Oberst, Jürgen

    2015-12-01

    A Draconid meteor shower outburst was observed from the boards of two scientific aircraft on 8 October 2011. In this paper we report the results of this double station experiment. The beginning and terminal heights are similar to other Draconid observations and confirm the fragile nature of the meteoroids. From the distribution function of terminal heights, a critical mass was found to be about 3.5 g. A behaviour of the terminal heights changes at this point. Light curves of Draconid meteors show great variability with a maximum of the F-number distribution around 0.35, which also confirms fragility of the material. Observed radiants of the meteors are in agreement with the theoretical model. Although encounters with two different filaments were predicted, it is impossible to distinguish between them from the radiants as well as the orbital data. Despite the complications with the data processing the airborne mission shows that such double station experiment is possible and provides valuable insight into meteor structure and dynamics.

  17. Meteor detection on ST (MST) radars

    NASA Technical Reports Server (NTRS)

    Avery, S. K.

    1987-01-01

    The ability to detect radar echoes from backscatter due to turbulent irregularities of the radio refractive index in the clear atmosphere has lead to an increasing number of established mesosphere - stratosphere - troposphere (MST or ST) radars. Humidity and temperature variations are responsible for the echo in the troposphere and stratosphere and turbulence acting on electron density gradients provides the echo in the mesosphere. The MST radar and its smaller version, the ST radar, are pulsed Doppler radars operating in the VHF - UHF frequency range. These echoes can be used to determine upper atmosphere winds at little extra cost to the ST radar configuration. In addition, the meteor echoes can supplement mesospheric data from an MST radar. The detection techniques required on the ST radar for delineating meteor echo returns are described.

  18. The cometary and asteroidal origins of meteors

    NASA Technical Reports Server (NTRS)

    Kresak, L.

    1973-01-01

    A quantitative examination of the gravitational and nongravitational changes of orbits shows that for larger interplanetary bodies the perturbations by Jupiter strongly predominate over all other effects, which include perturbations by other planets, splitting of comet nuclei and jet effects of cometary ejections. The structure of meteor streams, indicates that the mutual compensation of the changes in individual elements entering the Jacobian integral, which is characteristic for the comets, does not work among the meteoroids. It appears that additional forces of a different kind must exert appreciable influence on the motion of interplanetary particles of meteoroid size. Nevertheless, the distribution of the Jacobian constant in various samples of meteor orbits furnishes some information on the type of their parent bodies and on the relative contribution of individual sources.

  19. The Swedish Allsky Meteor Network: first results

    NASA Astrophysics Data System (ADS)

    Stempels, E.; Kero, E.

    2016-01-01

    The Swedish Allsky Meteor Network started operations with two cameras in early 2014 and has since grown steadily. Currently, seven stations are active and several more will come online in the near future. The network to a large degree relies on low-cost stations run by private individuals or small societies of amateur astronomers. Originally based on the Danish meteor network Stjerneskud, the central node of Uppsala University provides the network with the necessary infrastructure, such as a continually updated software distribution and automatic processing of data from all stations. Although covering a very large land mass with relatively low resources is challenging, there have up to now been several well-observed events, often in collaboration with observations from neighboring countries. We give a short overview of the network's current status, chosen technical solutions, and some results.

  20. Data processing of records of meteoric echoes

    NASA Astrophysics Data System (ADS)

    Dolinský, P.

    2016-01-01

    The data obtained in the period from 4 November 2014 to 31 July 2014 by our receiving and recording system was statistically processed. The system records meteoric echoes from the TV transmitter Lviv 49.739583 MHz (N49.8480° E24.0369°, Ukraine) using a 4-element Yagi antenna with horizontal polarization (elevation of 0° and azimuth of 60°), receiver ICOM R-75 in the CW mode, and a computer with a recording using HROFFT v1.0.0f. The main goal was to identify weak showers in these data. Mayor or strong showers are visible without processing (referred at IMC2015, Mistelbach). To find or to identify weaker showers is more difficult. Not all echoes are meteoric echoes, but also ionospheric echoes or lightning disturbances are present.

  1. The World's Most Famous Meteor Shower Picture

    NASA Astrophysics Data System (ADS)

    Hughes, David W.

    1995-01-01

    The world's most famous meteor shower picture (Fig. 1) is of the storm that took place in the early morning of Wednesday, 13 November 1833. The picture was, however, produce 54 years after the event, being first published in April 1888. It had a biblical origin and was only taken over by the astronomers in the mid 1920s. The artist was the Swiss painter Karl Jauslin and the engraver was Adolf Völlmy.

  2. Elementary process and meteor train spectra

    NASA Technical Reports Server (NTRS)

    Ovezgeldyev, O. G.

    1987-01-01

    Mechanisms of excitation of individual spectral line radiation were studied experimentally and theoretically and it was demonstrated that such processes as oxidation, resonant charge exchange, dissociative recombination and others play an important part in the chemistry of excited particles. The foundation was laid toward simulating the elementary processes of meteor physics. Having a number of advantages and possibilities, this method is sure to find a wide use in the future.

  3. A global atmospheric model of meteoric iron

    NASA Astrophysics Data System (ADS)

    Feng, Wuhu; Marsh, Daniel R.; Chipperfield, Martyn P.; Janches, Diego; Höffner, Josef; Yi, Fan; Plane, John M. C.

    2013-08-01

    The first global model of meteoric iron in the atmosphere (WACCM-Fe) has been developed by combining three components: the Whole Atmosphere Community Climate Model (WACCM), a description of the neutral and ion-molecule chemistry of iron in the mesosphere and lower thermosphere (MLT), and a treatment of the injection of meteoric constituents into the atmosphere. The iron chemistry treats seven neutral and four ionized iron containing species with 30 neutral and ion-molecule reactions. The meteoric input function (MIF), which describes the injection of Fe as a function of height, latitude, and day, is precalculated from an astronomical model coupled to a chemical meteoric ablation model (CABMOD). This newly developed WACCM-Fe model has been evaluated against a number of available ground-based lidar observations and performs well in simulating the mesospheric atomic Fe layer. The model reproduces the strong positive correlation of temperature and Fe density around the Fe layer peak and the large anticorrelation around 100 km. The diurnal tide has a significant effect in the middle of the layer, and the model also captures well the observed seasonal variations. However, the model overestimates the peak Fe+concentration compared with the limited rocket-borne mass spectrometer data available, although good agreement on the ion layer underside can be obtained by adjusting the rate coefficients for dissociative recombination of Fe-molecular ions with electrons. Sensitivity experiments with the same chemistry in a 1-D model are used to highlight significant remaining uncertainties in reaction rate coefficients, and to explore the dependence of the total Fe abundance on the MIF and rate of vertical transport.

  4. SPA Meteor Section results: September - October, 1995.

    NASA Astrophysics Data System (ADS)

    McBeath, A.

    1996-04-01

    A compilation of visual, photographic and radio results submitted to the SPA Meteor Section from September and October is given. Although September was not an especially good month for observers, October brought a quite well-viewed Orionid return, enabling some magnitude and train details to be derived for the shower, and another brilliant fireball occurred at 2h28mUT on October 31.

  5. Structural peculiarities of the Quadrantid meteor shower

    NASA Technical Reports Server (NTRS)

    Isamutdinov, Sh. O.; Chebotarev, R. P.

    1987-01-01

    Systematic radio observations to investigate the Quadrantid meteor shower structure are regularly carried out. They have now been conducted annually in the period of its maximum activity, January 1 to 6, since 1966. The latest results of these investigations are presented, on the basis of 1981 to 1984 data obtained using new equipment with a limiting sensitivity of +7.7 sup m which make it possible to draw some conclusions on the Quadrantids shower structure both for transverse and lengthwise directions.

  6. A Global Atmospheric Model of Meteoric Iron

    NASA Technical Reports Server (NTRS)

    Feng, Wuhu; Marsh, Daniel R.; Chipperfield, Martyn P.; Janches, Diego; Hoffner, Josef; Yi, Fan; Plane, John M. C.

    2013-01-01

    The first global model of meteoric iron in the atmosphere (WACCM-Fe) has been developed by combining three components: the Whole Atmosphere Community Climate Model (WACCM), a description of the neutral and ion-molecule chemistry of iron in the mesosphere and lower thermosphere (MLT), and a treatment of the injection of meteoric constituents into the atmosphere. The iron chemistry treats seven neutral and four ionized iron containing species with 30 neutral and ion-molecule reactions. The meteoric input function (MIF), which describes the injection of Fe as a function of height, latitude, and day, is precalculated from an astronomical model coupled to a chemical meteoric ablation model (CABMOD). This newly developed WACCM-Fe model has been evaluated against a number of available ground-based lidar observations and performs well in simulating the mesospheric atomic Fe layer. The model reproduces the strong positive correlation of temperature and Fe density around the Fe layer peak and the large anticorrelation around 100 km. The diurnal tide has a significant effect in the middle of the layer, and the model also captures well the observed seasonal variations. However, the model overestimates the peak Fe+ concentration compared with the limited rocket-borne mass spectrometer data available, although good agreement on the ion layer underside can be obtained by adjusting the rate coefficients for dissociative recombination of Fe-molecular ions with electrons. Sensitivity experiments with the same chemistry in a 1-D model are used to highlight significant remaining uncertainties in reaction rate coefficients, and to explore the dependence of the total Fe abundance on the MIF and rate of vertical transport.

  7. Impact mechanics at Meteor Crater, Arizona

    USGS Publications Warehouse

    Shoemaker, Eugene Merle

    1959-01-01

    Meteor Crator is a bowl-shaped depression encompassed by a rim composed chiefly of debris stacked in layers of different composition. Original bedrock stratigraphy is preserved, inverted, in the debris. The debris rests on older disturbed strata, which are turned up at moderate to steep angles in the wall of the crater and are locally overturned near the contact with the debris. These features of Meteor Crater correspond closely to those of a crater produced by nuclear explosion where depth of burial of the device was about 1/5 the diameter of the resultant crater. Studies of craters formed by detonation of nuclear devices show that structures of the crater rims are sensitive to the depth of explosion scaled to the yield of the device. The structure of Meteor Crater is such as would be produced by a very strong shock originating about at the level of the present crater floor, 400 feet below the original surface. At supersonic to hypersonic velocity an impacting meteorite penetrates the ground by a complex mechanism that includes compression of the target rocks and the meteorite by shock as well as hydrodynamic flow of the compressed material under high pressure and temperature. The depth of penetration of the meteorite, before it loses its integrity as a single body, is a function primarily of the velocity and shape of the meteorite and the densities and equations of state of the meteorite and target. The intensely compressed material then becomes dispersed in a large volume of breccia formed in the expanding shock wave. An impact velocity of about 15 km/sec is consonant with the geology of Meteor Crater in light of the experimental equation of state of iron and inferred compressibility of the target rocks. The kinetic energy of the meteorite is estimated by scaling to have been from 1.4 to 1.7 megatons TNT equivalent.

  8. Radar and Meteors: Controversy over the Origin of Meteors in Postwar Astronomy

    NASA Astrophysics Data System (ADS)

    Sullivan, Woodruff T., III

    2006-12-01

    After World War II radio physicists and engineers discovered that radar reflections were readily obtained off the ionized trails left by meteors. The group led by Bernard Lovell at the Jodrell Bank Experimental Station of Manchester University, England, led the effort to design radar transmitters, receivers, and antenna systems that could better understand these reflections. First, an entire suite of daytime meteor showers was found to accompany the familiar nighttime showers. Next, associating with meteor astronomers such as Fred Whipple, Ernst Öpik, and Cuno Hoffmeister, Lovell found that his radar data could contribute to a longstanding controversy in the field: was there any portion of the meteors whose speeds indicated that they were on hyperbolic orbits and therefore of interstellar origin (i.e., >72 km/s), or did all meteoroids originate within the solar system? By 1953 the Jodrell Bank radar astronomers’ huge samples of echoes and measured speeds of meteors indicated that there were in fact no interstellar interlopers. This settled the question for most workers in the field, although Opik and Hoffmeister did not give in.

  9. Long-Period Meteor Streams and the Dispersion of Semimajor Axes of Meteor Orbits

    NASA Astrophysics Data System (ADS)

    Hajduková, Mária, Jr.

    2013-06-01

    The present work is based on an analysis of a large statistical sample of meteor orbits collected in the Japanese shower catalogue (SonotaCo 2009, WGN, 37, 55) of 114280 video observed meteors. The shower meteor data were selected and analysed with the aim of determining the orbits' distribution in major meteor streams with heliocentric velocities close to the parabolic limit, in which the errors in the velocity determination correspond to large differences in the reciprocal semimajor axis, 1/a. The contribution of the real dispersion of the semimajor axes, a, can be deduced from the high proportion of hyperbolic orbits in the analysed streams, where an excess over the parabolic value can be regarded as being entirely due to measurement errors. The orbital dispersion described by the median absolute deviation in terms of 1/a was found to be ±0.083 AU-1 for the Leonids and ±0.080 AU-1 for the Orionids, and slightly smaller for the Perseid and Lyrid meteor streams (±0.055 and ±0.047 AU-1). The proximity of the parabolic limit caused a strong influence of observational effects; however, a significant contribution of the real dispersion is involved.

  10. An FDTD model of scattering from meteor head plasma

    NASA Astrophysics Data System (ADS)

    Marshall, R. A.; Close, S.

    2015-07-01

    We have developed a three-dimensional finite difference time domain (FDTD) model of scattering of radar waves from meteor head plasma. The model treats the meteor head plasma as a cold, collisional, and magnetized plasma, and solves Maxwell's equations and the Langevin equation simultaneously and self-consistently in and around the plasma. We use this model to investigate scattering of radar waves from a meteor head (the "head echo") under a range of plasma densities, meteor scale sizes, and wave frequencies. In this way we relate the radar cross section (RCS) to these variable parameters. We find that computed RCS disagrees with previous analytical theory at certain meteor sizes and densities, in some cases by over an order of magnitude. We find that the calculated meteor head RCS is monotonically related to the "overdense area" of the meteor, defined as the cross-section area of the part of the meteor where the plasma frequency exceeds the wave frequency. These results provides a physical measure of the meteor size and density that can be inferred from measured RCS values from ground-based radars. Meteoroid mass can then be inferred from the meteor plasma distribution using established methods.

  11. Great Minds? Great Lakes!

    ERIC Educational Resources Information Center

    Environmental Protection Agency, Chicago, IL. Great Lakes National Program Office.

    This booklet introduces an environmental curriculum for use in a variety of elementary subjects. The lesson plans provide an integrated approach to incorporating Great Lakes environmental issues into the subjects of history, social studies, and environmental sciences. Each of these sections contains background information, discussion points, and a…

  12. Photometric stellar catalogue for TV meteor astronomy

    NASA Astrophysics Data System (ADS)

    Leonov, V. A.; Bagrov, A. V.

    2016-01-01

    Photometry for ordinary astrophysics was carefully developed for its own purposes. As stars radiation is very similar to the blackbody radiation, astronomers measure star illumination in wide or narrow calibrated spectral bands. This is enough for star photometry with precise accuracy and for measuring their light flux in these bands in energetic units. Meteors are moving objects and do not allow collection of more photons then they emit. So meteor observers use the whole spectral band that can be covered by sensitivity of their light sensors. This is why measurements of stellar magnitudes of background stars by these sensors are not the same as catalogued star brightness in standard photometric spectral bands. Here we present a special photometric catalogue of 93 bright non-variable stars of the northern hemisphere, that can be used by meteor observers of standard background whose brightness are calculated in energetic units as well as in non-systematic stellar magnitudes in spectral wavelength of the WATEC 902 sensitivity.

  13. Comet outbursts and the meteor showers

    NASA Astrophysics Data System (ADS)

    Guliyev, A. S.; Kokhirova, G. I.; Poladova, U. D.

    2014-07-01

    The features of 116 comets that have shown an outbursts in their brightness, are considered in the paper. The hypothesis on that the outburst in activity of comets are caused by their passing through meteoroid streams is studied. For this purpose the orbital elements of such comets relative to the planes of motion of 68 meteor showers from Cook's catalogue are analyzed. It was found that four of the nearest and distant nodes of comet orbits relative to the planes of motion of nine meteor showers exceeds the average statistical background with confidence probability from 0.90 to 0.95, and more than 0.95, respectively. The October Draconids, Aurigids, kappa-Serpentids, delta-Draconids, sigma-Hydrids}, Coma Berenicids, Leonids, Leo Minorids, and Perseids showers are the most effective. The results of calculation show that often, the comets outbursts may be caused by collisions of comets with meteoroids under the passing through the meteoroid streams that are producing listed meteor showers as well as solar activity.

  14. Quantifying the direct use value of Condor seamount

    NASA Astrophysics Data System (ADS)

    Ressurreição, Adriana; Giacomello, Eva

    2013-12-01

    Seamounts often satisfy numerous uses and interests. Multiple uses can generate multiple benefits but also conflicts and impacts, calling, therefore, for integrated and sustainable management. To assist in developing comprehensive management strategies, policymakers recognise the need to include measures of socioeconomic analysis alongside ecological data so that practical compromises can be made. This study assessed the direct output impact (DOI) of the relevant marine activities operating at Condor seamount (Azores, central northeast Atlantic) as proxies of the direct use values provided by the resource system. Results demonstrated that Condor seamount supported a wide range of uses yielding distinct economic outputs. Demersal fisheries, scientific research and shark diving were the top-three activities generating the highest revenues, while tuna fisheries, whale watching and scuba-diving had marginal economic significance. Results also indicated that the economic importance of non-extractive uses of Condor is considerable, highlighting the importance of these uses as alternative income-generating opportunities for local communities. It is hoped that quantifying the direct use values provided by Condor seamount will contribute to the decision making process towards its long-term conservation and sustainable use.

  15. Condor seamount (Azores, NE Atlantic): A morpho-tectonic interpretation

    NASA Astrophysics Data System (ADS)

    Tempera, Fernando; Hipólito, Ana; Madeira, José; Vieira, Sara; Campos, Aldino S.; Mitchell, Neil C.

    2013-12-01

    High-resolution datasets collected by multibeam and acoustic backscatter surveys were used to produce fine-scale seafloor nature and morpho-tectonic interpretations of the Condor seamount. Condor constitutes an elongated volcanic ridge that extends for 39 km and rises more than 1800 m from the surrounding seafloor. Constructive morphologies include (i) linear eruptive centres, (ii) volcanic cones with or without summit depressions, (iii) lava flows and (iv) hummocky sectors. Eruptive type is interpreted to vary with depth. On the deeper seamount extremities, the predominance of highly acoustically backscattering volcanic cones and hummocky terrain is interpreted to result from effusive eruptions not yet covered by sediment deposits. In contrast, the smoother relief of the central seamount flanks is interpreted as draping and infilling of the underlying effusive relief by (i) primary volcaniclastic deposits produced by explosive eruptions on the shallowest parts of the ridge, together with (ii) secondary volcanigenic sediments resulting from truncation of the seamount top by swell erosion and (iii) sediments resulting from biogenic production.

  16. Erratic Continental Rocks on Volcanic Seamounts off California and Oregon

    NASA Astrophysics Data System (ADS)

    Paduan, J. B.; Clague, D. A.; Davis, A. S.

    2006-12-01

    The seamounts off the California continental margin, and those well offshore of California and Oregon that formed near mid-ocean ridges, are all constructed of basaltic lava flows and volcanic breccias and sandstones. However, explorations of these seamounts using dredges, and more recently, the remotely operated vehicle Tiburon, frequently recover rocks of a wide assortment of continental lithologies including gabbro, granodiorite, silicic volcanics, limestone, dolomite, and metamorphic rocks. These rocks are often rounded like river and beach cobbles, and the softer rocks are bored as by worms or bivalves. They are covered with manganese oxide crusts of thicknesses that range from a patina to several cm, approaching the thickness on the in-situ basaltic rocks. These rocks are often easier to collect than the basalts. We recognize these rocks to be erratics of continental origin. Erratics have been documented as being transported by icebergs at higher latitudes, but this mechanism is unlikely to be responsible for the erratics we have found as far south as 31.9° N. Three brief papers published by K.O. Emery from 1941 to 1954 proposed that such erratics found in many thick sections of fine-grained sedimentary sequences such as the Monterey Formation, were transported long distances by kelp holdfasts, tree roots, or in the guts of pinnipeds. We propose that these vectors also transport erratics to seamounts, where they have been accumulating since the seamounts formed millions of years ago. Those seamounts that were once islands would have intercepted even more erratics along their shorelines while they stood above sea level. We have recovered or observed such erratics on the Vance Seamounts; Gumdrop, Pioneer, Guide, Davidson, Rodriguez, San Juan, Little Joe, and San Marcos Seamounts; on the muddy bottom of Monterey Bay; and on Northeast Bank and along the Patton Escarpment at the western edge of the California Borderland. These locations are as far as 250 nautical

  17. Analysis of Historical Meteor and Meteor shower Records: Korea, China and Japan

    NASA Astrophysics Data System (ADS)

    Yang, Hong-Jin; Park, Changbom; Park, Myeong-Gu

    2015-03-01

    We have compiled and analyzed historical meter and meteor shower records in Korean, Chinese, and Japanese chronicles. We have confirmed the peaks of Perseids and an excess due to the mixture of Orionids, north-Taurids, or Leonids through the Monte-Carlo test from the Korean records. The peaks persist for almost one thousand years. We have also analyzed seasonal variation of sporadic meteors from Korean records. Major features in Chinese meteor shower records are quite consistent with those of Korean records, particularly for the last millennium. Japanese records also show Perseids feature and Orionids/north-Taurids/Leonids feature, although they are less prominent compared to those of Korean or Chinese records.

  18. Meteor radar signal processing and error analysis

    NASA Astrophysics Data System (ADS)

    Kang, Chunmei

    Meteor wind radar systems are a powerful tool for study of the horizontal wind field in the mesosphere and lower thermosphere (MLT). While such systems have been operated for many years, virtually no literature has focused on radar system error analysis. The instrumental error may prevent scientists from getting correct conclusions on geophysical variability. The radar system instrumental error comes from different sources, including hardware, software, algorithms and etc. Radar signal processing plays an important role in radar system and advanced signal processing algorithms may dramatically reduce the radar system errors. In this dissertation, radar system error propagation is analyzed and several advanced signal processing algorithms are proposed to optimize the performance of radar system without increasing the instrument costs. The first part of this dissertation is the development of a time-frequency waveform detector, which is invariant to noise level and stable to a wide range of decay rates. This detector is proposed to discriminate the underdense meteor echoes from the background white Gaussian noise. The performance of this detector is examined using Monte Carlo simulations. The resulting probability of detection is shown to outperform the often used power and energy detectors for the same probability of false alarm. Secondly, estimators to determine the Doppler shift, the decay rate and direction of arrival (DOA) of meteors are proposed and evaluated. The performance of these estimators is compared with the analytically derived Cramer-Rao bound (CRB). The results show that the fast maximum likelihood (FML) estimator for determination of the Doppler shift and decay rate and the spatial spectral method for determination of the DOAs perform best among the estimators commonly used on other radar systems. For most cases, the mean square error (MSE) of the estimator meets the CRB above a 10dB SNR. Thus meteor echoes with an estimated SNR below 10dB are

  19. Interferometric meteor head echo observations using the Southern Argentina Agile Meteor Radar

    NASA Astrophysics Data System (ADS)

    Janches, D.; Hocking, W.; Pifko, S.; Hormaechea, J. L.; Fritts, D. C.; Brunini, C.; Michell, R.; Samara, M.

    2014-03-01

    A radar meteor echo is the radar scattering signature from the free electrons generated by the entry of extraterrestrial particles into the atmosphere. Three categories of scattering mechanisms exist: specular, nonspecular trails, and head echoes. Generally, there are two types of radars utilized to detect meteors. Traditional VHF all-sky meteor radars primarily detect the specular trails, while high-power, large-aperture (HPLA) radars efficiently detect meteor head echoes and, in some cases, nonspecular trails. The fact that head echo measurements can be performed only with HPLA radars limits these studies in several ways. HPLA radars are sensitive instruments constraining the studies to the lower masses, and these observations cannot be performed continuously because they take place at national observatories with limited allocated observing time. These drawbacks can be addressed by developing head echo observing techniques with modified all-sky meteor radars. Such systems would also permit simultaneous detection of all different scattering mechanisms using the same instrument, rather than requiring assorted different classes of radars, which can help clarify observed differences between the different methodologies. In this study, we demonstrate that such concurrent observations are now possible, enabled by the enhanced design of the Southern Argentina Agile Meteor Radar (SAAMER). The results presented here are derived from observations performed over a period of 12 days in August 2011 and include meteoroid dynamical parameter distributions, radiants, and estimated masses. Overall, the SAAMER's head echo detections appear to be produced by larger particles than those which have been studied thus far using this technique.

  20. Caldera collapse at near-ridge seamounts: an experimental investigation

    NASA Astrophysics Data System (ADS)

    Coumans, Jason P.; Stix, John

    2016-10-01

    Collapse calderas are sub-circular volcanic depressions caused by subsidence of the magma reservoir roof during an eruption. Scaled physical models of caldera collapse using flat topography have been instrumental in investigating the spatial and temporal development of calderas, in particular, two distinctive sets of concentric ring faults, one reverse and one normal. More recent analog studies have investigated the effect of non-flat topography which alters the principle stress trajectories and resulting collapse structure. This work provides the basis for investigating how naturally scaled topographic loads may affect caldera collapse in relation to shallow magma reservoirs. The objective of this study is to understand how a near-ridge seamount affects caldera collapse from both a central and offset position as the seamount migrates above the magma reservoir as a result of plate motion. We utilize scaled analog models of caldera collapse in conjunction with three-dimensional (3D) laser scanning and digital particle image velocimetry (DPIV) to investigate caldera collapse dynamics at near-ridge seamounts. Experiments using a seamount cone positioned centrally above the magma reservoir result in (1) increased subsidence along the interior outward-dipping faults and (2) a preference to more symmetric collapse patterns as indicated by the subsidence profile and structure of the caldera relative to experiments with an offset cone. When the cone is offset, the collapse is asymmetric and trapdoor in nature, with the center of greatest subsidence displaced away from the region of largest topographic load. For these latter experiments, subsidence is focused where the roof is thinnest along an initial reverse fault, followed by a transition to an antithetic graben structure. The asymmetric collapse in the experiments results in a caldera with a tilted profile. Offset calderas at near-ridge seamounts are tilted towards the ridge axis, suggesting that they may have collapsed

  1. Mapping AUV Survey of Axial Seamount

    NASA Astrophysics Data System (ADS)

    Thomas, H.; Caress, D.; Conlin, D.; Clague, D.; Paduan, J.; Butterfield, D.; Chadwick, W.; Tucker, P.

    2006-12-01

    In late August and early September 2006, the MBARI Mapping Autonomous Underwater Vehicle (AUV) was deployed for 5 missions on Axial Seamount during a NOAA NeMO cruise on the R/V Thompson. The objective of the survey was to determine the geologic history of the summit of Axial Seamount using high resolution multibeam, sidescan, and sub-bottom profiler data. The Mapping AUV is a torpedo-shaped, 6000 m rated vehicle designed and constructed by MBARI. The vehicle is equipped with a 200 kHz multibeam sonar, 110 kHz and 410 kHz chirp sidescan sonar, and a 2-16 kHz sweep chirp sub-bottom profiler. The multibeam provides a 120-degree swath with 0.94 degree by 0.94 degree beam resolution. The endurance of the AUV is eight hours at 3 knots. Navigation derives from an inertial navigation system (INS) incorporating a ring laser gyro aided by GPS at the surface and by velocity-over- ground observations from a Doppler velocity log (DVL) when within 130 m of the seafloor. A navigational precision of 0.05 percent of distance traveled is achieved with continuous DVL bottom lock. An acoustic modem allows surface aiding of navigation during deep descents. The AUV ran two types of missions: those on the rim of the caldera were run at 90 m altitude with a line spacing of 250 m and those on the caldera floor were run at 50 m altitude with a line spacing of 150 or 175 m. The surveys covered most of 1998 lava flow on the south rim of the caldera and northern part of the south rift zone, the southern region of the caldera floor where hydrothermal vents are common, the northeast rim of the caldera where volcaniclastic deposits related to caldera collapse drape the surface, the north rift zone, and the northern portion of the caldera floor. The low-altitude maps have a resolution of 1 m, so large individual lava pillars and hydrothermal chimneys can be seen, fissures stand out clearly, and the regions of collapsed lobate flows and lava channels are prominent. Many of the flows, including the

  2. Meteoric water in metamorphic core complexes

    NASA Astrophysics Data System (ADS)

    Teyssier, Christian; Mulch, Andreas

    2015-04-01

    The trace of surface water has been found in all detachment shear zones that bound the Cordilleran metamorphic core complexes of North America. DeltaD values of mica fish in detachment mylonites demonstrate that these synkinematic minerals grew in the presence of meteoric water. Typically deltaD values are very negative (-120 to -160 per mil) corresponding to deltaD values of water that are < -100 per mil given the temperature of water-mica isotopic equilibration (300-500C). From British Columbia (Canada) to Nevada (USA) detachment systems bound a series of core complexes: the Thor-Odin, Valhalla, Kettle-Okanogan, Bitterroot -Anaconda, Pioneer, Raft River, Ruby Mountain, and Snake Range. The bounding shear zones range in thickness from ~100 m to ~1 km, and within the shear zones, meteoric water signature is recognized over 10s to 100s of meters beneath the detachment fault. The age of shearing ranges generally from Eocene in the N (~50-45 Ma) to Oligo-Miocene in the S (25-15 Ma). DeltaD water values derived from mica fish in shear zones are consistent with supradetachment basin records of the same age brackets and can be used for paleoaltimetry if coeval isotopic records from near sea level are available. Results show that a wave of topography (typically 4000-5000 m) developed from N to S along the Cordillera belt from Eocene to Miocene, accompanied by the propagation of extensional deformation and volcanic activity. In addition, each detachment system informs a particular extensional detachment process. For example, the thick Thor-Odin detachment shear zone provides sufficient age resolution to indicate the downward propagation of shearing and the progressive incorporation of footwall rocks into the hanging wall. The Kettle detachment provides a clear illustration of the dependence of fluid circulation on dynamic recrystallization processes. The Raft River system consists of a thick Eocene shear zone that was overprinted by Miocene shearing; channels of meteoric

  3. Diversity, ecological distribution and biotechnological potential of Actinobacteria inhabiting seamounts and non-seamounts in the Tyrrhenian Sea.

    PubMed

    Ettoumi, Besma; Chouchane, Habib; Guesmi, Amel; Mahjoubi, Mouna; Brusetti, Lorenzo; Neifar, Mohamed; Borin, Sara; Daffonchio, Daniele; Cherif, Ameur

    2016-01-01

    In the present study, the ecological distribution of marine Actinobacteria isolated from seamount and non-seamount stations in the Tyrrhenian Sea was investigated. A collection of 110 isolates was analyzed by Automated Ribosomal Intergenic Spacer Analysis (ARISA) and 16S rRNA gene sequencing of representatives for each ARISA haplotype (n=49). Phylogenetic analysis of 16S rRNA sequences showed a wide diversity of marine isolates and clustered the strains into 11 different genera, Janibacter, Rhodococcus, Arthrobacter, Kocuria, Dietzia, Curtobacterium, Micrococcus, Citricoccus, Brevibacterium, Brachybacterium and Nocardioides. Interestingly, Janibacter limosus was the most encountered species particularly in seamounts stations, suggesting that it represents an endemic species of this particular ecosystem. The application of BOX-PCR fingerprinting on J. limosus sub-collection (n=22), allowed their separation into seven distinct BOX-genotypes suggesting a high intraspecific microdiversity among the collection. Furthermore, by screening the biotechnological potential of selected actinobacterial strains, J. limosus was shown to exhibit the most important biosurfactant activity. Our overall data indicates that Janibacter is a major and active component of seamounts in the Tyrrhenian Sea adapted to low nutrient ecological niche. PMID:27242145

  4. Diversity, ecological distribution and biotechnological potential of Actinobacteria inhabiting seamounts and non-seamounts in the Tyrrhenian Sea.

    PubMed

    Ettoumi, Besma; Chouchane, Habib; Guesmi, Amel; Mahjoubi, Mouna; Brusetti, Lorenzo; Neifar, Mohamed; Borin, Sara; Daffonchio, Daniele; Cherif, Ameur

    2016-01-01

    In the present study, the ecological distribution of marine Actinobacteria isolated from seamount and non-seamount stations in the Tyrrhenian Sea was investigated. A collection of 110 isolates was analyzed by Automated Ribosomal Intergenic Spacer Analysis (ARISA) and 16S rRNA gene sequencing of representatives for each ARISA haplotype (n=49). Phylogenetic analysis of 16S rRNA sequences showed a wide diversity of marine isolates and clustered the strains into 11 different genera, Janibacter, Rhodococcus, Arthrobacter, Kocuria, Dietzia, Curtobacterium, Micrococcus, Citricoccus, Brevibacterium, Brachybacterium and Nocardioides. Interestingly, Janibacter limosus was the most encountered species particularly in seamounts stations, suggesting that it represents an endemic species of this particular ecosystem. The application of BOX-PCR fingerprinting on J. limosus sub-collection (n=22), allowed their separation into seven distinct BOX-genotypes suggesting a high intraspecific microdiversity among the collection. Furthermore, by screening the biotechnological potential of selected actinobacterial strains, J. limosus was shown to exhibit the most important biosurfactant activity. Our overall data indicates that Janibacter is a major and active component of seamounts in the Tyrrhenian Sea adapted to low nutrient ecological niche.

  5. Dynamics of intrathermocline vortices in a gyre flow over a seamount chain

    NASA Astrophysics Data System (ADS)

    Sokolovskiy, Mikhail A.; Filyushkin, Boris N.; Carton, Xavier J.

    2013-07-01

    The interaction of meddies with a complex distribution of seamounts is studied in a three-layer quasi-geostrophic model on the f-plane. This study aims at understanding if and how this seamount chain can represent a barrier to the propagation of these eddies and how it can be involved in their decay. The eddies are idealized as vortex patches in the middle layer, interacting with a regional cyclonic current and with ten idealized seamounts. The numerical code is based on the contour surgery technique. The initial position, radius, shape, number and polarity of the eddies are varied. The main results are the following: (1) Though they do not describe the unsteady flow, the streamlines of the regional and topographic flow provide a useful estimate of the vortex trajectories, in particular towards the major seamounts, where stronger velocity shears are expected. (2) The tallest and widest seamounts which have the largest vorticity reservoir are able to considerably erode the vortices, but also to draw anticyclones towards the seamount top. The ability of narrower seamounts to erode vortices is related to their multiplicity. (3) Only 1/3 of the anticyclones with about 30-km radius reach the southern boundary of the seamount chain, and their erosion is larger than 50 %. The other anticyclones are either completely eroded or trapped over a wide seamount top. Cyclones are less affected by seamounts because they oppose the topographic draft towards the seamount top and they drift along the side of the seamount. (4) Large vortices resist topographic erosion more efficiently. The rate of erosion grows from a few percent to about 35-50 % as the vortex radius decreases from about 60 to 30 km. Small cyclones are not eroded, contrary to small anticyclones (which completely decay), in relation with the different trajectories of these eddies in the vicinity of the seamounts. (5) The detailed vortex shape does not appear critical for their evolution, if they are close enough to the

  6. Age and Geochemical Data From the Madeira-Tore Rise and Surrounding Seamounts: New Insights Into East Atlantic Volcanism

    NASA Astrophysics Data System (ADS)

    Geldmacher, J.; Hoernle, K. A.; Kluegel, A.; van den Bogaard, P.

    2003-12-01

    Located off the NW African continental margin is a >3000 km long belt of volcanic archipelagoes (e.g. Canary, Madeira Islands) and large seamounts including the 900 km long Madeira-Tore Rise (MTR). The cause of the East Atlantic volcanism, and in particular the origin and age of the MTR, which is composed of a widespread plateau with several seamount groups, is controversial. Proposed models include an origin of the MTR at the Mid Atlantic Ridge, formation over a hotspot, or as a product of diffuse small-scale mantle convection. All recently dredged volcanic samples (RV Meteor cruise M51/1) from the MTR and nearby off-rise seamounts exhibit enriched Ocean Island Basalt-like incompatible trace element signatures similar to HIMU (high time integrated 238U/204Pb) ocean islands. Their isotope compositions are similar to those from Madeira with 87Sr/86Sr and 143Nd/144Nd overlapping Atlantic N-MORB to a large extent, but Pb isotope ratios plotting well below the Northern Hemisphere Reference Line and extending to 206Pb/204Pb values of 19.90. Our preliminary data confirm the existence of at least two distinct isotopic domains in the eastern North Atlantic: 1) a Madeira-like domain (as characterized above) stretching from Madeira Island along the MTR to the NE as far as the Azores Gibraltar fracture zone, and 2) a Canary-like domain with Sr, Nd, Pb isotope ratios intermediate between N-MORB and HIMU (206Pb/204Pb = 19.0-20.2; 207Pb/204Pb = 15.54-15.66) but with lower 143Nd/144Nd ratios (<0.5130) than the Madeira domain. We interpret the distinct compositions of these domains to reflect spatial zonation in the deeper sources of the mantle upwellings. The domains include zones influenced by Enriched Mantle (EM) I and II, which appear to be orientated along the extension of the Oceanographer (at ˜ 34° N) and the Azores-Gibraltar fracture zones (at ˜ 37° N), respectively. The first zone includes a hitherto unknown seamount that exhibits the most extreme EM I composition yet

  7. Mesospheric observations by a forward scattering meteor radar basic setup

    NASA Astrophysics Data System (ADS)

    Madkour, Waleed; Yamamoto, Masa-yuki

    2016-08-01

    The durations of radio echo signals scattered from meteor ionized trails might not show a consistent increase corresponding to higher density trails due to the rapid removal of meteor ions at certain heights. Several studies have concluded the dominant role of the secondary ozone layer over diffusion in the removal of the meteor trails below 95 km through chemical oxidization of the meteor ions. Using a basic setup configuration of a forward scattering receiver, a trial to observe the mesospheric ozone concentration was performed by analyzing the meteor echo duration distributions. The forward scattered meteor echoes have the advantage of long durations that can enable observing the transition from the diffusion-removal regime to the chemistry-removal regime. The cumulative meteor echo duration distribution of two meteor showers, the Perseids and the Geminids, were analyzed over 10 years and the chemistry-removal regime in each shower was observed. The knee duration position at which a drop in the number of long overdense meteor echoes starts differed by around 30 seconds between the two showers. As the secondary ozone concentration is inversely related to the solar activity level, the Geminids 2011 corresponding to a high solar activity level showed a significant higher counts of long duration echoes compared to the Geminids 2006 during a low activity level, with the knee position shifted to longer duration. The knee positions obtained during the two distinct meteor showers and the two half solar cycle points are generally in agreement with the mesospheric ozone conditions expected in each case. However, continuous data record is required for the other meteor showers and the sporadic meteors at different heights to observe the mesospheric ozone concentration vertically and the full 11-years solar cycle.

  8. On the origin of ringing irregularities - A meteor hypothesis

    NASA Technical Reports Server (NTRS)

    Deshpande, M. R.; Vats, H. O.; Trivedi, A. I.

    1978-01-01

    Isolated ionospheric irregularities produce oscillating diffraction patterns on the ground. In the present study typical physical properties such as density, size, etc. of these irregularities are estimated on the basis of diffraction pattern characteristics. These properties agree well with those of meteor trail ionization and it has been found that most of these oscillating irregularities occur on meteor shower days. It is therefore suggested that the oscillating irregularities are caused by meteor showers.

  9. Multi-Year CMOR Observations of the Geminid Meteor Shower

    NASA Technical Reports Server (NTRS)

    Webster, A. R.; Jones, J.

    2011-01-01

    The three-station Canadian Meteor Orbit Radar (CMOR) is used here to examine the Geminid meteor shower with respect to variation in the stream properties including the flux and orbital elements over the period of activity in each of the consecutive years 2005 2008 and the variability from year to year. Attention is given to the appropriate choice and use of the D-criterion in the separating the shower meteors from the sporadic background.

  10. Tracing hillslope sediment production and transport with in situ and meteoric 10Be

    NASA Astrophysics Data System (ADS)

    Jungers, Matthew C.; Bierman, Paul R.; Matmon, Ari; Nichols, Kyle; Larsen, Jennifer; Finkel, Robert

    2009-12-01

    We use in situ-produced and meteoric 10Be, analyzed in soils from 28 pits on four hillcrest-parallel transects along a 14° hillslope in the Great Smoky Mountains, North Carolina, as tracers of soil production and transport. We rely upon amalgamation both to investigate and smooth spatial variability in 10Be concentrations. Lidar indicates that the hillslope is topographically complex and that soil is moved downslope diffusively until it encounters the ephemeral channel network and is rapidly exported. In situ-produced 10Be, measured in depth profiles, indicates that over millennial timescales, soils are mixed above the soil-saprolite boundary. In contrast, meteoric 10Be concentrations increase with depth and are correlated to concurrent increases of dithionite-extractable Al and pH, observations explained by similar Al and Be mobility in the soil. The concentrations of both meteoric and in situ-produced 10Be increase downslope proportional to the maximum soil particle path length. The data suggest virtual downslope soil velocities of 1.1-1.7 cm yr-1 in a well-mixed active transport layer ˜60 cm thick. The thickness of this transport layer is constant downslope and depends on the rooting depth and consequent root wad thickness of downed trees on the slope, both of which reflect depth to the soil/saprolite boundary. Both meteoric and in situ-produced 10Be suggest that soil production is balanced by surface denudation at rates between 10 and 13 m Myr-1. Soil residence times on the slope range from 21 to 33 kyr based on the meteoric 10Be inventories. Major element geochemical analysis suggests little if any elemental loss during soil transport downslope.

  11. Endemicity, Biogeography, Composition, and Community Structure On a Northeast Pacific Seamount

    PubMed Central

    McClain, Craig R.; Lundsten, Lonny; Ream, Micki; Barry, James; DeVogelaere, Andrew

    2009-01-01

    The deep ocean greater than 1 km covers the majority of the earth's surface. Interspersed on the abyssal plains and continental slope are an estimated 14000 seamounts, topographic features extending 1000 m off the seafloor. A variety of hypotheses are posited that suggest the ecological, evolutionary, and oceanographic processes on seamounts differ from those governing the surrounding deep sea. The most prominent and oldest of these hypotheses, the seamount endemicity hypothesis (SMEH), states that seamounts possess a set of isolating mechanisms that produce highly endemic faunas. Here, we constructed a faunal inventory for Davidson Seamount, the first bathymetric feature to be characterized as a ‘seamount’, residing 120 km off the central California coast in approximately 3600 m of water (Fig 1). We find little support for the SMEH among megafauna of a Northeast Pacific seamount; instead, finding an assemblage of species that also occurs on adjacent continental margins. A large percentage of these species are also cosmopolitan with ranges extending over much of the Pacific Ocean Basin. Despite the similarity in composition between the seamount and non-seamount communities, we provide preliminary evidence that seamount communities may be structured differently and potentially serve as source of larvae for suboptimal, non-seamount habitats. PMID:19127302

  12. Shigaraki middle and upper atmosphere radar meteor-head-echo database

    NASA Astrophysics Data System (ADS)

    Kero, J.; Nakamura, T.; Szasz, C.; Kastinen, D.; Watanabe, J.; Yamamoto, M.; Fujiwara, Y.; Abo, M.; Tanaka, Y.; Abe, S.

    2014-07-01

    Introduction: Mass infux from space into the terrestrial atmosphere is mainly caused by meteors. Meteors deliver various elements into the atmosphere and the meteoric dust particles are of great importance in the terrestrial atmosphere. For example, they act as nucleus for condensation and clouds and affect various atmospheric phenomena both in physical and chemical aspects. Thus, to investigate the meteor flux, orbits and their interactions in the upper atmosphere is very important but at the same time the method of investigation is limited, especially for precise measurements. High-power large-aperture (HPLA) radar observation is a recent technique to provide useful information on meteor infux and orbits, as well as interactions with the atmosphere. Since 2009 orbital data of about 120,000 meteors [2] have been collected using a novel head-echo analysis algorithm for the lower VHF band [1]. The data was collected using the middle and upper atmosphere radar (MU radar) of Kyoto University at Shigaraki (34.9N, 136.1S). The MU radar is a large atmospheric VHF radar with 46.5 MHz frequency, 1 MW output transmission power and 8330 m^2 aperture array antenna. An open database (MU radar meteor head echo database: MURMHED) for research and education is now being created. Database: The database currently holds 53 different parameters for each event and a number of associated time series consisting of range, height, radar cross section, signal to noise ratio, radial velocity and meteorid velocity. The database parameters are MJD, Year [UT], Month [UT], Day [UT], Hour [UT], Minute [UT], Second [UT], Duration [s], RA [deg], Dec [deg], Az [deg], Ze [deg], Az uncorr [deg], Ze uncorr [deg], Ze correction [deg], Obs initial vel [km/s], Geocentric vel [km/s], RCS [dBsm], SNR [dB], Start hgt [km], End hgt [km], Az of start point [deg], Ze of start point [deg], Az of end point [deg], Ze of end point [deg], Semimajor axis [au], Eccentricity, Perihelion dist [au], Lon of asc node [deg

  13. Optical and Radar Measurements of the Meteor Speed Distribution

    NASA Technical Reports Server (NTRS)

    Moorhead, A. V.; Brown, P. G.; Campbell-Brown, M. D.; Kingery, A.; Cooke, W. J.

    2016-01-01

    The observed meteor speed distribution provides information on the underlying orbital distribution of Earth-intersecting meteoroids. It also affects spacecraft risk assessments; faster meteors do greater damage to spacecraft surfaces. Although radar meteor networks have measured the meteor speed distribution numerous times, the shape of the de-biased speed distribution varies widely from study to study. Optical characterizations of the meteoroid speed distribution are fewer in number, and in some cases the original data is no longer available. Finally, the level of uncertainty in these speed distributions is rarely addressed. In this work, we present the optical meteor speed distribution extracted from the NASA and SOMN allsky networks [1, 2] and from the Canadian Automated Meteor Observatory (CAMO) [3]. We also revisit the radar meteor speed distribution observed by the Canadian Meteor Orbit Radar (CMOR) [4]. Together, these data span the range of meteoroid sizes that can pose a threat to spacecraft. In all cases, we present our bias corrections and incorporate the uncertainty in these corrections into uncertainties in our de-biased speed distribution. Finally, we compare the optical and radar meteor speed distributions and discuss the implications for meteoroid environment models.

  14. The Orionid Meteor Shower Observed Over 70 Years

    NASA Astrophysics Data System (ADS)

    Rendtel, Jürgen

    2008-06-01

    Visual Orionid meteor data dating back to 1944 were transformed into the standard format of the Visual Meteor Data Base (VMDB) of the International Meteor Organization (IMO) for systematic analysis. The strong 2006 Orionid return with a very low population index ( r = 1.6) and a peak ZHR of 60 (about 2.5 of the average peak strength) resembled meteor showers connected with the returns of resonant meteoroids. An investigation of data dating back to 1928 yielded similar rate enhancements in 1936, further supporting the assumption that meteoroids trapped in the 1:6 resonance with Jupiter caused the unusual 2006 Orionid return.

  15. Results of the IMO Video Meteor Network - December 2014

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Crivello, Stefano; Stomeo, Enrico; Barentsen, Geert; Goncalves, Rui; Saraiva, Carlos; Maciewski, Maciej; Maslov, Mikhail

    2015-04-01

    In 2014 December, 85 cameras of the IMO Video Meteor Network recorded almost 45 000 meteors in over 9 300 hours of observing time. The flux density profile is presented for the Geminids, as well as the population index profile around the maximum. A short-lasting outburst of the Ursids occurred on 2014 December 23 at 0h UT that reached a flux density of 60 meteoroids per 1 000 km^2 per hour in a 30-minute interval. The annual summary of the 2014 IMO Video Meteor Network observations is presented. More than 367 000 meteors were recorded in almost 100 000 hours of observing time.

  16. Results of the IMO Video Meteor Network - December 2015

    NASA Astrophysics Data System (ADS)

    Molau, S.; Crivello, S.; Goncalves, R.; Saraiva, C.; Stomeo, E.; Kac, J.

    2016-04-01

    In 2015 December, 80 cameras of the IMO Video Meteor Network recorded over 60 000 meteors in more than 10 600 hours of observing time. The flux density profile is presented for the Geminids and compared to previous years. The population index profile of the Geminids is also presented. The activity of the Ursids was slightly enhanced again. The flux density profile is presented and compared to profiles since 2011. The annual summary of the 2015 IMO Video Meteor Network observations is presented. More than 480 000 meteors were recorded in almost 122 000 hours of observing time.

  17. Spectral analysis of a high-velocity meteor

    NASA Technical Reports Server (NTRS)

    Harvey, G. A.

    1977-01-01

    A spectrogram of a fast optical meteor was reduced and analyzed, and 60 features were identified in the spectrum. Air and ionized elements in this meteor radiate throughout the spectrum from 3000 A to 6800 A. A mass of 9 mg and an effective radiation temperature of approximately 5700 K were computed for the meteor. Weight ratios of Ca:Fe, and Mg:Fe, and Na:Fe were computed. A plasma particle velocity distribution for meteors was derived, and the average collision speed obtained from this distribution was compared with the relative collision speed of a Fe-N2 gas mixture at 5700 K.

  18. METEOR - an artificial intelligence system for convective storm forecasting

    SciTech Connect

    Elio, R.; De haan, J.; Strong, G.S.

    1987-03-01

    An AI system called METEOR, which uses the meteorologist's heuristics, strategies, and statistical tools to forecast severe hailstorms in Alberta, is described, emphasizing the information and knowledge that METEOR uses to mimic the forecasting procedure of an expert meteorologist. METEOR is then discussed as an AI system, emphasizing the ways in which it is qualitatively different from algorithmic or statistical approaches to prediction. Some features of METEOR's design and the AI techniques for representing meteorological knowledge and for reasoning and inference are presented. Finally, some observations on designing and implementing intelligent consultants for meteorological applications are made. 7 references.

  19. Observation and research for strong meteor shower and related catastrophic space weather

    NASA Astrophysics Data System (ADS)

    Ma, Y. H.; He, Y. W.; Xu, P. X.; Zhao, H. B.

    2007-07-01

    During the first international joint observation for strong meteor shower, we made multi-subject observations for Leonids and Draconids and their disaster space weather events by several methods. Combining the synthetical analysis of Leonids, Perseids and Draconids and their related data from 1957 to 2003, we sufficiently confirm that the periodic strong meteor showers can result in the formation of catastrophic space weather events. The following summing-up is confirmed basically: 1.The formation mechanism of the strong meteor shower There are meteoroids with high density and uneven distribution close the cometary nucleus, especially in the direction of opposite the Sun and backside of the nucleus. They can stretch 1-11AU along the cometary orbit and 1-5 (&sim10^3AU) cross the orbit. Therefore good displays of meteor shower (10---100 times as usual) or storms (103---104 times as usual) can occur when the Earth passes a high density meteoroid stream during the period of 3 years before and 5 years after the perihelion passage of the comet. During that period, bolides or shooting stars which are serious harmful to spaceflight security increase greatly to 3%~10%. This corrects the wrong point of view that the harmful micro-meteoroids to spaceflight security in period meteor showers are <1 g only. 2. The cosmic dust maintaining mechanism of long-life Es layer in mid-latitude area It is proved the life of Es layer increased greatly when most ions are long-life metal type ions (Fe +, Mg + ?? ) which composite coefficient is much smaller than that of molecule type ions(O2 + , NO + ?? ). The observation for about 50 years roughly approves that the blanketing frequency of Es layer (fb Es) abnormally increase in large area (>105km2) and lasting long time (>15 min) only when strong meteor shower occurred at night. It is not f, l and c type Es layer evolved from sequence Es layer. This shows that the cause of fb Es increase is that the ionosphere was bombarded by an additional

  20. Numerical simulation of earthquake rupture sequences on the Manila thrust fault: Effects of seamount subduction

    NASA Astrophysics Data System (ADS)

    Yu, H.; Liu, Y.; Ning, J.; He, C.; Zhang, L.

    2015-12-01

    The Manila subduction zone is located at the convergent boundary between the Philippine Sea Plate and the Sunda/Eurasian Plate from offshore Taiwan to northern Luzon of Philippines, where only infrequent M7 earthquakes were observed in modern seismological instrumentation history. The lack of great events (M8+) indicates the subduction fault is either aseismically slipping or is accumulating strain energy toward rapid release in a great earthquake. Here we conduct numerical simulations of earthquake rupture sequences in the framework of rate-state-friction along the 15-19.5ºN segment of the 3D plate boundary with subducted seamounts. Rate-state frictional properties are constrained by laboratory friction experiments conducted on IODP Expedition 349, South China Sea (SCS), drilling samples from the basaltic basement rock under 100ºC - 600ºC, effective normal stress of 50 MPa and pore pressure of 100 MPa. During the modeled 2000-year period, the maximum magnitude of earthquakes is Mw7. Each sequence repeats every ~200 years and is consisted of three sub-events, event 1 (Mw7) that can overcome the barrier, where dip angle changes most rapidly along the strike, to rupture the entire fault. Events 2 (Mw 6.4) and 3 (Mw 5.7) are of smaller magnitudes and result in north-south segmented rupture pattern. We further quantify the potential of earthquake nucleation by the S-ratio (lower S ratio means the initial stress is closer to peak strength, hence more likely to nucleate an earthquake). The subducted seamount shows higher S-ratios than its surroundings mostly, implying an unlikely nucleate area. Our results are qualitatively similar to 2D subduction earthquake modeling by Herrendörfer et al. (2015, 2-3 events per supercycle and median long-term S is 0.5-1). Finally, we plan to use our coseismic rupture model results as inputs for a tsunami propagation model in SCS. Compared to the kinematic seafloor deformation input, our physics-based earthquake source model and its

  1. A Global Model of Meteoric Sodium

    NASA Technical Reports Server (NTRS)

    Marsh, Daniel R.; Janches, Diego; Feng, Wuhu; Plane, John M. C.

    2013-01-01

    A global model of sodium in the mesosphere and lower thermosphere has been developed within the framework of the National Center for Atmospheric Research's Whole Atmosphere Community Climate Model (WACCM). The standard fully interactive WACCM chemistry module has been augmented with a chemistry scheme that includes nine neutral and ionized sodium species. Meteoric ablation provides the source of sodium in the model and is represented as a combination of a meteoroid input function (MIF) and a parameterized ablation model. The MIF provides the seasonally and latitudinally varying meteoric flux which is modeled taking into consideration the astronomical origins of sporadic meteors and considers variations in particle entry angle, velocity, mass, and the differential ablation of the chemical constituents. WACCM simulations show large variations in the sodium constituents over time scales from days to months. Seasonality of sodium constituents is strongly affected by variations in the MIF and transport via the mean meridional wind. In particular, the summer to winter hemisphere flow leads to the highest sodium species concentrations and loss rates occurring over the winter pole. In the Northern Hemisphere, this winter maximum can be dramatically affected by stratospheric sudden warmings. Simulations of the January 2009 major warming event show that it caused a short-term decrease in the sodium column over the polar cap that was followed by a factor of 3 increase in the following weeks. Overall, the modeled distribution of atomic sodium in WACCM agrees well with both ground-based and satellite observations. Given the strong sensitivity of the sodium layer to dynamical motions, reproducing its variability provides a stringent test of global models and should help to constrain key atmospheric variables in this poorly sampled region of the atmosphere.

  2. Meteor orbit determination with improved accuracy

    NASA Astrophysics Data System (ADS)

    Dmitriev, Vasily; Lupovla, Valery; Gritsevich, Maria

    2015-08-01

    Modern observational techniques make it possible to retrive meteor trajectory and its velocity with high accuracy. There has been a rapid rise in high quality observational data accumulating yearly. This fact creates new challenges for solving the problem of meteor orbit determination. Currently, traditional technique based on including corrections to zenith distance and apparent velocity using well-known Schiaparelli formula is widely used. Alternative approach relies on meteoroid trajectory correction using numerical integration of equation of motion (Clark & Wiegert, 2011; Zuluaga et al., 2013). In our work we suggest technique of meteor orbit determination based on strict coordinate transformation and integration of differential equation of motion. We demonstrate advantage of this method in comparison with traditional technique. We provide results of calculations by different methods for real, recently occurred fireballs, as well as for simulated cases with a priori known retrieval parameters. Simulated data were used to demonstrate the condition, when application of more complex technique is necessary. It was found, that for several low velocity meteoroids application of traditional technique may lead to dramatically delusion of orbit precision (first of all, due to errors in Ω, because this parameter has a highest potential accuracy). Our results are complemented by analysis of sources of perturbations allowing to quantitatively indicate which factors have to be considered in orbit determination. In addition, the developed method includes analysis of observational error propagation based on strict covariance transition, which is also presented.Acknowledgements. This work was carried out at MIIGAiK and supported by the Russian Science Foundation, project No. 14-22-00197.References:Clark, D. L., & Wiegert, P. A. (2011). A numerical comparison with the Ceplecha analytical meteoroid orbit determination method. Meteoritics & Planetary Science, 46(8), pp. 1217

  3. Emplacement, growth, and gravitational deformation of serpentinite seamounts on the Mariana forearc

    NASA Astrophysics Data System (ADS)

    Oakley, A. J.; Taylor, B.; Fryer, P.; Moore, G. F.; Goodliffe, A. M.; Morgan, J. K.

    2007-08-01

    Serpentinite seamounts, representing some of the first material outputs of the recycling process that takes place in subduction zones, are found on the outer Mariana forearc. Multichannel seismic (MCS) and bathymetric data collected in 2002 image the large-scale structures of five seamounts, as well as the pre-seamount basement geometry and sediment stratigraphy. We present data from three edifices that provide insights into seamount growth and internal deformation processes and allow us to support the interpretation that serpentinite mud volcanoes are formed by the episodic eruption of mud flows from a central region. The presence of thrust faulting at the base of Turquoise and Big Blue Seamounts, along with the low surface slopes (5°-18°) of all the seamounts studied, lead us to infer that these edifices spread laterally and are subject to gravitational deformation as they grow. Numerical simulations using the discrete element method (DEM) were used to model their growth and the origins of features that we see in MCS sections, such as basal thrusts, inward-dipping reflections and mid-flank benches. The DEM simulations successfully reproduced many of the observed features. Simulations employing very low basal and internal friction coefficients (~0.1 and ~0.4, respectively) provide the best match to the overall morphology and structures of the serpentinite seamounts. However the simulations do not capture all of the processes involved in seamount growth, such as withdrawal of material from a central conduit leading to summit deflation; compaction, dewatering and degassing of mud flows; mass wasting in the form of sector collapse and growth upon a dipping substrate. A strong reflection beneath the summit of Big Blue, the largest serpentinite seamount on the Mariana forearc, represents the floor of a summit depression that has been partially in-filled by younger muds, supporting the idea that serpentinite seamounts grow by episodic mud volcanism. Boundaries of mud

  4. Meteor Beliefs Project: Classical beliefs connecting meteors with life and death

    NASA Astrophysics Data System (ADS)

    McBeath, Alastair; Gheorghe, Andrei Dorian

    2006-10-01

    Details concerning meteors as indicators of life and death, extracted from ancient Greek and Latin sources between the circa 5th century BC to the circa 5th century AD, are presented. Some relevant material concerning souls as resident in stars in a similar vein is given too.

  5. Meteor Beliefs Project: some meteoric imagery in the works of William Shakespeare

    NASA Astrophysics Data System (ADS)

    McBeath, A.; Gheorghe, A. D.

    2003-08-01

    Passages from three of William Shakespeare's plays are presented, illustrating some of the beliefs in meteors in 16th-17th century England. They also reflect earlier beliefs and information which it is known Shakespeare drew on in constructing his works.

  6. Meteor Beliefs Project: Meteoric imagery associated with the death of John Brown in 1859

    NASA Astrophysics Data System (ADS)

    Drobnock, G. J.; McBeath, A.; Gheorghe, A. D.

    2009-12-01

    An examination is made of metaphorical meteor imagery used in conjunction with the death of American anti-slavery activist John Brown, who was executed in December 1859. Such imagery continues to be used in this regard into the 21st century.

  7. Present State and Prospects for the Meteor Research in Ukraine

    NASA Astrophysics Data System (ADS)

    Shulga, O.; Voloshchuk, Y.; Kolomiyets, S.; Cherkas, Y.; Kimakovskay, I.; Kimakovsky, S.; Knyazkova, E.; Kozyryev, Y.; Sybiryakova, Y.; Gorbanev, Y.; Stogneeva, I.; Shestopalov, V.; Kozak, P.; Rozhilo, O.; Taranukha, Y.

    2015-03-01

    ODESSA. Systematical study of the meteor events are being carried out since 1953. In 2003 complete modernization of the observing technique was performed, and TV gmeteor patrolh on the base of WATEC LCL902 cameras was created. @ wide variety of mounts and objectives are used: from Schmidt telescope F = 540 mm, F/D = 2.25 (field of view FOV = (0.68x0.51) deg, star limiting magnitude SLM = 13.5 mag, star astrometric accuracy 1-2 arcsec) up to Fisheye lenses F = 8 mm, F/D = 3.5 (FOV = (36x49) deg, SLM = 7 mag). The database of observations that was collected between 2003 and 2012 consists of 6176 registered meteor events. Observational programs on basis and non-basis observations in Odessa (Kryzhanovka station) and Zmeiny island are presented. Software suite of 12 programs was created for processing of meteor TV observations. It enables one to carry out the whole cycle of data processing: from image preprocessing up to orbital elements determination. Major meteor particles research directions: statistic, areas of streams, precise stream radiant, orbit elements, phenomena physics, flare appearance, wakes, afterglow, chemistry and density. KYIV. The group of meteor investigations has been functioning more than twenty years. The observations are carried out simultaneously from two points placed at the distance of 54 km. Super-isocon low light camera tubes are used with photo lens: F = 50mm, F/D = 1.5 (FOV = (23.5 x 19.0) deg, SLM = 9.5 mag), or F = 85, F/D = 1.5 (FOV = (13x11) deg, SLM = 11.5 mag). Astrometry, photometry, calculation of meteor trajectory in Earth atmosphere and computation of heliocentric orbit are realized in developed gFalling Starh software. KHARKOV. Meteor radio-observations have begun in 1957. In 1972, the radiolocation system MARS designed for automatic meteor registration was recognized as being the most sensitive system in the world. With the help of this system 250 000 faint meteors (up to 12 mag) were registered between 1972 and 1978 (frequency

  8. The meteor complex of P/Encke

    NASA Astrophysics Data System (ADS)

    Porubcan, V.; Stohl, J.

    The Taurid meteor complex associated with P/Encke is studied on the basis of relevant photographic and radar orbits. Orbital characteristics, radiants and durations of the postperihelion showers are compared with corresponding theoretical values derived from the observations of the preperihelion Taurids. The validity of the proposed associations of minor showers with the Taurid complex and the total duration of its activity are evaluated and discussed. Some of the associated showers (the Northern and Southern Chi Orionids, Northern Piscids and Southern Arietids) are confirmed to be in fact, parts of the Taurid shower itself.

  9. Aging comets and their meteor showers

    NASA Astrophysics Data System (ADS)

    Ye, Quan-Zhi

    2016-10-01

    Comets are thought to be responsible for the terrestrial accretion of water and organic materials. The aging of comets is one of the most critical yet poorly understood problems in planetary astronomy. Here we attack this problem by examining different parts of the cometary aging spectrum of Jupiter-family comets (JFCs), a group of comets that dominates the cometary influx in the near-Earth space, using both telescopic and meteor observations.We examine two representative JFCs and the population of dormant comets. At the younger end of the aging spectrum, we examine a moderately active JFC, 15P/Finlay, and review the puzzle of the non-detection of the associated Finlayid meteor shower. We find that, although having been behaved like a dying comet in the past several 102 years, 15P/Finlay does possess ability for energetic outbursts without a clear reason. Towards the more aged end of the spectrum, we examine a weakly active JFC, 209P/LINEAR. By bridging telescopic observations at visible and infrared wavelength, meteor observations and dynamical investigations, we find that 209P/LINEAR is indeed likely an aged yet long-lived comet. At the other end of the spectrum, we examine the population of dormant near-Earth comets, by conducting a comprehensive meteor-based survey looking for dormant comets that have recently been active. We find the lower limit of the dormant comet fraction in the near-Earth object (NEO) population to be 2.0 ± 1.7%. This number is at the lower end of the numbers found using dynamical and telescopic techniques, which may imply that a significant fraction of comets in the true JFC population are weakly active and are not yet detected.These results have revealed interesting diversities in dying or dead comets, both in their behaviors as well as their natures. An immediate quest in the understanding of cometary aging would be to examine a large number of dying or dead comets and understand their general characteristics.

  10. Analysis of photometric spectra of 17 meteors

    NASA Technical Reports Server (NTRS)

    Millman, P. M.

    1982-01-01

    The initial phase of the photometry which involved 17 meteor spectra consisting of eight Geminid spectra, six Orionid spectra and three Eta Aquarid spectra is discussed. Among these 17 spectra it is found that the Geminid spectra are of the best quality and are used for the identification of the atomic lines and molecular bands that normally appear on video tape spectra. The data from the Geminid records are used for developing calibration techniques in photometry. The Orionid and Eta Aquarid spectra are chosen for early analysis because of the current interest in all physical and chemical data relating to Comet Halley.

  11. In Situ-produced vs. Meteoric 10Be in Hillslope Soils: One Isotope, Two Tracers, Different Stories

    NASA Astrophysics Data System (ADS)

    Jungers, M. C.; Bierman, P. R.; Matmon, A.; Cox, R.; Pavich, M.; Finkel, R. C.

    2009-12-01

    In situ-produced and meteoric 10Be are both powerful tools for tracing the production and transport of hillslope sediment. In situ-produced 10Be is used to infer sediment production rates as well as investigate sediment sources and transport. Meteoric 10Be may also be useful for inferring sediment production and transport rates in some landscapes, especially those that lack the target minerals for in situ-produced 10Be. Few studies have investigated the insights gained by a comparing in situ-produced and meteoric 10Be inventories. We present a series of paired 10Be inventories from different climatic and tectonic regimes to illustrate both the value and the potential pitfalls of coupling these geomorphic tracers. The mean in situ and meteoric 10Be near surface (within a meter) inventories for our field areas are as follows: Great Smoky Mountains, NC, USA: 3.6 x 107 atoms cm-2 and 3.3 x 1010 atoms cm-2; Laurely Fork, PA, USA: 2.6 x 106 atoms cm-2 and 3.0 x 109 atoms cm-2; Oregon Coast Range, OR, USA: no in situ data and 3.87 x 1010 atoms cm-2; North Island, New Zealand: no in situ data and 1.8 x 109 atoms cm-2; and Amparafaravola, Madagascar: 1.86 x 107 atoms cm-2 and 8.0 x 109 atoms cm-2. The associated inferred soil residence times, respectively, are: Great Smoky Mountains, NC, USA: 40.9 ky and 25.6 ky; Laurely Fork, PA, USA: 2.9 ky and 2.3 ky; Oregon Coast Range, OR, USA: n/a and 30ky; North Island, New Zealand: n/a and 1.5 ky; and Amparafaravola, Madagascar: 21 ky and 6.2 ky. Soil residence times inferred from meteoric 10Be assume a global average delivery rate of 1.3 x 106 atoms cm-2 yr-1. These soil residence times are minimum values that assume that all in situ and meteoric 10Be is accounted for. Discrepancies between inferred soil residence times most likely highlight some error in assumptions regarding meteoric 10Be retention in the soil mantles that we sampled. For example, if meteoric 10Be is not retained at the near surface where we collected our samples

  12. Determination of Parameters of Meteor Bodies from Observational Data with High Accuracy of Estimate

    NASA Astrophysics Data System (ADS)

    Gritsevich, Maria

    A great volume of data has been accumulated thus far related to the photoregistration of the paths of meteor bodies in the terrestrial atmosphere. Most images have been obtained by four fireball networks, which operate in the USA, Canada, Europe, and Spain in different time periods. The approximation of the actual data using theoretical models makes it possible to achieve additional estimates, which do not directly follow from the observations. For example, the correct mathematical modeling of meteor events in the atmosphere is necessary for further estimates of the key parameters, including the extra-atmospheric mass, the ablation coefficient, and the effective enthalpy of evaporation of entering bodies. In turn, this information is needed by some applications, namely, those aimed at studying the problems of asteroid and comet security, to develop measures of planetary defense, and to determine the bodies that can reach Earth's surface. In the report, the mathematical technique to find basic dynamic parameters of the theoretical relationship between the height and the velocity of the meteor body motion that help to fit observations along the luminous part of the trajectories in the best way is suggested. The main difference from previous studies is that the given observations are approximated using the analytical solution of the equations of meteor physics. Note that, for the limited values of the mass loss parameter, analytical solution is usually replaced by the simpler expression (e.g., Stulov et al., 1995). In particular, this approximate solution was earlier used as a trial function during the implementation of the least-squares method. New model presented in the report was applied to a number of bright meteors observed by the Canadian camera network and by the US Prairie network. Results of such calculation are partly presented. During our data processing we discovered several sufficiently thermostable meteor bodies whose mass loss parameters were almost

  13. Stepwise coupled mode scattering of ambient noise by a cylindrically symmetric seamount.

    PubMed

    Evans, Richard B

    2006-01-01

    The question of how underwater ambient noise, at low frequencies, interacts with seamounts is addressed. The vertical directivity of the ambient noise, with and without the seamount interaction, is of particular interest. The problem of ambient noise scattering by seamounts motivates the development of a numerical modeling procedure, based on stepwise coupled modes. The procedure is designed to analyze scattering from a cylindrically symmetric seamount. The stepwise coupled mode procedure is extended to more general boundary conditions and brought up to date in the process. An example, using the geometry of the Dickins seamount, suggests that the seamount removes energy from the steeply traveling ambient noise, for this case. The energy is not converted into angles near the horizontal; the energy is lost through bottom interaction and attenuation.

  14. Computer code simulations of the formation of Meteor Crater, Arizona - Calculations MC-1 and MC-2

    NASA Technical Reports Server (NTRS)

    Roddy, D. J.; Schuster, S. H.; Kreyenhagen, K. N.; Orphal, D. L.

    1980-01-01

    It has been widely accepted that hypervelocity impact processes play a major role in the evolution of the terrestrial planets and satellites. In connection with the development of quantitative methods for the description of impact cratering, it was found that the results provided by two-dimensional finite difference, computer codes is greatly improved when initial impact conditions can be defined and when the numerical results can be tested against field and laboratory data. In order to address this problem, a numerical code study of the formation of Meteor (Barringer) Crater, Arizona, has been undertaken. A description is presented of the major results from the first two code calculations, MC-1 and MC-2, that have been completed for Meteor Crater. Both calculations used an iron meteorite with a kinetic energy of 3.8 Megatons. Calculation MC-1 had an impact velocity of 25 km/sec and MC-2 had an impact velocity of 15 km/sec.

  15. 50 CFR Table 22 to Part 679 - Alaska Seamount Habitat Protection Areas

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 50 Wildlife and Fisheries 9 2010-10-01 2010-10-01 false Alaska Seamount Habitat Protection Areas... ZONE OFF ALASKA Pt. 679, Table 22 Table 22 to Part 679— Alaska Seamount Habitat Protection Areas Area No. Name Latitude Longitude 1 Dickins Seamount 54 39.00 N 136 48.00 W 54 39.00 N 137 9.00 W 54...

  16. 50 CFR Table 22 to Part 679 - Alaska Seamount Habitat Protection Areas

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 50 Wildlife and Fisheries 11 2011-10-01 2011-10-01 false Alaska Seamount Habitat Protection Areas... ZONE OFF ALASKA Pt. 679, Table 22 Table 22 to Part 679— Alaska Seamount Habitat Protection Areas Area No. Name Latitude Longitude 1 Dickins Seamount 54 39.00 N 136 48.00 W 54 39.00 N 137 9.00 W 54...

  17. 50 CFR Table 22 to Part 679 - Alaska Seamount Habitat Protection Areas

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 50 Wildlife and Fisheries 13 2012-10-01 2012-10-01 false Alaska Seamount Habitat Protection Areas... ZONE OFF ALASKA Pt. 679, Table 22 Table 22 to Part 679— Alaska Seamount Habitat Protection Areas Area No. Name Latitude Longitude 1 Dickins Seamount 54 39.00 N 136 48.00 W 54 39.00 N 137 9.00 W 54...

  18. 50 CFR Table 22 to Part 679 - Alaska Seamount Habitat Protection Areas

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 50 Wildlife and Fisheries 13 2013-10-01 2013-10-01 false Alaska Seamount Habitat Protection Areas... ZONE OFF ALASKA Pt. 679, Table 22 Table 22 to Part 679— Alaska Seamount Habitat Protection Areas Area No. Name Latitude Longitude 1 Dickins Seamount 54 39.00 N 136 48.00 W 54 39.00 N 137 9.00 W 54...

  19. 50 CFR Table 22 to Part 679 - Alaska Seamount Habitat Protection Areas

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 50 Wildlife and Fisheries 13 2014-10-01 2014-10-01 false Alaska Seamount Habitat Protection Areas... ZONE OFF ALASKA Pt. 679, Table 22 Table 22 to Part 679— Alaska Seamount Habitat Protection Areas Area No. Name Latitude Longitude 1 Dickins Seamount 54 39.00 N 136 48.00 W 54 39.00 N 137 9.00 W 54...

  20. On geoid heights and flexure of the lithosphere at seamounts

    NASA Astrophysics Data System (ADS)

    Watts, A. B.; Ribe, N. M.

    1984-12-01

    The sea surface height has now been mapped to an accuracy of better than ±1 m by using radar altimeters on board orbiting satellites. The major influence on the mean sea surface height is the marine geoid which is an equipotential surface. We have carried out preliminary studies of how oceanic volcanoes, which rise above the ocean floor as isolated seamounts and oceanic islands or linear ridges, contribute to the marine geoid. Simple one- and two-dimensional models have been constructed in which it is assumed that the oceanic lithosphere responds to volcanic loads as a thin elastic plate overlying a weak fluid substratum. Previous studies based on gravity and bathymetry data and uplift/subsidence patterns show that the effective flexural rigidity of oceanic lithosphere and the equivalent elastic thickness Te increase with the age of the lithosphere at the time of loading. The models predict that isolated seamounts emplaced on relatively young lithosphere on or near a mid-ocean ridge crest will be associated with relatively low amplitude geoid anomalies (about 0.4-0.5 m/km of height), while seamounts formed on relatively old lithosphere, on ridge flanks, will be associated with much higher amplitude anomalies (1.4-1.5 m/km). Studies of the Seasat altimetric geoid prepared by NASA's Jet Propulsion Laboratory support these model predictions; geoid amplitudes are relatively low over the Mid-Pacific Mountains and Line Islands, which formed on or near a mid-ocean ridge crest, and relatively high over the Magellan Seamounts and Wake Guyots, which formed off ridge. Direct modeling of the altimetric geoid over these features is complicated, however, by the wide spacing of the satellite tracks (which can exceed 100 km) and poor bathymetric control beneath individual satellite tracks. In regions where multibeam bathymetric surveys are available, models can be constructed that fit the altimetric geoid to better than ±1 m. Studies of geoid anomalies over the Emperor seamount

  1. Very Precise Orbits of 1998 Leonid Meteors

    NASA Technical Reports Server (NTRS)

    Betlem, Hans; Jenniskens, Peter; vantLeven, Jaap; terKuile, Casper; Johannink, Carl; Zhao, Hai-Bin; Lei, Chen-Ming; Li, Guan-You; Zhu, Jin; Evans, Steve; DeVincenzi, Donald L. (Technical Monitor)

    1999-01-01

    Seventy-five orbits of Leonid meteors obtained during the 1998 outburst are presented. Thirty-eight are precise enough to recognize significant dispersion in orbital elements. Results from the nights of 1998 November 16/17 and 17/18 differ, in agreement with the dominant presence of different dust components. The shower rate profile of 1998 November 16/17 was dominated by a broad component, rich in bright meteors. The radiant distribution is compact. The semimajor axis is confined to values close to that of the parent comet, whereas the distribution of inclination has a central condensation in a narrow range. On the other hand, 1998 November 17/18 was dominated by dust responsible for a more narrow secondary peak in the flux curve. The declination of the radiant and the inclination of the orbit are more widely dispersed. The argument of perihelion, inclination, and the perihelion distance are displaced. These data substantiate the hypothesis that trapping in orbital resonances is important for the dynamical evolution of the broad component.

  2. Meteoric Magnesium Ions in the Martian Atmosphere

    NASA Technical Reports Server (NTRS)

    Pesnell, William Dean; Grebowsky, Joseph

    1999-01-01

    From a thorough modeling of the altitude profile of meteoritic ionization in the Martian atmosphere we deduce that a persistent layer of magnesium ions should exist around an altitude of 70 km. Based on current estimates of the meteoroid mass flux density, a peak ion density of about 10(exp 4) ions/cm is predicted. Allowing for the uncertainties in all of the model parameters, this value is probably within an order of magnitude of the correct density. Of these parameters, the peak density is most sensitive to the meteoroid mass flux density which directly determines the ablated line density into a source function for Mg. Unlike the terrestrial case, where the metallic ion production is dominated by charge-exchange of the deposited neutral Mg with the ambient ions, Mg+ in the Martian atmosphere is produced predominantly by photoionization. The low ultraviolet absorption of the Martian atmosphere makes Mars an excellent laboratory in which to study meteoric ablation. Resonance lines not seen in the spectra of terrestrial meteors may be visible to a surface observatory in the Martian highlands.

  3. Investigation of meteor shower parent bodies using various metrics

    NASA Astrophysics Data System (ADS)

    Dumitru, B. A.; Birlan, M.; Nedelcu, A.; Popescu, M.

    2016-01-01

    The present knowledge of meteor showers identifies the small bodies of our Solar System as supply sources for meteor streams. Both comets and asteroids are considered as the origin of meteor showers. The new paradigm of "active asteroids" opens up a large field of investigation regarding the relationships between asteroids and meteors. Processes like ejection and disaggregation at impacts, rotational instabilities, electrostatic repulsion, radiation pressure, dehydration stress followed by thermal fractures, sublimation of ices are sources of matter loss from asteroids. Our objective is to find genetic relationships between asteroids and meteor showers using metrics based on orbital elements. For this objective we selected three metrics (Southworth and Hawkins, 1963; Asher et al. 1993, and Jopek, 1993, respectively), the recent MPC database and the more recent IAU meteor shower database. From our analysis, 41 of the meteor showers have probabilities of being produced (or to be fueled) by asteroids. Our sample of asteroids contains more than 1000 objects, all of them belonging to the Near-Earth Asteroid population. The systematic approach performed, based on the physical properties of our sample, reinforced the link between asteroids and their associated meteor shower.

  4. The motion of radio meteor reflection point of Geminids

    NASA Astrophysics Data System (ADS)

    Ohnishi, Kouji; Ishikawa, Toshiyuki; Hattori, Shinobu; Nishimura, Osamu; Miyazawa, Akiko; Yanagisawa, Masatoshi; Endo, Makoto; Kawamura, Masaki; Maruyama, Toshiyuki; Hosayama, Kai; Tokunaga, Mai; Maegawa, Kimio; Abe, Shinsuke

    2001-11-01

    Ham-band Radio Observation (HRO) is one of the observational techniques for the forward scatter observation of meteors. We observe the meteor echo with two-element loop antennas (F/B ratio is 10 dB) at the Nagano National College of Technology (Nagano, Japan) using the continuous transmission of beacon signals for meteor observations at 53.750 MHz, 50W from Fukui National College of Technology (Fukui, Japan). To prove that the radio echo is really the echo due to meteor, we have constructed the direction determination system using the paired antennas that can detect the direction roughly where the radio echo come from. The direction of one of this paired antennas was West toward Sabae and the other was East which has proved to be the most sensitive for this research. Using this system, we detected the change of the direction of reflection point of meteor radio signal of Geminids in 2000; from the westward to eastward before and after the culmination of the radiant which is consistent the formula of reflection point of meteors. At the same time, we detected the change of an intensity and a trend of the Doppler shift of meteor echoes. This result is consistent of the meteor wind data of MU Rader of Radio Science Center for Space & Atmosphere (RASC), Kyoto University.

  5. Don Quixote - a possible parent body of a meteor shower

    NASA Astrophysics Data System (ADS)

    Rudawska, Regina; Vaubaillon, Jérémie

    2014-02-01

    Here we are interested in whether the meteoroid stream of (3552) Don Quixote can generate some observed meteor showers. We have showed that particles originating from Don Quixote particles produce two meteor showers at Earth: Kappa Lyrids and August Mu Draconids.

  6. Meteor trails observed by the Sloan Digital Sky Survey

    NASA Astrophysics Data System (ADS)

    Cikota, A.; Bektešević, D.; Cikota, S.; Weaver, B.; Jevremović, D.; Vinković, D.

    2014-07-01

    Scientific observation of meteors is not simple because they have large angular size and random appearance in time and position on the sky. Bright meteors can be easily observed by naked eye or by video cameras in low resolution, but the luminosity distribution of meteors at their fainter end, the actual column diameter of the radiating zone, meteor fragmentation and the microstructure of lightcurves (especially when a meteor is detected through several color filters, as it happened in SDSS) is not well investigated. However, wide-field surveys, such as SDSS or the future LSST, with long time coverage over a significant fraction of sky might be helpful in collecting a scientifically relevant sample of low-brightness meteors. We used a custom designed Python script to detect linear features in SDSS images. The detection is performed in two steps: 1) we detect stars with Source Extractor [1] and blend them out; 2) we define a threshold so as to analyze 10000 points over the threshold; 3) we apply RANSAC [2] to detect points forming a line. We detected trails in over 15000 calibrated and sky-subtracted ''frame'' images in two filters so far. The drift scan in imaging survey mode of SDSS enables simple distinction between "apparently fast" meteors and other "slow" linear features caused by satellites and space debris, so that around 4000 frames could be eliminated as obvious satellites. Here we discuss the detection method, show some interesting preliminary results of the analysis of detected meteors, and discuss implications for other surveys.

  7. Goals, technique and equipment of meteor study in Russia

    NASA Astrophysics Data System (ADS)

    Kartashova, A.; Bagrov, A. V.; Bolgova, G. T.; Kruchkov, S. V.; Leonov, V. A.; Mazurov, V. A.

    2013-09-01

    Institute of Astronomy RAS is one of the science institutes in the Russian Federation providing systematic optical meteor observations and supervises several meteor groups in our country. The main tasks of our investigations are dedicated to study meteoroid nature as well as meteoroid streams and meteoroid population in the Solar System. In the XXI century we in Russia carry out the reconstruction of our meteor astronomy due to possibilities of new meteor observation equipment (more powerful than were used before as visual and photographic methods) had made possible to select more interesting goals. First of our task is investigation of meteoroid streams crossing the Earth's orbit, and character of meteoroid distributions along of them. The multi stations meteor monitoring from located in the both hemispheres of the Earth can help in this study. According to the analysis of the evolution of meteor orbits, the compact and long lived meteoroid streams consist mainly from large particles. The observation equipment (cheap TV-cameras) with low limiting magnitude we use for gathering observational data. On the other hand, the observations of weak meteors are needed for new meteor shower indication (or confirmation of known meteor shower). The more effective way to do it is comparison of individual meteor orbits parameters (then calculation of radiants of meteor showers). The observations of space debris (as the meteors with low velocity - less 11.2 km/s) can be taking up within this task. The combination of high sensitive TV-cameras WATEC and super-fast lenses COMPUTAR are widely used for meteor TV-monitoring. The TVsystems for round-year meteor observations are fixed and are permanently oriented to the zenith area (the patrol camera - PatrolCa). The mobile TV-cameras (MobileCa) are used for double station observations (if it is possible) and located not far from main cameras PatrolCa (20-30 km). The mobile TVcameras observe 90% of main PatrolCa cameras FOV at altitudes

  8. Abstracts for the International Conference on Asteroids, Comets, Meteors 1991

    NASA Technical Reports Server (NTRS)

    1991-01-01

    Topics addressed include: chemical abundances; asteroidal belt evolution; sources of meteors and meteorites; cometary spectroscopy; gas diffusion; mathematical models; cometary nuclei; cratering records; imaging techniques; cometary composition; asteroid classification; radio telescopes and spectroscopy; magnetic fields; cosmogony; IUE observations; orbital distribution of asteroids, comets, and meteors; solar wind effects; computerized simulation; infrared remote sensing; optical properties; and orbital evolution.

  9. Quetelet and the Discovery of the First Meteor Showers

    NASA Astrophysics Data System (ADS)

    Sauval, J.

    1997-02-01

    The contribution of Adolphe Quetelet to meteor astronomy is important. In 1836 he predicted the return of the Perseids and in 1837 he published the first catalogue of meteors. He was also an independent co-discoverer of the Orionids and the Quadrantids in 1839.

  10. Meteor Showers of the Earth-crossing Asteroids

    NASA Astrophysics Data System (ADS)

    Pulat, Babadzhanov; Gulchekhra, Kokhirova

    2015-03-01

    The results of search for meteor showers associated with the asteroids crossing the Earthfs orbit and moving on comet-like orbits are given. It was shown that among 2872 asteroids discovered till 1.01.2005 and belonging to the Apollo and Amor groups, 130 asteroids have associated meteor showers and, therefore, are the extinct cometary nuclei.

  11. EISCAT observations of meteors from the sporadic complex

    NASA Astrophysics Data System (ADS)

    Brosch, Noah; Häggström, Ingemar; Pellinen-Wannberg, Asta

    2013-10-01

    We report meteor observation with the European Incoherent Scatter Scientific Association (EISCAT) radars obtained during a continuous 24-h period in 2009 December. The period, just after the Geminid meteor shower, was selected to have no strong meteor shower activity to allow a comparison with our previous observations collected during the 2008 Geminid shower. During the 2009 run, we used the very high frequency (VHF) and ultrahigh frequency systems, but most of the results presented here were derived from the VHF data. We discuss the statistical properties of the radar echoes, their Doppler velocity and altitude distributions, their radar cross-section, etc. We concentrate, as in our previous paper, on the population of high-altitude echoes, which we clearly detect, and discuss these specifically. We recognize a few echoes with positive Doppler velocities as produced by meteoroids that presumably entered the atmosphere at ˜grazing incidence angles and were leaving it when detected by radar. We detect meteor echoes with essentially zero Doppler velocity, reported here for the first time, which we interpret as meteoroids moving almost perpendicular to the beam and producing specular reflections off the meteor trail. We discuss meteors detected with tristatic measurements for which we find bunching in azimuth and depression angle that depends on the time of the day. Finally, we report again of the lack of extreme velocity meteors, a fact that weakens significantly the claim of the existence and abundance of interstellar meteors.

  12. Comets and meteors in the beliefs of ancient mayas

    NASA Astrophysics Data System (ADS)

    Yershova, G. G.

    2001-12-01

    Data concerning the Mayan approach to comets and meteors have till now been available mostly from ethnographical and folklore sources which dealt, as a rule, with various beliefs and tokens. The studies of hieroglyphic texts of the Classic Period (AD 600-900) have proved that comets and meteors were undoubtedly known in this culture through astronomical observations and their periodicity.

  13. Dredged trachyte and basalt from kodiak seamount and the adjacent aleutian trench, alaska.

    PubMed

    Forbes, R B; Hoskin, C M

    1969-10-24

    Blocky fragments of aegirine-augite trachyte (with accompanying icerafted gravels.) were recovered from the upper slopes of Kodiak Seamount in several dredge hauls. An alkali basalt pillow segment was also dredged from a moatlike depression, at a depth of 5000 meters, near the west base of the seamount. These retrievals confirm the volcanic origin of Kodiak Seamount and further support the view of Engel, Engel, and Havens that the higher elevations of seamounts are composed of alkali basalts or related variants. PMID:17731907

  14. 76 FR 15222 - Hawaii Bottomfish and Seamount Groundfish Fisheries; Modification of Fishery Closures

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-03-21

    ... (76 FR 8330). Briefly, reducing the advance notification period for a closure of the Deep 7 bottomfish... Seamount Groundfish Fisheries; Modification of Fishery Closures AGENCY: National Marine Fisheries...

  15. Statistical self-similarity of hotspot seamount volumes modeled as self-similar criticality

    USGS Publications Warehouse

    Tebbens, S.F.; Burroughs, S.M.; Barton, C.C.; Naar, D.F.

    2001-01-01

    The processes responsible for hotspot seamount formation are complex, yet the cumulative frequency-volume distribution of hotspot seamounts in the Easter Island/Salas y Gomez Chain (ESC) is found to be well-described by an upper-truncated power law. We develop a model for hotspot seamount formation where uniform energy input produces events initiated on a self-similar distribution of critical cells. We call this model Self-Similar Criticality (SSC). By allowing the spatial distribution of magma migration to be self-similar, the SSC model recreates the observed ESC seamount volume distribution. The SSC model may have broad applicability to other natural systems.

  16. 76 FR 10524 - Hawaii Bottomfish and Seamount Groundfish Fisheries; Fishery Closure

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-02-25

    ...) of Deep 7 bottomfish (75 FR 53606; September 1, 2010). Progress toward the TAC was monitored using... Seamount Groundfish Fisheries; Fishery Closure AGENCY: National Marine Fisheries Service (NMFS),...

  17. Ocean eddies generated by seamounts in the north pacific.

    PubMed

    Royer, T C

    1978-03-10

    Small-scale (diameters of about 37 kilometers) fluctuations in dynamic topography north of Hawaii along 158 degrees W are well correlated with upstream seamounts. The fluctuations are subsurface but are manifested as baroclinic eddies at the sea surface. These eddies are confirmed by direct observations and supported by theoretical considerations. The eddies cause small-scale variability in the currents and hydrographic structures in this area, and they should be considered in any sampling programs of the region.

  18. THE RETURN OF THE ANDROMEDIDS METEOR SHOWER

    SciTech Connect

    Wiegert, Paul A.; Brown, Peter G.; Weryk, Robert J.; Wong, Daniel K.

    2013-03-15

    The Andromedid meteor shower underwent spectacular outbursts in 1872 and 1885, producing thousands of visual meteors per hour and described as ''stars fell like rain'' in Chinese records of the time. The shower originates from comet 3D/Biela whose disintegration in the mid-1800's is linked to the outbursts, but the shower has been weak or absent since the late 19th century. This shower returned in 2011 December with a zenithal hourly rate of approximately 50, the strongest return in over a hundred years. Some 122 probable Andromedid orbits were detected by the Canadian Meteor Orbit Radar while one possible brighter Andromedid member was detected by the Southern Ontario Meteor Network and several single station possible Andromedids by the Canadian Automated Meteor Observatory. The shower outburst occurred during 2011 December 3-5. The radiant at R.A. +18 Degree-Sign and decl. +56 Degree-Sign is typical of the ''classical'' Andromedids of the early 1800s, whose radiant was actually in Cassiopeia. Numerical simulations of the shower were necessary to identify it with the Andromedids, as the observed radiant differs markedly from the current radiant associated with that shower. The shower's orbital elements indicate that the material involved was released before 3D/Biela's breakup prior to 1846. The observed shower in 2011 had a slow geocentric speed (V{sub G} = 16 km s{sup -1}) and was comprised of small particles: the mean measured mass from the radar is {approx}5 Multiplication-Sign 10{sup -7} kg, corresponding to radii of 0.5 mm at a bulk density of 1000 kg m{sup -3}. Numerical simulations of the parent comet indicate that the meteoroids of the 2011 return of the Andromedids shower were primarily ejected during 3D/Biela's 1649 perihelion passage. The orbital characteristics, radiant, and timing as well as the absence of large particles in the streamlet are all broadly consistent with simulations. However, simulations of the 1649 perihelion passage necessitate going

  19. Subsidence and flexure along the Pratt-Welker seamount chain

    NASA Astrophysics Data System (ADS)

    Lambeck, K.; Penney, C. L.; Nakiboglu, S. M.; Coleman, R.

    1984-02-01

    A geophysical examination of the degree of isostatic compensation of guyots in the Pratt-Welker seamount chain in the Gulf of Alaska is presented in order to test the hypothesis of several previous studies that the origin of the Pratt-Welker chain cannot be attributed to a single cause. The test is carried out using GEOS 3 and Seasat altimeter data. The effective flexural rigidity of the lithosphere below all the seamounts in the chain is found to be less than about 10 to the 20th Nm, such that the isostatic state is local rather than regional. This may be the result of all seamounts having formed on an initially weak lithosphere. The subsidence of guyots in the chain is associated with numerous factors including thermal contraction of the seafloor, sediment loading, the flexure of the lithosphere prior to its subduction along the Aleutian Trench, and stress relaxation. The conclusions from the flexure and subsidence analyses are in agreement with the bulk of data from previous studies of the area.

  20. Diurnal variation of overdense meteor echo duration and ozone

    NASA Technical Reports Server (NTRS)

    Simek, Milos

    1992-01-01

    The diurnal variation of the median duration of overdense sporadic radar meteor echoes is examined. The meteors recorded in August, December, and January by the Ondrejov meteor radar during the period 1958-1990 were used for the analysis. A maximum median echo duration 1-3 hours after the time of local sunrise in the meteor region confirms the already known sunrise effect. Minimum echo duration occurring at the time of sunset seems to be the most important point of diurnal variation of the echo duration, when ozone is no longer dissociated by solar UV radiation. The effect of diurnal changes of the echo duration should be considered when the mass distribution of meteor showers is analyzed.

  1. Determination of the structure of meteor showers from radar observations.

    NASA Astrophysics Data System (ADS)

    Kolomiets, S. V.; Milyutchenko, I. A.

    1995-08-01

    A method for the determination of the parameter s for meteor mass distribution and meteor shower number density from radar measurements of meteor quantities during shower activities is considered. The data from radar observations of η Aquarids and Orionids in Khar'kov in 1986 are analyzed with this method. For the duration of both showers, the maximum activity of the parameter s is found to be equal to 1.65. The dependencies of the number densities of the meteor showers and of the parameter s on the solar longitude and the time of observation are also derived. The mean number density of meteor bodies with M ≥ 10-3g is equal to 2.9×10-11m-2s-1 for the η Aquarids and 2.5×10-11m-2s-1 for the Orionids.

  2. Multi-station Video Orbits of Minor Meteor Showers

    NASA Astrophysics Data System (ADS)

    Madiedo, José M.; Trigo-Rodríguez, Josep M.

    2008-06-01

    During 2006 the SPanish Meteor Network (SPMN) set up three automated video stations in Andalusia for increasing the atmospheric coverage of the already existing low-scan-rate all-sky CCD systems. Despite their initially thought complementary nature, sensitive video cameras have been employed to setup an automatic meteor detection system that provides valuable real-time information on unusual meteor activity, and remarkable fireball events. In fact, during 2006 SPMN video stations participated in the detection of two unexpected meteor outbursts: Orionids and Comae Berenicids. The three new SPMN stations guarantee almost a continuous monitoring of meteor and fireball activity in Andalusia (Spain) and also increase the chance of future meteorite recoveries. A description of the main characteristics of these new observing video stations and some examples of the trajectory, radiant and orbital data obtained so far are presented here.

  3. Meteor showers of comet C/1917 F1 Mellish

    NASA Astrophysics Data System (ADS)

    Vereš, P.; Kornoš, L.; Tóth, J.

    2011-03-01

    December Monocerotids and November Orionids are weak but established annual meteor showers active throughout November and December. Analysis of a high quality orbits subset of the SonotaCo video meteor data base shows that the distribution of orbital elements, geocentric velocity and also the orbital evolution of the meteors and potential parent body may imply a common origin for these meteors coming from the parent comet C/1917 F1 Mellish. This is also confirmed by the physical properties and activity of these shower meteors. An assumed release of meteoroids at the perihelion of the comet in the past and the sky-plane radiant distribution reveal that the December Monocerotid stream might be younger than the November Orionids. A meteoroid transversal component of ejection velocity at the perihelion must be larger than 100 m s-1. A few authors have also associated December Canis Minorids with the comet C/1917 F1 Mellish. However, we did not find any connection.

  4. A processing method and results of meteor shower radar observations

    NASA Technical Reports Server (NTRS)

    Belkovich, O. I.; Suleimanov, N. I.; Tokhtasjev, V. S.

    1987-01-01

    Studies of meteor showers permit the solving of some principal problems of meteor astronomy: to obtain the structure of a stream in cross section and along its orbits; to retrace the evolution of particle orbits of the stream taking into account gravitational and nongravitational forces and to discover the orbital elements of its parent body; to find out the total mass of solid particles ejected from the parent body taking into account physical and chemical evolution of meteor bodies; and to use meteor streams as natural probes for investigation of the average characteristics of the meteor complex in the solar system. A simple and effective method of determining the flux density and mass exponent parameter was worked out. This method and its results are discussed.

  5. First results on video meteors from Crete, Greece

    NASA Astrophysics Data System (ADS)

    Maravelias, G.

    2012-01-01

    This work presents the first systematic video meteor observations from a, forthcoming permanent, station in Crete, Greece, operating as the first official node within the International Meteor Organization's Video Network. It consists of a Watec 902 H2 Ultimate camera equipped with a Panasonic WV-LA1208 (focal length 12mm, f/0.8) lens running MetRec. The system operated for 42 nights during 2011 (August 19-December 30, 2011) recording 1905 meteors. It is significantly more performant than a previous system used by the author during the Perseids 2010 (DMK camera 21AF04.AS by The Imaging Source, CCTV lens of focal length 2.8 mm, UFO Capture v2.22), which operated for 17 nights (August 4-22, 2010) recording 32 meteors. Differences - according to the author's experience - between the two softwares (MetRec, UFO Capture) are discussed along with a small guide to video meteor hardware.

  6. The Updated IAU MDC Catalogue of Photographic Meteor Orbits

    NASA Technical Reports Server (NTRS)

    Porubcan, V.; Svoren, J.; Neslusan, L.; Schunova, E.

    2011-01-01

    The database of photographic meteor orbits of the IAU Meteor Data Center at the Astronomical Institute SAS has gradually been updated. To the 2003 version of 4581 photographic orbits compiled from 17 different stations and obtained in the period 1936-1996, additional new 211 orbits compiled from 7 sources have been added. Thus, the updated version of the catalogue contains 4792 photographic orbits (equinox J2000.0) available either in two separate orbital and geophysical data files or a file with the merged data. All the updated files with relevant documentation are available at the web of the IAU Meteor Data Center. Keywords astronomical databases photographic meteor orbits 1 Introduction Meteoroid orbits are a basic tool for investigation of distribution and spatial structure of the meteoroid population in the close surroundings of the Earth s orbit. However, information about them is usually widely scattered in literature and often in publications with limited circulation. Therefore, the IAU Comm. 22 during the 1976 IAU General Assembly proposed to establish a meteor data center for collection of meteor orbits recorded by photographic and radio techniques. The decision was confirmed by the next IAU GA in 1982 and the data center was established (Lindblad, 1987). The purpose of the data center was to acquire, format, check and disseminate information on precise meteoroid orbits obtained by multi-station techniques and the database gradually extended as documented in previous reports on the activity of the Meteor Data Center by Lindblad (1987, 1995, 1999 and 2001) or Lindblad and Steel (1993). Up to present, the database consists of 4581 photographic meteor orbits (Lindblad et al., 2005), 63.330 radar determined orbit: Harvard Meteor Project (1961-1965, 1968-1969), Adelaide (1960-1961, 1968-1969), Kharkov (1975), Obninsk (1967-1968), Mogadish (1969-1970) and 1425 video-recordings (Lindblad, 1999) to which additional 817 video meteors orbits published by Koten el

  7. Meteoric ion layers in the ionospheres of venus and mars: Early observations and consideration of the role of meteor showers

    NASA Astrophysics Data System (ADS)

    Withers, Paul; Christou, A. A.; Vaubaillon, J.

    2013-10-01

    Layers of metal ions produced by meteoroid ablation have been known in Earth's ionosphere for decades, but have only recently been discovered at Venus and Mars. Here we report the results of a search for meteoric layers in earlier datasets from Venus and Mars. We find 13 candidates at Venus in Mariner 10, Venera 9/10, and Pioneer Venus Orbiter data that augment the 18 previously identified in Venus Express data. We find 8 candidates at Mars in Mariner 7 and Mariner 9 data that augment the 71 and 10 previously identified in Mars Global Surveyor and Mars Express data, respectively. These new findings extend the ranges of conditions under which meteoric layers have been observed, support studies of the temporal variability of meteoric layers, and (for Venus) independently confirm the existence of meteoric layers. One of the proposed causes of temporal variations in the occurrence rate of meteoric layers is meteor showers. This possibility is controversial, since meteor showers have minimal observed effect on meteoric layers in Earth's ionosphere. In order to aid progress towards a resolution of this issue, we present a series of tests for this hypothesis.

  8. Meteor Crater (Barringer Meteorite Crater), Arizona: Summary of Impact Conditions

    NASA Astrophysics Data System (ADS)

    Roddy, D. J.; Shoemaker, E. M.

    1995-09-01

    -field rock and meteorite ejecta parameters, 13) Inferred and estimated cloud-rise and fall-out conditions, 14) Late-stage meteorite falls after impact, 15) Estimated damage effect ranges, 16) Erosion of crater and ejecta blanket, 17) New topographic and digital maps of crater and ejecta blanket, 18) Other. (Suggestions are welcome) This compilation will contain expanded discussions of new data as well as revised interpretations of existing information. For example in Item 1, we suggest the impacting body most likely formed during a collision in the main asteroid belt that fragmented the iron-nickel core of an asteroid some 0.5 billion years ago. The fragments remained in space until about 50,000+/-3000 yrs ago, when they were captured by the Earth's gravitational field. In Item 3, the trajectory of the impacting body is interpreted by EMS as traveling north-northwest at a relatively low impact angle. The presence of both shocked meteorite fragments and melt spherules indicate the meteorite had a velocity in the range of about 13 to 20 km/s, probably in the lower part of this range [4]. In Item 4, the coherent meteorite diameter is estimated to have been 45 to 50 m with a mass of 300,000 to 400,000 tons, i.e., large enough to experience less than 1% in both mass ablation and velocity deceleration. During this time, minor flake-off of the meteorite's exterior produced a limited number of smaller fragments that followed the main mass to the impact site but at greatly reduced velocities. In Item 6, we estimate the kinetic energy of impact to be in the range of 20 to 40 Mt depending on the energy coupling functions used and corrections for angle of oblique impact. At impact, terrain conditions were about as we see them today, a gently rolling plain with outcrops of Moenkopi and a meter or so of soil cover. In Item 18, EMS estimates production of a Meteor Crater-size event should occur on the continents about every 50,000 years; interestingly, this is the age of Meteor Crater

  9. Is there a seamount effect on microbial community structure and biomass? The case study of Seine and Sedlo seamounts (northeast Atlantic).

    PubMed

    Mendonça, Ana; Arístegui, Javier; Vilas, Juan Carlos; Montero, Maria Fernanda; Ojeda, Alicia; Espino, Minerva; Martins, Ana

    2012-01-01

    Seamounts are considered to be "hotspots" of marine life but, their role in oceans primary productivity is still under discussion. We have studied the microbial community structure and biomass of the epipelagic zone (0-150 m) at two northeast Atlantic seamounts (Seine and Sedlo) and compared those with the surrounding ocean. Results from two cruises to Sedlo and three to Seine are presented. Main results show large temporal and spatial microbial community variability on both seamounts. Both Seine and Sedlo heterotrophic community (abundance and biomass) dominate during winter and summer months, representing 75% (Sedlo, July) to 86% (Seine, November) of the total plankton biomass. In Seine, during springtime the contribution to total plankton biomass is similar (47% autotrophic and 53% heterotrophic). Both seamounts present an autotrophic community structure dominated by small cells (nano and picophytoplankton). It is also during spring that a relatively important contribution (26%) of large cells to total autotrophic biomass is found. In some cases, a "seamount effect" is observed on Seine and Sedlo microbial community structure and biomass. In Seine this is only observed during spring through enhancement of large autotrophic cells at the summit and seamount stations. In Sedlo, and despite the observed low biomasses, some clear peaks of picoplankton at the summit or at stations within the seamount area are also observed during summer. Our results suggest that the dominance of heterotrophs is presumably related to the trapping effect of organic matter by seamounts. Nevertheless, the complex circulation around both seamounts with the presence of different sources of mesoscale variability (e.g. presence of meddies, intrusion of African upwelling water) may have contributed to the different patterns of distribution, abundances and also changes observed in the microbial community. PMID:22279538

  10. Is there a seamount effect on microbial community structure and biomass? The case study of Seine and Sedlo seamounts (northeast Atlantic).

    PubMed

    Mendonça, Ana; Arístegui, Javier; Vilas, Juan Carlos; Montero, Maria Fernanda; Ojeda, Alicia; Espino, Minerva; Martins, Ana

    2012-01-01

    Seamounts are considered to be "hotspots" of marine life but, their role in oceans primary productivity is still under discussion. We have studied the microbial community structure and biomass of the epipelagic zone (0-150 m) at two northeast Atlantic seamounts (Seine and Sedlo) and compared those with the surrounding ocean. Results from two cruises to Sedlo and three to Seine are presented. Main results show large temporal and spatial microbial community variability on both seamounts. Both Seine and Sedlo heterotrophic community (abundance and biomass) dominate during winter and summer months, representing 75% (Sedlo, July) to 86% (Seine, November) of the total plankton biomass. In Seine, during springtime the contribution to total plankton biomass is similar (47% autotrophic and 53% heterotrophic). Both seamounts present an autotrophic community structure dominated by small cells (nano and picophytoplankton). It is also during spring that a relatively important contribution (26%) of large cells to total autotrophic biomass is found. In some cases, a "seamount effect" is observed on Seine and Sedlo microbial community structure and biomass. In Seine this is only observed during spring through enhancement of large autotrophic cells at the summit and seamount stations. In Sedlo, and despite the observed low biomasses, some clear peaks of picoplankton at the summit or at stations within the seamount area are also observed during summer. Our results suggest that the dominance of heterotrophs is presumably related to the trapping effect of organic matter by seamounts. Nevertheless, the complex circulation around both seamounts with the presence of different sources of mesoscale variability (e.g. presence of meddies, intrusion of African upwelling water) may have contributed to the different patterns of distribution, abundances and also changes observed in the microbial community.

  11. Meteoric cosmogenic Beryllium-10 adsorbed to river sediment and soil: Applications for Earth-surface dynamics

    NASA Astrophysics Data System (ADS)

    Willenbring, Jane K.; von Blanckenburg, Friedhelm

    2010-01-01

    Rainfall scavenges meteoric cosmogenic 10Be from the atmosphere. 10Be falls to the Earth's surface, where it binds tightly to sediment particles in non-acidic soils over the life-span of those soils. As such, meteoric 10Be has the potential to be an excellent geochemical tracer of erosion and stability of surfaces in a diverse range of natural settings. Meteoric 10Be has great potential as a recorder of first-order erosion rates and soil residence times. Even though this tracer was first developed in the late 1980s and showed great promise as a geomorphic tool, it was sidelined in the past two decades with the rise of the "sister nuclide", in situ10Be, which is produced at a known rate inside quartz minerals. Since these early days, substantial progress has been made in several areas that now shed new light on the applicability of the meteoric variety of this cosmogenic nuclide. Here, we revisit the potential of this tracer and we summarize the progress: (1) the atmospheric production and fallout is now described by numeric models, and agrees with present-day measurements and paleo-archives such as from rain and ice cores; (2) short-term fluctuations in solar modulation of cosmic rays or in the delivery of 10Be are averaged out over the time scale soils accumulate; (3) in many cases, the delivery of 10Be is not dependent on the amount of precipitation; (4) we explore where 10Be is retained in soils and sediment; (5) we suggest a law to account for the strong grain-size dependence that controls adsorption and the measured nuclide concentrations; and (6) we present a set of algebraic expressions that allows calculation of both soil or sediment ages and erosion rates from the inventory of meteoric 10Be distributed through a vertical soil column. The mathematical description is greatly simplified if the accumulation of 10Be is at a steady state with its export through erosion. In this case, a surface sample allows for the calculation of an erosion rate. Explored

  12. A study of meteor spectroscopy and physics from earth-orbit: A preliminary survey into ultraviolet meteor spectra

    NASA Technical Reports Server (NTRS)

    Meisel, D. D.

    1976-01-01

    Preliminary data required to extrapolate available meteor physics information (obtained in the photographic, visual and near ultraviolet spectral regions) into the middle and far ultraviolet are presented. Wavelength tables, telluric attenuation factors, meteor rates, and telluric airglow data are summarized in the context of near-earth observation vehicle parameters using moderate to low spectral resolution instrumentation. Considerable attenuation is given to the problem of meteor excitation temperatures since these are required to predict the strength of UV features. Relative line intensities are computed for an assumed chondritic composition. Features of greatest predicted intensities, the major problems in meteor physics, detectability of UV meteor events, complications of spacecraft motion, and UV instrumentation options are summarized.

  13. Petrogenesis of Near-Ridge Seamounts: AN Investigation of Mantle Source Heterogeneity and Melting Processes

    NASA Astrophysics Data System (ADS)

    Baxter, N. L.; Perfit, M. R.; Lundstrom, C.; Clague, D. A.

    2010-12-01

    Near-ridge (NR) seamounts offer an important opportunity to study lavas that have similar sources to ridge basalts but have been less affected by fractionation and homogenization that takes place at adjacent spreading ridge axes. By studying lavas erupted at these off-axis sites, we have the potential to better understand source heterogeneity and melting and transport processes that can be applied to the ridge system as a whole. One purpose of our study is to investigate the role of dunite conduits in the formation of near-ridge seamount chains. We believe that near-ridge seamounts could form due to focusing of melts in dunite channels located slightly off-axis and that such conduits may be important in the formation and transport of melt both on- and off-axis (Lundstrom et al., 2000). New trace element and isotopic analyses of glasses from Rogue, Hacksaw, and T461 seamounts near the Juan de Fuca Ridge (JdFR), the Lamont Seamounts adjacent to the East Pacific Rise (EPR) ~ 10°N, and the Vance Seamounts next to the JdFR ~45°N provide a better understanding of the petrogenesis of NR seamounts. Our data indicate that lavas from these seamounts have diverse incompatible trace element compositions that range from highly depleted to slightly enriched in comparison to associated ridge basalts. Vance A lavas (the oldest in the Vance chain) have the most enriched signatures and lavas from Rogue seamount on the JdFR plate have the most depleted signatures. Sr-Nd-Pb isotopic ratios indicate that NR seamount lava compositions vary within the chains as well as within individual seamounts, and that there is some mixing between heterogeneous, small-scale mantle sources. Using the program PRIMELT2.XLS (Herzberg and Asimow, 2008), we calculated mantle potential temperatures (Tp) for some of the most primitive basalts erupted at these seamounts. Our data indicate that NR seamount lavas have Tp values that are only slightly higher than that of average ambient mantle. Variations in

  14. Organic matter composition and macrofaunal diversity in sediments of the Condor Seamount (Azores, NE Atlantic)

    NASA Astrophysics Data System (ADS)

    Bongiorni, Lucia; Ravara, Ascensão; Parretti, Paola; Santos, Ricardo S.; Rodrigues, Clara F.; Amaro, Teresa; Cunha, Marina R.

    2013-12-01

    In recent years increasing knowledge has been accumulated on seamounts ecology; however their sedimentary environments and associated biological communities remain largely understudied. In this study we investigated quantity and biochemical composition of organic matter and macrofaunal diversity in sediments of the Condor Seamount (NE Atlantic, Azores). In order to test the effect of the seamount on organic matter distribution, sediment samples were collected in 6 areas: the summit, the northern and southern flanks and bases, and in an external far field site. Macrofauna abundance and diversity were investigated on the summit, the southern flank and in the far field site. The organic matter distribution reflected the complex hydrodynamic conditions occurring on the Condor. Concentrations of organic matter compounds were generally lower on the whole seamount than in the far field site and on the seamount summit compared to flanks and bases. A clear difference was also evident between the northern and southern slopes of the Condor, suggesting a role of the seamount in conditioning sedimentation processes and distribution of food resources for benthic consumers. Macrofauna assemblages changed significantly among the three sampling sites. High abundance and dominance, accompanied by low biodiversity, characterized the macrofauna community on the Condor summit, while low dominance and high biodiversity were observed at the flank. Our results, although limited to five samples on the seamount and two off the seamount, do not necessarily support the paradigm that seamounts are more biodiverse than the surrounding seafloor. However, the abundance (and biomass), functional diversity and taxonomical distinctiveness of the macrofaunal assemblages from the Condor Seamount suggest that seamounts habitats may play a relevant role in adding to the regional biodiversity.

  15. Comet Machholz and the Quadrantid meteor stream

    NASA Astrophysics Data System (ADS)

    Jones, J.; Jones, W.

    1993-04-01

    Until quite recently, the Quadrantid meteor stream was considered to be an 'orphan'. Because of the difficulty in accounting for the large difference in the longitudes of the ascending nodes, McIntosh (1990) suggested that Comet Machholz and the stream have a sibling rather than a parent-child relationship. Gonczi et al. (1992) proposed that gravitational perturbations by Jupiter may be amplified sufficiently by the 2:1 resonance of the stream with Jupiter to explain the difference in the longitudes of ascending nodes if the stream was born when the comet's perihelion distance was last at its minimum about 4000 yr ago. In this paper, we show by computer simulations that, if the comet was captured at its last close approach with Jupiter about 2200 yr ago, there has been sufficient time for the resulting stream to produce most of the features of the presently observed Quadrantid/Arietid/Southern Delta-Aquarid complex.

  16. Asteroids in the Eccentrids meteor system

    NASA Astrophysics Data System (ADS)

    Terentjeva, A. K.; Barabanov, S. I.

    2016-09-01

    Among 11 673 of near-Earth objects (NEOs), 52 asteroids are identified, which, together with the Eccentrids meteor system, comprise a single population of small bodies of the Solar System with the smallest orbits of high eccentricity. Some features of this unique system of bodies are discussed in this paper. The distribution of perihelion longitudes is studied for the given group of asteroids and compared to that of the Aten asteroids, which are the most similar to the Eccentrids. The dependence is obtained of the character of perihelion longitude distribution on the eccentricities of the NEO orbits. Eight asteroid stream of the Eccentrids are found. The Eccentrids asteroids approaching the Earth's orbit along its whole length in their aphelia can pose a certain hazard for the Earth.

  17. Changes in nematode communities in different physiographic sites of the condor seamount (north-East atlantic ocean) and adjacent sediments.

    PubMed

    Zeppilli, Daniela; Bongiorni, Lucia; Serrão Santos, Ricardo; Vanreusel, Ann

    2014-01-01

    Several seamounts are known as 'oases' of high abundances and biomass and hotspots of biodiversity in contrast to the surrounding deep-sea environments. Recent studies have indicated that each single seamount can exhibit a high intricate habitat turnover. Information on alpha and beta diversity of single seamount is needed in order to fully understand seamounts contribution to regional and global biodiversity. However, while most of the seamount research has been focused on summits, studies considering the whole seamount structure are still rather poor. In the present study we analysed abundance, biomass and diversity of nematodes collected in distinct physiographic sites and surrounding sediments of the Condor Seamount (Azores, North-East Atlantic Ocean). Our study revealed higher nematode biomass in the seamount bases and values 10 times higher in the Condor sediments than in the far-field site. Although biodiversity indices did not showed significant differences comparing seamount sites and far-field sites, significant differences were observed in term of nematode composition. The Condor summit harboured a completely different nematode community when compared to the other seamount sites, with a high number of exclusive species and important differences in term of nematode trophic diversity. The oceanographic conditions observed around the Condor Seamount and the associated sediment mixing, together with the high quality of food resources available in seamount base could explain the observed patterns. Our results support the hypothesis that seamounts maintain high biodiversity through heightened beta diversity and showed that not only summits but also seamount bases can support rich benthic community in terms of standing stocks and diversity. Furthermore functional diversity of nematodes strongly depends on environmental conditions link to the local setting and seamount structure. This finding should be considered in future studies on seamounts, especially in

  18. Changes in nematode communities in different physiographic sites of the condor seamount (north-East atlantic ocean) and adjacent sediments.

    PubMed

    Zeppilli, Daniela; Bongiorni, Lucia; Serrão Santos, Ricardo; Vanreusel, Ann

    2014-01-01

    Several seamounts are known as 'oases' of high abundances and biomass and hotspots of biodiversity in contrast to the surrounding deep-sea environments. Recent studies have indicated that each single seamount can exhibit a high intricate habitat turnover. Information on alpha and beta diversity of single seamount is needed in order to fully understand seamounts contribution to regional and global biodiversity. However, while most of the seamount research has been focused on summits, studies considering the whole seamount structure are still rather poor. In the present study we analysed abundance, biomass and diversity of nematodes collected in distinct physiographic sites and surrounding sediments of the Condor Seamount (Azores, North-East Atlantic Ocean). Our study revealed higher nematode biomass in the seamount bases and values 10 times higher in the Condor sediments than in the far-field site. Although biodiversity indices did not showed significant differences comparing seamount sites and far-field sites, significant differences were observed in term of nematode composition. The Condor summit harboured a completely different nematode community when compared to the other seamount sites, with a high number of exclusive species and important differences in term of nematode trophic diversity. The oceanographic conditions observed around the Condor Seamount and the associated sediment mixing, together with the high quality of food resources available in seamount base could explain the observed patterns. Our results support the hypothesis that seamounts maintain high biodiversity through heightened beta diversity and showed that not only summits but also seamount bases can support rich benthic community in terms of standing stocks and diversity. Furthermore functional diversity of nematodes strongly depends on environmental conditions link to the local setting and seamount structure. This finding should be considered in future studies on seamounts, especially in

  19. Changes in Nematode Communities in Different Physiographic Sites of the Condor Seamount (North-East Atlantic Ocean) and Adjacent Sediments

    PubMed Central

    Zeppilli, Daniela; Bongiorni, Lucia; Serrão Santos, Ricardo; Vanreusel, Ann

    2014-01-01

    Several seamounts are known as ‘oases’ of high abundances and biomass and hotspots of biodiversity in contrast to the surrounding deep-sea environments. Recent studies have indicated that each single seamount can exhibit a high intricate habitat turnover. Information on alpha and beta diversity of single seamount is needed in order to fully understand seamounts contribution to regional and global biodiversity. However, while most of the seamount research has been focused on summits, studies considering the whole seamount structure are still rather poor. In the present study we analysed abundance, biomass and diversity of nematodes collected in distinct physiographic sites and surrounding sediments of the Condor Seamount (Azores, North-East Atlantic Ocean). Our study revealed higher nematode biomass in the seamount bases and values 10 times higher in the Condor sediments than in the far-field site. Although biodiversity indices did not showed significant differences comparing seamount sites and far-field sites, significant differences were observed in term of nematode composition. The Condor summit harboured a completely different nematode community when compared to the other seamount sites, with a high number of exclusive species and important differences in term of nematode trophic diversity. The oceanographic conditions observed around the Condor Seamount and the associated sediment mixing, together with the high quality of food resources available in seamount base could explain the observed patterns. Our results support the hypothesis that seamounts maintain high biodiversity through heightened beta diversity and showed that not only summits but also seamount bases can support rich benthic community in terms of standing stocks and diversity. Furthermore functional diversity of nematodes strongly depends on environmental conditions link to the local setting and seamount structure. This finding should be considered in future studies on seamounts, especially in

  20. Meteoric Metal Layer in Mars' Atmosphere: Steady-state Flux and Meteor Showers

    NASA Astrophysics Data System (ADS)

    Crismani, Matteo; Schneider, Nicholas; Jain, Sonal; Plane, John; Diego Carrillo-Sanchez, Juan; Deighan, Justin; Stevens, Michael; Evans, Scott; Chaffin, Michael; Stewart, Ian; Jakosky, Bruce

    2016-04-01

    We report on a steady state metal ion layer at Mars produced by meteoric ablation in the upper atmosphere as observed by the Imaging Ultraviolet Spectrograph (IUVS) on MAVEN. The response of the Martian atmosphere to meteoroid influx constrains cometary activity, dust dynamics, ionospheric production at Mars and meteoric smoke may represent a site of nucleation for high altitude clouds. Using observations that span more than an Earth year, we find this layer is global and steady state, contrary to previous observations, but in accordance with predictions. IUVS observations cover a range of observation conditions, which allows us to determine the variability of the Mg+ layer seasonally and geographically. In December 2015, Mars encountered three predicted meteor showers, and analysis of these events will determine whether Mars' atmosphere responds to such events dramatically, as was the case with comet Siding Spring, or more similarly to Earth. Mg is also detected, but Mg/Mg+ less than predicted by factor >3, indicative of undetermined chemical processes in the Mars atmosphere.

  1. Meteor stream survey in the southern hemisphere using SAAMER

    NASA Astrophysics Data System (ADS)

    Janches, D.; da Silva, D.; Pifko, S.; Hormaechea, J.; Hocking, W.; Brunini, C.; Close, S.; Fritts, D.

    2014-07-01

    We present in this manuscript two meteor shower surveys in the Southern Hemisphere utilizing the Southern Argentina Agile Meteor Radar (SAAMER). SAAMER, which operates at the southern most region of South America, is a new generation SKiYMET system designed with significant differences from typical meteor radars including high transmitted power and an 8-antenna transmitting array enabling large detected rates at low zenith angles. For the first survey, we applied the statistical methodology developed by Jones and Jones (2006) to the data collected each day during 4 years and compiled the results into 1 composite representative year at 1-degree resolution in Solar Longitude. We then search for enhancements in the activity, which last for at least 3 days and evolve temporally as is expected for a meteor shower. Using this methodology, we have identified in our data 32 shower radiants, two of which were not part of the IAU commission 22 meteor shower working list (Janches et al., 2014). Recently, SAAMER's capabilities were enhanced by adding two remote stations to receive meteor forward scatter signals from meteor trails and thus enable the determination of meteoroid orbital parameters. SAAMER started recording orbits in January 2012. We also present a 1-year survey using a wavelet-transform approach (Galligan and Baggaley, 2002ab; Brown et al., 2008) of this new orbital dataset to isolate enhancements in radiant density in geocentric coordinates resulting in not only radiant information but shower orbital properties.

  2. eMeteorNews: website and PDF journal

    NASA Astrophysics Data System (ADS)

    Roggemans, P.; Kacerek, R.; Koukal, J.; Miskotte, K.; Piffl, R.

    2016-01-01

    Amateur meteor workers have always been interested to exchange information and experience. In the past this was only possible via personal contacts by letter or by specialized journals. With internet a much faster medium became available and plenty of websites, mailing lists, Facebook groups, etc., have been created in order to communicate about meteors. Today there is a wealth of meteor data circulating on internet, but the information is very scattered and not directly available to everyone. The authors have been considering how to organize an easy access to the many different meteor related publications. The best solution for the current needs of amateur meteor observers proved to be a dedicated website combined with a PDF journal, both being free available without any subscription fee or registration requirement. The authors decided to start with this project and in March 2016 the website meteornews.org has been created. A first issue of eMeteorNews was prepared in April 2016. The year 2016 will be a test period for this project. The mission statement of this project is: "Minimizing overhead and editorial constraints to assure a swift exchange of information dedicated to all fields of active amateur meteor work."

  3. A decadal survey of the Daytime Arietid meteor shower using the Canadian Meteor Orbit Radar

    NASA Astrophysics Data System (ADS)

    Bruzzone, J. S.; Brown, P.; Weryk, R. J.; Campbell-Brown, M. D.

    2015-01-01

    We present results from a 12 year survey of the Daytime Arietid meteor shower using the Canadian Meteor Orbit Radar, a VHF backscattering orbital meteor radar, covering the interval 2002-2013. This survey recorded more than 2 × 104 Daytime Arietid orbits having representative masses of 8 × 10-8 kg and sizes of ≈0.4 mm. The core activity for the Arietids is found in the range 73.5° ≤ λ⊙ ≤ 84.5° and shows a broad 4-d maximum centred near λ⊙ = 80.5° of 0.04 meteoroids km-2 h-1 producing meteors of equivalent radio magnitude of +6.5 from a mean radiant at αg = 44.9° ± 1.1°, δg = 25.5° ± 1 .0°. During the plateau of shower peak activity, the mass index of the stream reaches a minimum with s = 1.6-1.7. Contamination from another nearby shower (likely the Daytime Zeta Perseids) and/or sub-streams showing different orbits compared to the core of the stream is evident in the interval 60.5° ≤ λ⊙ ≤ 71.5°. Similar contamination beyond λ⊙ = 84.5° may be due to the Helion sporadic source. We also characterized the deceleration profiles for Daytime Arietid meteor echoes using several independent speed techniques including Fresnel pre-t0, Fresnel amplitude oscillation and time-of-flight speeds which together with modelling produced a best estimate for the stream's out-of-atmosphere speed of v∞ = 40.5 ± 0.7 km s-1. The mean radar orbit from our study is noticeably smaller in semi-major axis and eccentricity than is found for larger Arietids measured with optical systems, a difference which if real indicates a particle-size sorting of the stream orbit. The broad activity maximum, long duration of activity and particle-size dependence of the orbital elements suggest the stream is too old to have been solely formed during the breakup of the parent comet of the Marsden sunskirters about a millennium ago as proposed by Sekanina & Chodas.

  4. Fish biodiversity of the Vitória-Trindade Seamount Chain, southwestern Atlantic: an updated database.

    PubMed

    Pinheiro, Hudson T; Mazzei, Eric; Moura, Rodrigo L; Amado-Filho, Gilberto M; Carvalho-Filho, Alfredo; Braga, Adriana C; Costa, Paulo A S; Ferreira, Beatrice P; Ferreira, Carlos Eduardo L; Floeter, Sergio R; Francini-Filho, Ronaldo B; Gasparini, João Luiz; Macieira, Raphael M; Martins, Agnaldo S; Olavo, George; Pimentel, Caio R; Rocha, Luiz A; Sazima, Ivan; Simon, Thiony; Teixeira, João Batista; Xavier, Lucas B; Joyeux, Jean-Christophe

    2015-01-01

    Despite a strong increase in research on seamounts and oceanic islands ecology and biogeography, many basic aspects of their biodiversity are still unknown. In the southwestern Atlantic, the Vitória-Trindade Seamount Chain (VTC) extends ca. 1,200 km offshore the Brazilian continental shelf, from the Vitória seamount to the oceanic islands of Trindade and Martin Vaz. For a long time, most of the biological information available regarded its islands. Our study presents and analyzes an extensive database on the VTC fish biodiversity, built on data compiled from literature and recent scientific expeditions that assessed both shallow to mesophotic environments. A total of 273 species were recorded, 211 of which occur on seamounts and 173 at the islands. New records for seamounts or islands include 191 reef fish species and 64 depth range extensions. The structure of fish assemblages was similar between islands and seamounts, not differing in species geographic distribution, trophic composition, or spawning strategies. Main differences were related to endemism, higher at the islands, and to the number of endangered species, higher at the seamounts. Since unregulated fishing activities are common in the region, and mining activities are expected to drastically increase in the near future (carbonates on seamount summits and metals on slopes), this unique biodiversity needs urgent attention and management. PMID:25738798

  5. Geochemistry and petrogenesis of volcanic rocks from Daimao Seamount (South China Sea) and their tectonic implications

    NASA Astrophysics Data System (ADS)

    Yan, Quanshu; Castillo, Paterno; Shi, Xuefa; Wang, Liaoliang; Liao, Lin; Ren, Jiangbo

    2015-03-01

    The South China Sea (SCS) experienced three episodes of seafloor spreading and left three fossil spreading centers presently located at 18°N, 17°N and 15.5°N. Spreading ceased at these three locations during magnetic anomaly 10, 8, and 5c, respectively. Daimao Seamount (16.6 Ma) was formed 10 my after the cessation of the 17°N spreading center. Volcaniclastic rocks and shallow-water carbonate facies near the summit of Daimao Seamount provide key information on the seamount's geologic history. New major and trace element and Sr-Nd-Pb isotopic compositions of basaltic breccia clasts in the volcaniclastics suggest that Daimao and other SCS seamounts have typical ocean island basalt-like composition and possess a 'Dupal' isotopic signature. Our new analyses, combined with available data, indicate that the basaltic foundation of Daimao Seamount was formed through subaqueous explosive volcanic eruptions at 16.6 Ma. The seamount subsided rapidly (> 0.12 mm/y) at first, allowing the deposition of shallow-water, coral-bearing carbonates around its summit and, then, at a slower rate (< 0.12 mm/y). We propose that the parental magmas of SCS seamount lavas originated from the Hainan mantle plume. In contrast, lavas from contemporaneous seamounts in other marginal basins in the western Pacific are subduction-related.

  6. Geophysical investigation of seamounts near the Ogasawara Fracture Zone, western Pacific

    NASA Astrophysics Data System (ADS)

    Lee, T.-G.; Lee, K.; Hein, J. R.; Moon, J.-W.

    2009-03-01

    This paper provides an analysis of multi-channel seismic data obtained during 2000-2001 on seamounts near the Ogasawara Fracture Zone (OFZ) northwest of the Marshall Islands in the western Pacific. The OFZ is unique in that it is a wide rift zone that includes many seamounts. Seven units are delineated on the basis of acoustic characteristics and depth: three units (I, II, and III) on the summit of seamounts and four units (IV, V, VI, and VII) in basins. Acoustic characteristics of layers on the summit of guyots and dredged samples indicate that the seamounts had been built above sea level by volcanism. This was followed by reef growth along the summit margin, which enabled deposition of shallow-water carbonates on the summit, and finally by subsidence of the edifices. The subsidence depth of the seamounts, estimated from the lower boundary of unit II, ranges between 1,550 and 2,040 m. The thick unit I of the southern seamounts is correlated with proximity to the equatorial high productivity zone, whereas local currents may have strongly affected the distribution of unit I on northern seamounts. A seismic profile in the basin around the Ita Mai Tai and OSM4 seamounts shows an unconformity between units IV and V, which is widespread from the East Mariana Basin to the Pigafetta Basin.

  7. Fish Biodiversity of the Vitória-Trindade Seamount Chain, Southwestern Atlantic: An Updated Database

    PubMed Central

    Pinheiro, Hudson T.; Mazzei, Eric; Moura, Rodrigo L.; Amado-Filho, Gilberto M.; Carvalho-Filho, Alfredo; Braga, Adriana C.; Costa, Paulo A. S.; Ferreira, Beatrice P.; Ferreira, Carlos Eduardo L.; Floeter, Sergio R.; Francini-Filho, Ronaldo B.; Gasparini, João Luiz; Macieira, Raphael M.; Martins, Agnaldo S.; Olavo, George; Pimentel, Caio R.; Rocha, Luiz A.; Sazima, Ivan; Simon, Thiony; Teixeira, João Batista; Xavier, Lucas B.; Joyeux, Jean-Christophe

    2015-01-01

    Despite a strong increase in research on seamounts and oceanic islands ecology and biogeography, many basic aspects of their biodiversity are still unknown. In the southwestern Atlantic, the Vitória-Trindade Seamount Chain (VTC) extends ca. 1,200 km offshore the Brazilian continental shelf, from the Vitória seamount to the oceanic islands of Trindade and Martin Vaz. For a long time, most of the biological information available regarded its islands. Our study presents and analyzes an extensive database on the VTC fish biodiversity, built on data compiled from literature and recent scientific expeditions that assessed both shallow to mesophotic environments. A total of 273 species were recorded, 211 of which occur on seamounts and 173 at the islands. New records for seamounts or islands include 191 reef fish species and 64 depth range extensions. The structure of fish assemblages was similar between islands and seamounts, not differing in species geographic distribution, trophic composition, or spawning strategies. Main differences were related to endemism, higher at the islands, and to the number of endangered species, higher at the seamounts. Since unregulated fishing activities are common in the region, and mining activities are expected to drastically increase in the near future (carbonates on seamount summits and metals on slopes), this unique biodiversity needs urgent attention and management. PMID:25738798

  8. 15 CFR Appendix F to Subpart M of... - Davidson Seamount Management Zone

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 15 Commerce and Foreign Trade 3 2014-01-01 2014-01-01 false Davidson Seamount Management Zone F Appendix F to Subpart M of Part 922 Commerce and Foreign Trade Regulations Relating to Commerce and Foreign... Sanctuary Pt. 922, Subpt. M, App. F Appendix F to Subpart M of Part 922—Davidson Seamount Management...

  9. Fish biodiversity of the Vitória-Trindade Seamount Chain, southwestern Atlantic: an updated database.

    PubMed

    Pinheiro, Hudson T; Mazzei, Eric; Moura, Rodrigo L; Amado-Filho, Gilberto M; Carvalho-Filho, Alfredo; Braga, Adriana C; Costa, Paulo A S; Ferreira, Beatrice P; Ferreira, Carlos Eduardo L; Floeter, Sergio R; Francini-Filho, Ronaldo B; Gasparini, João Luiz; Macieira, Raphael M; Martins, Agnaldo S; Olavo, George; Pimentel, Caio R; Rocha, Luiz A; Sazima, Ivan; Simon, Thiony; Teixeira, João Batista; Xavier, Lucas B; Joyeux, Jean-Christophe

    2015-01-01

    Despite a strong increase in research on seamounts and oceanic islands ecology and biogeography, many basic aspects of their biodiversity are still unknown. In the southwestern Atlantic, the Vitória-Trindade Seamount Chain (VTC) extends ca. 1,200 km offshore the Brazilian continental shelf, from the Vitória seamount to the oceanic islands of Trindade and Martin Vaz. For a long time, most of the biological information available regarded its islands. Our study presents and analyzes an extensive database on the VTC fish biodiversity, built on data compiled from literature and recent scientific expeditions that assessed both shallow to mesophotic environments. A total of 273 species were recorded, 211 of which occur on seamounts and 173 at the islands. New records for seamounts or islands include 191 reef fish species and 64 depth range extensions. The structure of fish assemblages was similar between islands and seamounts, not differing in species geographic distribution, trophic composition, or spawning strategies. Main differences were related to endemism, higher at the islands, and to the number of endangered species, higher at the seamounts. Since unregulated fishing activities are common in the region, and mining activities are expected to drastically increase in the near future (carbonates on seamount summits and metals on slopes), this unique biodiversity needs urgent attention and management.

  10. 75 FR 69015 - Fisheries in the Western Pacific; Hawaii Bottomfish and Seamount Groundfish; Measures To Rebuild...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-11-10

    ... on August 30, 2010 (75 FR 52921), and is not repeated here. The public comment period for the... Pacific; Hawaii Bottomfish and Seamount Groundfish; Measures To Rebuild Overfished Armorhead at Hancock Seamounts AGENCY: National Marine Fisheries Service (NMFS), National Oceanic and Atmospheric...

  11. 15 CFR Appendix F to Subpart M of... - Davidson Seamount Management Zone

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 15 Commerce and Foreign Trade 3 2011-01-01 2011-01-01 false Davidson Seamount Management Zone F Appendix F to Subpart M of Part 922 Commerce and Foreign Trade Regulations Relating to Commerce and Foreign... Sanctuary Pt. 922, Subpt. M, App. F Appendix F to Subpart M of Part 922—Davidson Seamount Management...

  12. 15 CFR Appendix F to Subpart M of... - Davidson Seamount Management Zone

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 15 Commerce and Foreign Trade 3 2013-01-01 2013-01-01 false Davidson Seamount Management Zone F Appendix F to Subpart M of Part 922 Commerce and Foreign Trade Regulations Relating to Commerce and Foreign... Sanctuary Pt. 922, Subpt. M, App. F Appendix F to Subpart M of Part 922—Davidson Seamount Management...

  13. 15 CFR Appendix F to Subpart M of... - Davidson Seamount Management Zone

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 15 Commerce and Foreign Trade 3 2010-01-01 2010-01-01 false Davidson Seamount Management Zone F Appendix F to Subpart M of Part 922 Commerce and Foreign Trade Regulations Relating to Commerce and Foreign... Sanctuary Pt. 922, Subpt. M, App. F Appendix F to Subpart M of Part 922—Davidson Seamount Management...

  14. 15 CFR Appendix F to Subpart M of... - Davidson Seamount Management Zone

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 15 Commerce and Foreign Trade 3 2012-01-01 2012-01-01 false Davidson Seamount Management Zone F Appendix F to Subpart M of Part 922 Commerce and Foreign Trade Regulations Relating to Commerce and Foreign... Sanctuary Pt. 922, Subpt. M, App. F Appendix F to Subpart M of Part 922—Davidson Seamount Management...

  15. Data processing of solar EUV instruments on the METEOR satellite

    NASA Technical Reports Server (NTRS)

    Brown, Hipook

    1995-01-01

    The Multiple Experiment Transporter into Earth Orbit and Return-Solar EUV Experiment (METEOR-SEE) project will take daily extreme ultraviolet (EUV) irradiance spectra starting in the summer of 1995. The METEOR-SEE package consists of an EUV grating spectrograph (EGS) and a cluster of 5 soft x-ray photometers (XP's). Both these instruments have flown previously on NASA sounding rockets. Because of the scope of the project, new data processing algorithms had to be developed for the SEE instruments onboard the METEOR satellite. An overview of the data flow describes how satellite data are collected and processed. Detailed descriptions of specific routines will show what data processing entails.

  16. [Pathogenetic basis and therapeutic management of meteorism (author's transl)].

    PubMed

    Hafter, E

    1980-09-01

    Meteorism might be a symptom of organic intestinal obstruction, which needs surgical treatment in most cases. However it is often a functional phenomenon. It may be produced by aerophagy, followed by sonor, non fetid flatulence. Large amounts of gas are produced by the contact of gastric acidity with alcaline pancreatic secretion and by enzymatic digestion of food. Most of these gases are absorbed by the intestine and exhaled. In the colon bacterial fermentation and putrefaction produce fetid gas which is expulsed as flatus. Overeating, bacterial invasion of the small intestin, inflammatory and circulatory disturbances of the small bowel and obstipation favour meteorism. The treatment depends of the origin of meteorism.

  17. Double station observation of faint meteors in Nikolaev

    NASA Astrophysics Data System (ADS)

    Kulichenko, Mykola; Shulga, Alexandr; Sybiryakova, Yevgeniya

    2016-07-01

    Meteor research using TV CCD unintensified techniques was started in 2011 in Nikolaev astronomical observatory (RI NAO). The method of meteor registration is based on combined observation method developed at RI NAO. The main accent of the research is made on precise astrometry and meteoroid orbits calculation. In 2013 first double station meteors with low baseline were observed. The accuracy of visible radiant estimation is 0.7" with baseline 5 km, and less 0.5" with baseline 11.8 km. The accuracy of velocity and height estimation is 0.5 km/s and 1-2 km.

  18. Particle-based ablation model for faint meteors

    NASA Astrophysics Data System (ADS)

    Stokan, E.; Campbell-Brown, M.

    2014-07-01

    Modeling the ablation of meteoroids as they enter the atmosphere is a way of determining their physical structure and elemental composition. This can provide insight into the structure of parent bodies when combined with an orbit computed from observations. The Canadian Automated Meteor Observatory (CAMO) is a source of new, high-resolution observations of faint meteors [1]. These faint objects tend to have pre-atmospheric masses around 10^{-5} kg, corresponding to a radius of 1 mm. A wide-field camera with a 28° field of view provides guidance to a high-resolution camera that tracks meteors in flight with 1.5° field of view. Meteors are recorded with a scale of 4 m per pixel at a range of 135 km, at 110 frames per second, allowing us to investigate detailed meteor morphology. This serves as an important new constraint for ablation models, in addition to meteor brightness (lightcurves) and meteoroid deceleration. High-resolution observations of faint meteors have revealed that contemporary ablation models are not able to predict meteor morphology, even while matching the observed lightcurve and meteoroid deceleration [2]. This implies that other physical processes, in addition to fragmentation, must be considered for faint meteor ablation. We present a new, particle-based approach to modeling the ablation of small meteoroids. In this model, we simulate the collisions between atmospheric particles and the meteoroid to determine the rate of evaporation and deceleration. Subsequent collisions simulated between evaporated meteoroid particles and ambient atmospheric particles then produce light that would be observed by high-resolution cameras. Preliminary results show simultaneous agreement with meteor morphology, lightcurves, and decelerations recorded with CAMO. A sample comparison of simulated and observed meteor morphology is given in the attached figure. Several meteoroids are well-represented as solid, stony bodies, but some require modeling as a dustball [3

  19. New insights into asteroid 3200 Phaethon's meteor complex

    NASA Astrophysics Data System (ADS)

    Jakubik, Marian; Neslusan, Lubos

    2015-11-01

    In this work, we study the meteor complex originating from asteroid 3200 Phaethon. Using a modeling of variety of meteoroid streams and following their dynamical evolution, we confirm the presence of two filaments crossing the Earth observed as Geminid and Daytime Sextantid meteor showers. We use numerical integrations of modeled particles performed for several past perihelion passages of the asteroid considering (i) only the gravity of planets and (2) gravity of planets and the Poynting-Robertson effect. We present the results of comparing our models (predicted showers) with observed showers. We also point out discrepancies, their possible solutions and/or new hypothesis concerning the examined meteor complex.

  20. New approaches to some methodological problems of meteor science

    NASA Technical Reports Server (NTRS)

    Meisel, David D.

    1987-01-01

    Several low cost approaches to continuous radioscatter monitoring of the incoming meteor flux are described. Preliminary experiments were attempted using standard time frequency stations WWVH and CHU (on frequencies near 15 MHz) during nighttime hours. Around-the-clock monitoring using the international standard aeronautical beacon frequency of 75 MHz was also attempted. The techniques are simple and can be managed routinely by amateur astronomers with relatively little technical expertise. Time series analysis can now be performed using relatively inexpensive microcomputers. Several algorithmic approaches to the analysis of meteor rates are discussed. Methods of obtaining optimal filter predictions of future meteor flux are also discussed.

  1. Comet P/Machholtz and the Quadrantid meteor stream

    SciTech Connect

    Mcintosh, B.A. )

    1990-07-01

    Attention is drawn to the suggestive similarities between the calculated perturbation behavior of Comet P/Machholtz 1986 VIII, on the one hand, and on the other those of the Quadrantid, Delta Aquarid, and Arietid meteor streams. There appears to be adequate evidence for the formation by the Comets P/Machholtz and 1491-I, together with the three meteor streams, of a related complex controlled by Jupiter's gravitational perturbations; there is no comparably compelling information, however, bearing on the questions of parent-offspring or sibling relationships among these comets and meteor streams. 13 refs.

  2. Discovery of the 2011 eruption at Axial Seamount

    NASA Astrophysics Data System (ADS)

    Chadwick, B.; Nooner, S. L.; Butterfield, D. A.; Lilley, M. D.; Clague, D. A.; Caress, D. W.; Dziak, R. P.; Haxel, J. H.

    2011-12-01

    A new lava flow was discovered on the seafloor at Axial Seamount during an expedition in late July on R/V Atlantis with ROV Jason to conduct time-series monitoring and sampling. Major changes in depth, lava morphology, and the burial of pre-existing markers, monuments, and instruments made it clear that the new lava had not been there during the previous visit in August 2010. Pre-existing high-resolution bathymetry in the area aided in recognizing that the seafloor had changed significantly. The 2011 lava appears to have been erupted along the upper south rift, in a similar location to the 1998 eruption. The 2011 lava appears to be constrained by pre-existing topography to the east, but flowed at least 2 km downslope to the west, where it fills pre-existing channels and basins, and came with 170 m of the ASHES vent field near the SW caldera wall. The morphology of the 2011 lava is pillowed near the thin margins of the flows, and lobate elsewhere. The thin margins are the only places where the 2011 lava appears black, shiny, and new. Elsewhere where the lava is thicker it is covered by an orange/tan "eruption mat" (also observed after the 1998 eruption) that appears to be hydrothermal in origin, and is probably associated with cooling of the flow. In such places the 2011 lava looks deceptively "old". No collapse features were observed in the 2011 lavas, in marked contrast to the 1998 lava flow. This suggests that the 2011 eruption was longer-lived and larger in volume, consistent with the longer flow lengths. A fuller view of the extent of the 2011 lava flows will be provided by a coordinated re-survey collected with the MBARI mapping AUV on the heels of our Atlantis cruise. Hydrothermal venting on the 2011 lava flow was limited to isolated snow-blower vents and pre-existing vent sites, but we likely did not find all the sources of new venting in our limited dive time, based on the extremely poor visibility near the seafloor. CTD casts showed near bottom plumes up

  3. Deformation and faulting of subduction overriding plate caused by a subducted seamount

    NASA Astrophysics Data System (ADS)

    Ding, Min; Lin, Jian

    2016-09-01

    We conducted numerical experiments to simulate elastoplastic deformation of the overriding plate caused by a subducted seamount. Calculations revealed development of a distinct pair of fault-like shear zones, including a landward dipping forethrust fault initiated from the seamount top and a seaward dipping backthrust fault from the landward base of the seamount. Significant dome-shaped surface uplift was predicted above the thrust faults. Lesser-developed seaward dipping backthrust faults were calculated to develop under certain conditions. The overriding plate was calculated to deform in two stages: In Stage I, elastic deformation leads to the formation of fault-like shear zones. After major faults have cut through the entire plate, plastic deformation on faults dominates Stage II. On the subduction interface, compressional normal stress was calculated to increase on the landward leading flank of the seamount and decrease on the seaward trailing flank. These changes, together with associated stress singularities at seamount edges, could affect earthquake processes.

  4. The ecology of xenophyophores (Protista) on eastern Pacific seamounts

    NASA Astrophysics Data System (ADS)

    Levin, Lisa A.; Thomas, Cynthia L.

    1988-12-01

    Large, agglutinating protozoans of the class Xenophyophorea are the dominant epifaunal organisms on soft and hard substrates of many bathyal seamounts in the eastern Pacific Ocean off Mexico. Observations made with the submersible Alvin and remotely towed camera sleds on 17 seamounts at 31°, 20°, 13° and 10°N revealed more than ten distinct xenophyophore test morphologies. Most of these appear to represent previously undescribed species. Reticulate forms are numerically dominant at 20°, 13° and 10°N. Xenophyophore abundances increase with decreasing latitude, being rare at 30°N, present at densities of 0.1-1.0 m -2 at 20° and 13°N and often exceeding 1.0 m -2 at 10°N, occasionally reaching 10-18 m -2. Highest concentrations are observed on caldera floors near the base of steep caldera walls, at depths between 1700 and 2500 m. Most individuals select sand-size pelagic foraminiferan tests (63-500 μm) and exclude pebble, silt and clay-size particles for test construction. Xenophyophore on seamounts modify the structure of metazoan communities and may play a role in maintenance of infaunal diversity. Twenty-seven xenophyophore tests were found to provide habitat for 16 major macrofaunal taxa (152 individuals) and three meiofaunal taxa (333 individuals). The presence of xenophyophores also enhances the abundance of isopods, tanaids, ophiuroids, nematodes and harpacticoid copepods dwelling in sediments surrounding the tests. Mobile megafauna are attracted to sediment beneath and adjacent to xenophyophores. We suggest that xenophyophores, which are abundant on many topographic features in deep water (e.g. guyots, trenches, canyons and continental slopes), are a functionally important component of deep-sea benthic communities and require further autecological and synecological investigation.

  5. NASA Meteor Cam Video of June 2, 2016 Arizona Fireball

    NASA Video Gallery

    Video obtained from the NASA meteor camera situated at the MMT Observatory on the site of the Fred Lawrence Whipple Observatory, located on Mount Hopkins, Arizona, in the Santa Rita Mountains. Cred...

  6. Activity and observability of meteor showers throughout the year

    NASA Astrophysics Data System (ADS)

    Zimnikoval, Peter

    2014-02-01

    Diagrams on the poster present the activity periods of meteor showers as well as the rising and setting times of meteor shower radiants. Plotted are sunrises, sunsets and the period of twilight. It was constructed according to data from the IMO Meteor Shower Working List. More active showers are displayed in red and less active showers in green. The diagrams are calculated for geographic latitudes of 40° N, 0° and 40° S. The time scale is given as local time at the relevant zonal meridian and supplemented by local daylight saving time. The diagrams contain rounded values of solar longitude J2000. The star chart shows the radiant positions and drift of IMO meteor showers while the other diagrams display shower activity and date of maximum.

  7. Precession of parent bodies from historical meteor outbursts

    NASA Astrophysics Data System (ADS)

    Ahn, S.-H.

    2015-01-01

    We collect records of meteor outbursts from world-wide historical archives, and analyzed them to see which meteor outbursts have existed during the last two millennia. We calculate the dates of occurrence within the sidereal year for each record, and find four prominent major meteor streams having existed continuously. The prominent and continuous meteor streams are the Lyrids, the Perseids, the Leonids, and the eta- Aquariids/Orionids pair. We also check the regression of nodal points of these streams, and find that both the Leonids and the eta-Aquariids/Orionids pair have relatively large precession rates, while the other streams have small rates. We discuss that the near-type outbursts have occurred more frequently than the far-type outbursts.

  8. Results of the IMO Video Meteor Network - December 2012

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert; Goncalves, Rui

    2013-04-01

    A summary of the 2012 December results of the IMO Video Meteor Network is presented, based on almost 40 000 meteors collected in over 6 800 hours of observing time. Flux density profiles of the Geminids and Ursids are presented. The Geminids peaked on December 13/14 and their activity could be followed between November 30 and December 17. No activity from meteors associated with comet 46P/Wirtanen could be detected. Shower parameters for ψ-Ursae Majorids, December α-Draconids, December κ-Draconids, Comae Berenicids, ρ-Leonids, χ-Orionids, December σ-Virginids, α-Hydrids, and December χ-Virginids are presented. The 2012 IMO Video Meteor Network observations are also summarized.

  9. The Formation and Dissipation of a Meteor Coma

    NASA Astrophysics Data System (ADS)

    Kramer, E. N.; Shestaka, I. S.

    The results of reduction of instantaneous fireball photographs are presented. The observational data testify to the fact that linear dimensions of the region radiating after the meteor's flight amount to tens and hundreds of meters, and in the case of particularly bright fireballs to some kilometers. The suggested by authors hypothesis of synchronous length change of the region of fireball afterglow alongside with its light variation is verified. The analysis of the spectral photograph obtained by authors with the method of instantaneous exposure shows that the afterglow proceeds mainly to radiation in H and K lines of CaII. Several mechanisms of ionized atoms afterglow of the meteor substance are discussed. Photometric profiles of the instantaneous images of meteors are compared with theoretical calculations made both on the supposition of the parent body fragmentation and on that of afterglow of ionized atoms of meteor substance. The conclusion on a joint effect of both above-mentioned mechanisms is obtained.

  10. A Passive FPAA-Based RF Scatter Meteor Detector

    NASA Astrophysics Data System (ADS)

    Popowicz, A.; Malcher, A.; Bernacki, K.; Fietkiewicz, K.

    2015-02-01

    In the article, we present a hardware meteor detector. The detection principle is based on the electromagnetic wave reflection from the ionized meteor trail in the atmosphere. The detector uses the ANADIGM field programmable analog array (FPAA), which is an attractive alternative for typically used detecting equipment—a PC computer with dedicated software. We implement an analog signal path using most of available FPAA resources to obtain precise audio signal detection. Our new detector was verified in collaboration with the Polish Fireball Network, the organization which monitors meteor activity in Poland. When compared with currently used signal processing PC software employing real radio meteor scatter signals, our low-cost detector proved to be more precise and reliable. Due to its cost and efficiency superiority over the current solution, the presented module is going to be implemented in the planned distributed detectors system.

  11. Martian Atmospheric Methane Plumes from Meteor Shower Infall: A Hypothesis

    NASA Astrophysics Data System (ADS)

    Fries, M.; Christou, A.; Archer, D.; Conrad, P.; Cooke, W.; Eigenbrode, J.; ten Kate, I. L.; Matney, M.; Niles, P.; Sykes, M.; Steele, A.; Treiman, A.

    2016-09-01

    Methane plumes in the martian atmosphere were previously reported, but their source remains a mystery. We hypothesize a meteor shower source, as we find a correlation between Mars/cometary orbit encounters and detections of plumes.

  12. Improving Photometric Calibration of Meteor Video Camera Systems

    NASA Technical Reports Server (NTRS)

    Ehlert, Steven; Kingery, Aaron; Cooke, William

    2016-01-01

    Current optical observations of meteors are commonly limited by systematic uncertainties in photometric calibration at the level of approximately 0.5 mag or higher. Future improvements to meteor ablation models, luminous efficiency models, or emission spectra will hinge on new camera systems and techniques that significantly reduce calibration uncertainties and can reliably perform absolute photometric measurements of meteors. In this talk we discuss the algorithms and tests that NASA's Meteoroid Environment Office (MEO) has developed to better calibrate photometric measurements for the existing All-Sky and Wide-Field video camera networks as well as for a newly deployed four-camera system for measuring meteor colors in Johnson-Cousins BV RI filters. In particular we will emphasize how the MEO has been able to address two long-standing concerns with the traditional procedure, discussed in more detail below.

  13. Meteor Outbursts and Storms from the Spacecraft Hazard Perspective

    NASA Technical Reports Server (NTRS)

    Cooke, William; Moser, Danielle; Suggs, Rob

    2004-01-01

    The recent Leonid meteor storms have propelled meteor shower forecasting from an idea into the realm of practical application, invoked several times per year by numerous spacecraft. This paper will describe shower activity predictions, which give zenith hourly rate (ZHR) as a function of time, and how these are translated into spacecraft risks. Common spacecraft meteor shower mitigation strategies will also be discussed, and the important issue as to when to implement such operations considered. It should be noted that, while the recent meteor storms did not result in the loss of a vehicle, there were a few spacecraft anomalies attributed to Leonid strikes, and the nature of these will be commented upon. Finally, we assess the current state of the art in shower forecasting, and take a look "down the road" at some possible outbursts in the near future.

  14. The investigation of multiplet structures in meteor spectra

    NASA Astrophysics Data System (ADS)

    Mozgova, Alona; Churyumov, Klim

    2016-07-01

    The structures of the iron multiplets and some other elements observed in spectra of meteor comas were considered. The catalog of iron multiplets lines was made. For each term there are indicated energy levels and wavelengths of spectral lines. For clearly explaining the transitions that accompany the radiation in given multiplets the complete Grotrian diagrams were constructed. Spectral analysis has an important role in understanding the physical processes which occur in meteor comas. Each meteor spectrum contains a large number of spectral lines belonging to atoms of different chemical elements and has a multiplet structures. The multiplets are usually spaced pairs or triples of lines but the multiplet may consist of one or more lines than three. The studying of multiplet structures in meteor spectra makes it possible to investigate the properties and a behavior of atoms of the meteor body matter. It can be used for creating models of physical and chemical processes which occur during the meteor flight in the Earth's atmosphere. For some tasks of meteor physics it needs to know not only the wavelength of a line and its belonging to some multiplet, but also both the excitation potentials of the upper and lower levels. This is useful, for example, for the study of the atoms distribution over the levels and how it differs from the Boltzmann distribution, as well as for the construction of curves growth and for determining the temperature excitation in the meteor coma, etc. For this purpose, the Walt Grotrian diagrams or chart of terms are built. They show the allowed transitions between the energy levels of the atoms. These diagrams can be used for one or more electrons (multielectrons) in the atom. The specific selection rules are taken into account in their construction. These rules are related to the change in angular momentum of the electron.

  15. ESA/ESTEC Meteor Research Group - behind the scenes

    NASA Astrophysics Data System (ADS)

    Rudawska, R.

    2016-01-01

    The ESA/ESTEC Meteor Research Group consists of a team people with one goal: understand the effects of meteoric phenomena on planetary atmospheres and surfaces, as well as on spacecraft. The team carries out observational and theoretical studies in order to increase our knowledge of the small particle complex in the solar system. This talk addresses a number of tasks within the group seen from a perspective of a research fellow.

  16. Meteor Beliefs Project: Spears of GodSpears of God

    NASA Astrophysics Data System (ADS)

    Hendrix, Howard V.; McBeath, Alastair; Gheorghe, Andrei Dorian

    2012-04-01

    A selection of genuine or supposedly sky-fallen objects from real-world sources, a mixture of weapons, tools and "magical" objects of heavenly provenance, are drawn from their re-use in the near-future science-fiction novel Spears of God by author Howard V Hendrix, with additional discussion. The book includes other meteoric and meteoritic items too, some of which have been the subject of previous Meteor Beliefs Project examinations.

  17. Comet Encke: Meteor metallic ion identification by mass spectrometer

    NASA Technical Reports Server (NTRS)

    Goldberg, R. A.; Aikin, A. C.

    1973-01-01

    Positive metallic ions have been measured in the earth's atmosphere between 85 and 120 km, during the period of the beta Taurids meteor shower, which is associated with Comet Encke. The ions originate during and following ablation of extraterrestrial debris by the earth's atmosphere. The enhancement of metal ion density during meteor showers is primary evidence for their extraterrestrial origin. The present results were obtained from a rocket-borne ion mass spectrometer.

  18. Results of the IMO Video Meteor Network - November 2012

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert; Goncalves, Rui

    2013-02-01

    More than 27 000 meteors were registered by the IMO Video Meteor Network cameras in 2012 November. Flux density profiles are presented for the Leonids, Northern and Southern Taurids and compared to profiles from 2011. It is confirmed that the Southern October delta-Arietids are an early segment of the Southern Taurids. Shower parameters for November iota-Draconids, November Orionids, December Monocerotids and sigma-Hydrids are presented.

  19. On the accuracy of orbits from video meteor observations

    NASA Astrophysics Data System (ADS)

    Skokić, I.; Šegon, D.; Kurtović, G.

    2016-01-01

    The velocity limits of the meteor shower's geocentric velocity distribution from the CAMS meteoroid database were determined and used to calculate perturbed orbits. These were compared with the mean stream orbit using the DSH dissimilarity criterion. It was found that for the slow meteor showers (Alpha Capricornids and Geminids), the resulting orbits are within the generally accepted cutoff values for stream associations, while for the faster showers (Perseids, Orionids and Quadrantids) the resulting orbits differ significantly from their mean stream orbit.

  20. Results of the IMO Video Meteor Network - September 2010

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor

    2010-12-01

    In September 2010, 46 cameras of the IMO Video Meteor Network were active with more than 3 700 hours of observations and almost 19 000 meteors recorded. Minor showers active in September were explored. Activity profiles of the September epsilon-Perseids, nu-Eridanids and iota-Cassiopeiids are presented. Signs of early activity of the Orionids were searched for. A small increase could be detected from September 25, and convincing rates could be observed from September 30.

  1. Influence of meteor showers on Earth's upper atmosphere temperature

    NASA Astrophysics Data System (ADS)

    Salivonov, A.; Kozak, L.

    2005-04-01

    The warming of night atmosphere of the Earth during action of meteor showers is analyzed. It was used a satellite measurements in Earth's upper atmosphere for the period of 1993 in height range 85-130 km. Temperature values were obtained with the help of device WINDII (Wind Imaging Interferometer) installed on the America-French satellite UARS (Upper Atmosphere Research Satellite). The most intensive meteor showers Perseids, Leonids, Orionids and Geminids were considered.

  2. Results of the IMO Video Meteor Network - November 2010

    NASA Astrophysics Data System (ADS)

    Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal

    2011-02-01

    Preliminary results of the IMO Video Meteor Network data, collected by 50 cameras of the network, are presented. Almost 16 000 meteors were recorded in more than 3 300 hours of observing time. The activity profile of the Leonids is presented, with their maximum occurring on November 18. Activity profiles of two November minor showers, the Andromedids and the November Orionids, are also presented, fitting well to results from previous years.

  3. Results of the IMO Video Meteor Network - October 2015

    NASA Astrophysics Data System (ADS)

    Molau, S.; Crivello, S.; Goncalves, R.; Saraiva, C.; Stomeo, E.; Kac, J.

    2016-02-01

    The October 2015 overview of IMO Video Meteor Network observations is presented, covering more than 9 600 hours of observations with almost 55 000 recorded meteors. The flux density profile is presented for the October Ursae Majorids for the years 2011 to 2015. The flux density profiles for Orionids are presented for years 2012 to 2015, showing a broad maximum between October 20 and 27.

  4. Results of the IMO Video Meteor Network - January 2016

    NASA Astrophysics Data System (ADS)

    Molau, S.; Crivello, S.; Goncalves, R.; Saraiva, C.; Stomeo, E.; Kac, J.

    2016-06-01

    The January 2016 report of IMO Video Meteor Network observations is presented, based on more than 9 000 hours of observations with almost 28 000 meteors recorded. The flux density profile is presented for the 2016 Quadrantids and compared to the profiles from the years 2011-2015. The flux density profile is also presented for the 2016 gamma-Ursae Minorids. Development of a new algorithm for the calculation of the limiting magnitude is presented.

  5. On the spatial structure of the Perseids meteor stream

    NASA Technical Reports Server (NTRS)

    Andreev, G. V.; Rubtsov, L. N.; Tarasova, I. I.

    1987-01-01

    The analysis of radar observations of the Perseid meteor stream conducted in an ionospherical laboratory in the period from 1964 to 1981 is presented. The Perseids meteor rates were determined by the fluctuation method. Analysis of their hourly distributions showed that the stream maximum position is different for different years, i.e., the stream nodal position is constantly changing. The results of the analysis are presented and discussed.

  6. Origin of meteor swarms of the Arietid and Geminid types

    SciTech Connect

    Lebedinets, V.N.

    1985-10-01

    The author proposes a physical mechanism for the formation of meteor swarms on orbits of small size and very small perihelion distance, similar to the orbits of Arietid and Geminid meteor swarms, which are rarely encountered among the larger bodies of the solar system, and he justifies the mechanism mathematically. He shows that comets can transfer to such orbits from orbits of large size during evaporation of their ice nuclei under the action of reactive drag.

  7. ``Hiss, clicks and pops'' - The enigmatic sounds of meteors

    NASA Astrophysics Data System (ADS)

    Finnegan, J. A.

    2015-04-01

    The improbability of sounds heard simultaneously with meteors allows the phenomenon to remain on the margins of scientific interest and research. This is unjustified, since these audibly perceived electric field effects indicate complex, inconsistent and still unresolved electric-magnetic coupling and charge dynamics; interacting between the meteor; the ionosphere and mesosphere; stratosphere; troposphere and the surface of the earth. This paper reviews meteor acoustic effects, presents illustrating reports and hypotheses and includes a summary of similar and additional phenomena observed during the 2013 February 15 asteroid fragment disintegration above the Russian district of Chelyabinsk. An augmenting theory involving near ground, non uniform electric field production of Ozone, as a stimulated geo-physical phenomenon to explain some hissing `meteor sounds' is suggested in section 2.2. Unlike previous theories, electric-magnetic field fluctuation rates are not required to occur in the audio frequency range for this process to acoustically emit hissing and intermittent impulsive sounds; removing the requirements of direct conversion, passive human transduction or excited, localised acoustic `emitters'. Links to the Armagh Observatory All-sky meteor cameras, electrophonic meteor research and full construction plans for an extremely low frequency (ELF) receiver are also included.

  8. Optical observations of meteors in RI Nikolaev Astronomical Observatory

    NASA Astrophysics Data System (ADS)

    Shulga, Alexander; Sybiryakova, Yevgeniya; Kulichenko, Nikolay; Vovk, Vasyl

    2015-08-01

    Video observations of meteors at the RI NAO are conducted using meteor patrol, which includes 6 optical telescopes (4 lenses: f = 85 mm, f/1.8; 2 lenses: f = 100 mm, f/2.0) equipped with a TV CCD cameras WAT-902H2 (768×576, 8.6×8.3µ). The field of view of 4 telescopes is 3.2°×4.2° and 2.7°×3.6° for 2 telescopes. System doesn't have any intensifier. Each video system is contained in a hermetic capsule to prevent it from rain and other aggressive meteorological conditions. Cameras work in the interlace mode with rate 50 half-frames per second.During 2011-2014 4135 single station meteors were observed. The mean duration of observed meteor trajectories are in 0.05-0.6 s. Double station observation campaigns has been started in September 2013 and it is still working with baseline 11.8 km. During September 2013 - September 2014 total number of observed meteor trajectories was 1757. Number of double station meteors - 328. The mean accuracy of visible radiant determination is less than 0.5 arc sec, more than 80% of radiates have standard deviation less than 0.2 arc sec.

  9. Echoes from the Sky: The Plasma Physics of Meteors Trails

    NASA Astrophysics Data System (ADS)

    Oppenheim, Meers

    2002-11-01

    Since ancient times people have witnessed the spectacular pyrotechnics caused by impacts of high velocity particles with the Earth's upper atmosphere. Today, we study the plasma created by ablating meteors in order to better understand the Earth's space environment, the dynamics and composition of the upper atmosphere and the primordial state of the solar system. Large aperture radars, probing the atmosphere between 75 and 130 km, will typically observe a couple of micro-meteors every minute. Until recently, meteor researchers assumed that these objects created columns of plasma that simply diffused away and used these assumptions to infer characteristics of the meteors and the surrounding atmosphere. However, meteor trails develop in the E-region ionosphere (90-150km altitude), where electrons are magnetized and ions are collisionally demagnetized, and where trails are subject to a set of plasma instabilities which develops into turbulent dynamics. This turbulence substantially modifies the dynamics and diffusion of the trails and explains a number of long-standing observational questions. We have explored this turbulent dynamics with kinetic simulations and theory and have used this knowledge to better interpret meteor radar signals.

  10. The 2014 KCG Meteor Outburst: Clues to a Parent Body

    NASA Technical Reports Server (NTRS)

    Moorhead, Althea V.; Brown, Peter G.; Spurny, Pavel; Cooke, William J.

    2015-01-01

    The Kappa Cygnid (KCG) meteor shower exhibited unusually high activity in 2014, producing ten times the typical number of meteors. The shower was detected in both radar and optical systems and meteoroids associated with the outburst spanned at least five decades in mass. In total, the Canadian Meteor Orbit Radar, European Network, and NASA All Sky and Southern Ontario Meteor Network produced thousands of KCG meteor trajectories. Using these data, we have undertaken a new and improved characterization of the dynamics of this little-studied, variable meteor shower. The Cygnids have a di use radiant and a significant spread in orbital characteristics, with multiple resonances appearing to play a role in the shower dynamics. We conducted a new search for parent bodies and found that several known asteroids are orbitally similar to the KCGs. N-body simulations show that the two best parent body candidates readily transfer meteoroids to the Earth in recent centuries, but neither produces an exact match to the KCG radiant, velocity, and solar longitude. We nevertheless identify asteroid 2001 MG1 as a promising parent body candidate.

  11. SPA Meteor Section Results: November -- December 1999

    NASA Astrophysics Data System (ADS)

    McBeath, A.

    2000-10-01

    Results and reports submitted to the SPA Meteor Section for November and December, 1999, are summarized, except for the Leonid details already discussed [1-3]. The Taurids received some useful coverage in early November, without anything unusual being detected. A brilliant fireball accurred around 22h10m UT on November 28 over southeast Ireland, after which about 271 g of L6 chondritic meteorites were recovered near Leighlinbridge, County Carlow, Ireland, the first recovered meteorite fall in the British Isles since 1991. Two other bright fireballs accurred on November 27-28 and 29-30 over Europe as well. December 13-14 saw the highest Geminid ZHRs, 100 +- 10, during a well-observed Geminid epoch. Radio data showed strong echo counts on both December 13 and 14, with the latter date (lambda approx 263 deg, eq. J2000.0) producing the highest counts generally, but with no specific clear maximum time. The Ursid peak was detected by radio only, giving a very weak showing in most data sets especially around lambda = 269-270 deg.

  12. Radiant ephemeris of the Taurid meteor complex

    NASA Astrophysics Data System (ADS)

    Triglav-Čekada, M.; Arlt, R.

    2005-04-01

    The radiant ephemeris of the Taurid complex meteor showers derived from IMO video observations from 1995-2004 is presented. Detailed radiant ephemerides of the Northern (NPI) and Southern Piscids (SPI) and the Northern (NTA) and Southern Taurids (STA) are derived. Tentative radiant motions of the Northern and Southern chi-Orionids (ORN and ORS) are presented. The Taurids (NTA and STA) are active from the beginning of September to the end of November; the Southern Taurids disappear earlier around November 20. While the Northern Taurids appear to be slower until about October 20 than in the second part of their activity period, the Southern Taurids do not exhibit sub-components. The Southern Piscids (SPI) are active only in September and their activity is much lower than the activity of the Taurids at that time. The Northern Piscids are a little more prominent than the Southern Piscids and are detectable from the beginning of September to October 18, with a probable maximum period from September 20 to October 2.

  13. Seamount, ridge, and transform subduction in southern Central America

    NASA Astrophysics Data System (ADS)

    Morell, Kristin D.

    2016-02-01

    Understanding the factors that control subduction zone processes is a first-order goal in the study of convergent margins. In southern Central America, a growing body of research reveals strong links between the character of the subducting slab and the mechanics of important processes that include subduction erosion, fluid flow, deformation, and seismogenesis. In this paper, I evaluate the role that seamount, ridge, and transform subduction have in the development of upper plate deformation and volcanism by summarizing previous work across a >500 km long region of Central America where each of these three scenarios are present along strike. The data show that the subduction of short-wavelength bathymetry (e.g., seamounts and faults on the seafloor) produces short-wavelength deformation that persists for relatively short timescales (104-105 years), whereas the subduction of longer-wavelength bathymetry (e.g., the aseismic Cocos Ridge) results in longer-wavelength deformation that endures over a longer time scale (106 years). The timing and distribution of upper plate deformation are consistent with subhorizontal Cocos Ridge subduction driving upper plate deformation, and the increased crustal thickness (>20 km) of the subducting Cocos Ridge is likely one of the most important factors in the production of upper plate contraction and crustal thickening. The data illustrate a fundamental connection between lower plate properties and upper plate deformation and highlight the profound influence that bathymetry and crustal thickness have in the localization and kinematics of upper plate strain and volcanism in Middle America.

  14. Tidal currents and anticyclonic motions on two North Pacific seamounts

    USGS Publications Warehouse

    Genin, A.; Noble, M.; Lonsdale, P.F.

    1989-01-01

    Near-bottom currents were measured for several days at three sites on the summits of Fieberling Guyot (32??26???N, 127??46???W) and Horizon Guyot (19??15???N, 160??00???W). Three moorings comprised of two current meters were deployed on each summit; two moorings were deployed on opposite sides of the rim of the summit and one mooring was deployed near the center of the summit. The observed currents were strong, with maximum speeds of 48 and 24 cm s-1 on Fieberling and Horizon, respectively. The currents at specific frequencies were enhanced relative to those in the surrounding ocean. Diurnal currents were the dominant component of the current field on Fieberling Guyot. They accounted for 39-68% of the energy and had amplitudes around 12 cm s-1. We suspect that these diurnal currents were waves trapped over the seamount. Semidiurnal internal tidal currents were the strongest currents over Horizon Guyot, with amplitudes around 4 cm s-1. The flow patterns determined in this study seemed to affect the biological and geological characteristics of the seamounts. ?? 1990.

  15. Volcanology and Geochemistry of the Taney Seamounts northeast Pacific Ocean

    NASA Astrophysics Data System (ADS)

    Coumans, J. P.; Clague, D. A.; Stix, J.

    2011-12-01

    The Taney seamounts are a NW-SE trending, linear, near-ridge chain consisting of five submarine volcanoes located on the Pacific plate 300 km west of San Francisco, California. Morphologically, the seamounts are characterized as truncated cones with nested calderas decreasing in age towards the ridge axis. This study examines the volcanology and geochemistry of the largest and oldest seamount, (Taney A, ~26 Ma), which is comprised of four well-exposed nested calderas. Each successive collapse event exposes previously infilled lavas, defining a relative chronology. The caldera walls and intracaldera pillow mounds were carefully sampled by the remotely operated vehicle (ROV) Doc Ricketts to obtain stratigraphically-controlled samples. Whole rock samples were analyzed for major and trace elements, volcanic glasses were analyzed for major and volatile elements(S, Cl), and plagioclase phenocrysts were separated for mineral and glass inclusion microprobe analysis. Overall, the erupted lavas are mostly subalkalic mid-ocean ridge basalts (MORB) varying from differentiated to more primitive (6.0 - 8.2 wt. % MgO) with decreasing age. Incompatible elements and REE profiles normalized to primitive mantle suggest that the lavas are transitional to slightly enriched (0.1 - 0.3 wt. % K2O; 1.1 - 2.2 wt. % TiO2), which is unusual for near-ridge seamounts. Sc, which is compatible in clinopyroxene, increases linearly with TiO2 at primitive compositions (>7.0 wt. % MgO). In more evolved seamount basalts (<7.0 wt. % MgO), the low CaO and Sc contents and decreasing CaO/Al2O3 suggest that there is either extensive clinopyroxene fractionation, or mixing with magmas that have undergone extensive clinopyroxene fractionation. MELTS modeling suggests that clinopyroxene fractionation occurs at <6.0 wt. % MgO, inconsistent with the observed clinopyroxene imprint at <7.0 wt. % MgO. The discrepancy could indicate magma mixing. Although whole rock ICP-MS data have some scatter, especially for

  16. Prokaryote diversity and viral production in deep-sea sediments and seamounts

    NASA Astrophysics Data System (ADS)

    Danovaro, Roberto; Corinaldesi, Cinzia; Luna, Gian Marco; Magagnini, Mirko; Manini, Elena; Pusceddu, Antonio

    2009-05-01

    Despite the fact that marine prokaryotes and viruses have been increasingly investigated over the last decade, knowledge on prokaryote diversity and viral production in bathyal sediments is limited. We investigated microbial variables in the deep-sea sediments around two seamounts at 3000-m depth in the Tyrrhenian Sea and sediments located at the same depth, but not affected by the presence of the seamounts. We hypothesized that seamounts altered significantly prokaryotes-viruses interactions in surrounding deep-sea sediments. Sediments surrounding seamounts were characterised by prokaryotic abundances significantly higher than those observed in non-seamount sediments. Benthic viral production was about double in sediments close to seamounts than in non-seamount sediments, where virus turnover was up to 3 times lower. Total Bacteria, as assessed by CARD-FISH, dominated prokaryotic community structure, whereas Archaea accounted on average for approximately 10%. The fraction of Crenarchaeota was always higher than Euryarchaeota. Bacterial diversity, estimated using ARISA, was high, with up to 127 different microbial operational taxonomic units (OTUs) in a single sample. Archaeal richness (determined using T-RFLP of the 16S rRNA gene) ranged from 12 to 20 OTUs, while Archaeal evenness was comprised between 0.529±0.018 and 0.623±0.08. Results represent a pointer for future investigations dealing with the interactions between viruses and prokaryotes in deep-sea sediments.

  17. Seasonal changes in fish assemblage structure at a shallow seamount in the Gulf of California.

    PubMed

    Jorgensen, Salvador J; Klimley, A Peter; Muhlia-Melo, Arturo; Morgan, Steven G

    2016-01-01

    Seamounts have generally been identified as locations that can promote elevated productivity, biomass and predator biodiversity. These properties attract seamount-associated fisheries where elevated harvests can be obtained relative to surrounding areas. There exists large variation in the geological and oceanographic environment among the thousands of locations that fall within the broad definition of seamount. Global seamount surveys have revealed that not all seamounts are hotspots of biodiversity, and there remains a strong need to understand the mechanisms that underlie variation in species richness observed. We examined the process of fish species assembly at El Bajo Espiritu Santo (EBES) seamount in the Gulf of California over a five-year study period. To effectively quantify the relative abundance of fast-moving and schooling fishes in a 'blue water' habitat, we developed a simplified underwater visual census (UVC) methodology and analysis framework suitable for this setting and applicable to future studies in similar environments. We found correlations between seasonally changing community structure and variability in oceanographic conditions. Individual species responses to thermal habitat at EBES revealed three distinct assemblages, a 'fall assemblage' tracking warmer overall temperature, a 'spring assemblage' correlated with cooler temperature, and a 'year-round assemblage' with no significant response to temperature. Species richness was greatest in spring, when cool and warm water masses stratified the water column and a greater number of species from all three assemblages co-occurred. We discuss our findings in the context of potential mechanisms that could account for predator biodiversity at shallow seamounts. PMID:27651985

  18. Temporal patterns in the acoustic signals of beaked whales at Cross Seamount.

    PubMed

    Johnston, D W; McDonald, M; Polovina, J; Domokos, R; Wiggins, S; Hildebrand, J

    2008-04-23

    Seamounts may influence the distribution of marine mammals through a combination of increased ocean mixing, enhanced local productivity and greater prey availability. To study the effects of seamounts on the presence and acoustic behaviour of cetaceans, we deployed a high-frequency acoustic recording package on the summit of Cross Seamount during April through October 2005. The most frequently detected cetacean vocalizations were echolocation sounds similar to those produced by ziphiid and mesoplodont beaked whales together with buzz-type signals consistent with prey-capture attempts. Beaked whale signals occurred almost entirely at night throughout the six-month deployment. Measurements of prey presence with a Simrad EK-60 fisheries acoustics echo sounder indicate that Cross Seamount may enhance local productivity in near-surface waters. Concentrations of micronekton were aggregated over the seamount in near-surface waters at night, and dense concentrations of nekton were detected across the surface of the summit. Our results suggest that seamounts may provide enhanced foraging opportunities for beaked whales during the night through a combination of increased productivity, vertical migrations by micronekton and local retention of prey. Furthermore, the summit of the seamount may act as a barrier against which whales concentrate prey. PMID:18252660

  19. Temporal patterns in the acoustic signals of beaked whales at Cross Seamount.

    PubMed

    Johnston, D W; McDonald, M; Polovina, J; Domokos, R; Wiggins, S; Hildebrand, J

    2008-04-23

    Seamounts may influence the distribution of marine mammals through a combination of increased ocean mixing, enhanced local productivity and greater prey availability. To study the effects of seamounts on the presence and acoustic behaviour of cetaceans, we deployed a high-frequency acoustic recording package on the summit of Cross Seamount during April through October 2005. The most frequently detected cetacean vocalizations were echolocation sounds similar to those produced by ziphiid and mesoplodont beaked whales together with buzz-type signals consistent with prey-capture attempts. Beaked whale signals occurred almost entirely at night throughout the six-month deployment. Measurements of prey presence with a Simrad EK-60 fisheries acoustics echo sounder indicate that Cross Seamount may enhance local productivity in near-surface waters. Concentrations of micronekton were aggregated over the seamount in near-surface waters at night, and dense concentrations of nekton were detected across the surface of the summit. Our results suggest that seamounts may provide enhanced foraging opportunities for beaked whales during the night through a combination of increased productivity, vertical migrations by micronekton and local retention of prey. Furthermore, the summit of the seamount may act as a barrier against which whales concentrate prey.

  20. Seasonal changes in fish assemblage structure at a shallow seamount in the Gulf of California.

    PubMed

    Jorgensen, Salvador J; Klimley, A Peter; Muhlia-Melo, Arturo; Morgan, Steven G

    2016-01-01

    Seamounts have generally been identified as locations that can promote elevated productivity, biomass and predator biodiversity. These properties attract seamount-associated fisheries where elevated harvests can be obtained relative to surrounding areas. There exists large variation in the geological and oceanographic environment among the thousands of locations that fall within the broad definition of seamount. Global seamount surveys have revealed that not all seamounts are hotspots of biodiversity, and there remains a strong need to understand the mechanisms that underlie variation in species richness observed. We examined the process of fish species assembly at El Bajo Espiritu Santo (EBES) seamount in the Gulf of California over a five-year study period. To effectively quantify the relative abundance of fast-moving and schooling fishes in a 'blue water' habitat, we developed a simplified underwater visual census (UVC) methodology and analysis framework suitable for this setting and applicable to future studies in similar environments. We found correlations between seasonally changing community structure and variability in oceanographic conditions. Individual species responses to thermal habitat at EBES revealed three distinct assemblages, a 'fall assemblage' tracking warmer overall temperature, a 'spring assemblage' correlated with cooler temperature, and a 'year-round assemblage' with no significant response to temperature. Species richness was greatest in spring, when cool and warm water masses stratified the water column and a greater number of species from all three assemblages co-occurred. We discuss our findings in the context of potential mechanisms that could account for predator biodiversity at shallow seamounts.

  1. Generation of mesoscale hydrodynamic phenomena by the Grappler and Whiting Seamounts, southeast of Puerto Rico

    SciTech Connect

    Capella, J.E.

    1983-01-01

    This work presents the results of research on topographically generated mesoscale eddies in the region of the Grappler and Whiting Seamounts which are located 22 km southeast of Puerto Rico. Three different data sets were used: (1) site specific hydrographic data, (2) satellite images from TIROS/NOAA, Landsat and Skylab satellites, and (3) free-drifting drogued-buoy tracks. A reference current meter station was established at the Benchmark B OTEC site (17/sup 0/ 57.3' N, 65/sup 0/ 51.5' W), at a depth of 20 meters. Predictions from numerical and analytical models were tested using the site specific data and then compared to experimental results. The hydrographic and drogue data definitively establish the presence of perturbations over the seamounts which are qualitatively consistent with model predictions. Closed contour regions in the distribution of dynamic heights, temperature, salinity and dissolved oxygen were found in the surface and subsurface waters above the top of Grappler Seamount. Horizontal flow perturbations, detected down to 100m, probably extend deeper. Whiting Seamount's effect was detected in the depth range from 200 to 300m, also near its top. Two distinct warm and cold regions were detected over this seamount. A cyclonic eddy-like feature located close to Grappler Seamount, in the satellite images, also suggests that eddies are being shed from the seamount region. 42 refs., 22 figs., 3 tabs.

  2. Petrology and tectonic significance of seamounts within transitional crust east of Orphan Knoll, offshore eastern Canada

    NASA Astrophysics Data System (ADS)

    Pe-Piper, Georgia; Meredyk, Shawn; Zhang, Yuanyuan; Piper, David J. W.; Edinger, Evan

    2013-12-01

    The Early Cretaceous separation of Newfoundland from Iberia-Ireland is a classic example of a magma-poor continental margin with hyperextension and with widespread minor magmatism resulting in seamounts. This study defines the distribution of seamounts east of Orphan Knoll, and documents and interprets the geochemical character of the one recovered lava sample. Video imagery of lava outcrops, and the sample, were obtained by ROV from Orphan seamount, one of a linear series of small seamounts overlying transitional thinned continental crust on the seaward side of Orphan Knoll. New multibeam bathymetry and legacy seismic data show several seamounts that extend irregularly along the fault-bound NE margin of Orphan Knoll. Whole rock geochemistry shows the sample to be highly alkaline basanite or possibly tephrite. Diopside-hedenbergite, kaersutite and K-feldspar phenocrysts were analyzed by electron microprobe and scanning electron microscope, and alteration minerals including kaolinite were identified by X-ray diffraction. The highly alkaline character of the basanite is similar only to Early Cretaceous volcanic and sub-volcanic rocks erupted through thick continental crust of the Mesoproterozoic Grenville Orogeny. The location of the linear set of seamounts is related to margin-parallel faults on the seaward side of Orphan Knoll that provided a pathway for magma, although ENE-trending lineaments in individual seamounts or seamount groups suggest the influence of oceanic fracture zones. A lower gradient crest to Orphan seamount above 2,200 m suggests subaerial erosion, consistent with the presence of kaolinite as an alteration product and the absence of lava pillows at and above this depth.

  3. Morphology, petrography, age and origin of Fogo Seamount chain, offshore eastern Canada

    NASA Astrophysics Data System (ADS)

    Pe-Piper, G.; de Jonge, A.; Piper, D. J. W.; Jansa, L. F.

    2003-04-01

    The Fogo Seamounts are located approximately 500 km offshore from Newfoundland to the southwest of the Grand Banks of Newfoundland. This complex seamount chain is early Cretaceous in age and is partially buried under later continental slope deposits. It has in the past been ascribed to the passage of a Canary or Azores hot spot. The seamounts are developed along the northeastern transform margin of the Jurassic central Atlantic Ocean. The Narwhal F-99 well was drilled in 1986 on the continental slope into one buried seamount. In this study, we bring together unpublished data on the bathymetry, seismic-reflection character, and distribution of the Fogo Seamounts and interpret new petrographic, geochemical, isotopic and geochronological data from a dredge sample from the central part of the seamount chain and from the Narwhal F-99 well, making comparisons with other offshore volcanic rocks on the eastern Canadian margin. Petrographically, the seamount samples consist of vitrophyric basalt, with clinopyroxene at Narwhal and kaersutite in the dredge sample. Chemically, the samples are olivine basalt with a low Mg number and low concentration of transition metals. Trace element and REE abundances are similar to those of other early Cretaceous volcanic rocks on the southeast Canadian margin. Three petrogenetic types of mafic magma are recognised in the area. The dredge sample is typical OIB rather alkalic basalts and similar to those in other seamount chains. Rocks at Narwhal and Brant have a greater signature of a depleted mantle source (are more tholeiitic). All have Nd isotopes similar to the Newfoundland and New England seamounts. In Orpheus graben to the northwest, there appears to have been greater crustal contamination, either from the crust in the region or from mantle previously enriched in crustal contaminants. The dredge sample gave a 40Ar/39Ar age of 130.3 +/- 1.3 Ma (Hauterivian). A K/Ar age from the Narwhal F-99 well of 127 +/- 6 Ma is inconsistent with

  4. Dynamical Model for the Toroidal Sporadic Meteors

    NASA Astrophysics Data System (ADS)

    Pokorný, Petr; Vokrouhlický, David; Nesvorný, David; Campbell-Brown, Margaret; Brown, Peter

    2014-07-01

    More than a decade of radar operations by the Canadian Meteor Orbit Radar have allowed both young and moderately old streams to be distinguished from the dispersed sporadic background component. The latter has been categorized according to broad radiant regions visible to Earth-based observers into three broad classes: the helion and anti-helion source, the north and south apex sources, and the north and south toroidal sources (and a related arc structure). The first two are populated mainly by dust released from Jupiter-family comets and new comets. Proper modeling of the toroidal sources has not to date been accomplished. Here, we develop a steady-state model for the toroidal source of the sporadic meteoroid complex, compare our model with the available radar measurements, and investigate a contribution of dust particles from our model to the whole population of sporadic meteoroids. We find that the long-term stable part of the toroidal particles is mainly fed by dust released by Halley type (long period) comets (HTCs). Our synthetic model reproduces most of the observed features of the toroidal particles, including the most troublesome low-eccentricity component, which is due to a combination of two effects: particles' ability to decouple from Jupiter and circularize by the Poynting-Robertson effect, and large collision probability for orbits similar to that of the Earth. Our calibrated model also allows us to estimate the total mass of the HTC-released dust in space and check the flux necessary to maintain the cloud in a steady state.

  5. Dynamical model for the toroidal sporadic meteors

    SciTech Connect

    Pokorný, Petr; Vokrouhlický, David; Nesvorný, David; Campbell-Brown, Margaret; Brown, Peter E-mail: vokrouhl@cesnet.cz E-mail: margaret.campbell@uwo.ca

    2014-07-01

    More than a decade of radar operations by the Canadian Meteor Orbit Radar have allowed both young and moderately old streams to be distinguished from the dispersed sporadic background component. The latter has been categorized according to broad radiant regions visible to Earth-based observers into three broad classes: the helion and anti-helion source, the north and south apex sources, and the north and south toroidal sources (and a related arc structure). The first two are populated mainly by dust released from Jupiter-family comets and new comets. Proper modeling of the toroidal sources has not to date been accomplished. Here, we develop a steady-state model for the toroidal source of the sporadic meteoroid complex, compare our model with the available radar measurements, and investigate a contribution of dust particles from our model to the whole population of sporadic meteoroids. We find that the long-term stable part of the toroidal particles is mainly fed by dust released by Halley type (long period) comets (HTCs). Our synthetic model reproduces most of the observed features of the toroidal particles, including the most troublesome low-eccentricity component, which is due to a combination of two effects: particles' ability to decouple from Jupiter and circularize by the Poynting-Robertson effect, and large collision probability for orbits similar to that of the Earth. Our calibrated model also allows us to estimate the total mass of the HTC-released dust in space and check the flux necessary to maintain the cloud in a steady state.

  6. Towards a paleolatitude record from the Louisville Seamount trail

    NASA Astrophysics Data System (ADS)

    Gee, J. S.; Pressling, N.; Hoshi, H.; Yamazaki, T.; Scientists, E. 3; IODP Expedition 330 Scientists

    2011-12-01

    The 4300 km long Louisville Seamount trail is the South Pacific counterpart of the much better studied Hawaii-Emperor chain. Both chains are thought to reflect motion of the Pacific plate over persistent mantle melting anomalies although the stationarity of these hotspots, and thus their suitability as a reference frame for Pacific plate motions, remains uncertain. Drilling at the Emperor Seamounts documented an ~15° southward shift of the Hawaiian hotspot between about 80 and 50 Ma. IODP Expedition 330 provided the first drillcore samples from the Louisville chain, with a primary goal of documenting the paleolatitudes of seamounts with ages comparable to those drilled in the Hawaii-Emperor chain. Six sites were drilled on five Louisville guyots. The recovered materials include sediments, submarine lava flows/pillows, less abundant subaerial flows and a substantial proportion of volcaniclastic and hyaloclastite material. Sites U1374 and U1373 on Rigil Guyot (28.6°S, ~73 Ma) penetrated 522m and 66m, respectively, and yielded about thirty cooling units including both normal and reversed polarity flows. Approximately 20 normal polarity cooling units were recovered from the 233m cored interval at Site U1372 on Canopus Guyot (26.5°, ~76 Ma). Site U1376 on Burton Guyot (32.2°, ~64 Ma) penetrated 182m, with 11 reversed polarity flows. A total of 17 reversed polarity cooling units were sampled at Hadar Guyot (38.2°S, ~50 Ma) despite more limited penetration. Characteristic remanent magnetization directions were determined for more than 22,000 two-cm intervals on the archive half cores. The most reliable of these data were used to calculate average directions for individual core pieces that compare well with results from stepwise demagnetization of nearly 500 discrete samples. Because of the abundance of (mostly submarine) volcaniclastic material recovered, estimating the paleolatitude for the Louisville guyots is less straightforward than for the sites on the Hawaii

  7. Automated Optical Meteor Fluxes and Preliminary Results of Major Showers

    NASA Technical Reports Server (NTRS)

    Blaauw, R.; Campbell-Brown, M.; Cooke, W.; Kingery, A.; Weryk, R.; Gill, J.

    2014-01-01

    NASA's Meteoroid Environment Office (MEO) recently established a two-station system to calculate daily automated meteor fluxes in the millimeter-size-range for both single-station and double-station meteors. The cameras each consist of a 17 mm focal length Schneider lens (f/0.95) on a Watec 902H2 Ultimate CCD video camera, producing a 21.7x15.5 degree field of view. This configuration sees meteors down to a magnitude of +6. This paper outlines the concepts of the system, the hardware and software, and results of 3,000+ orbits from the first 18 months of operations. Video from the cameras are run through ASGARD (All Sky and Guided Automatic Real-time Detection), which performs the meteor detection/photometry, and invokes MILIG and MORB (Borovicka 1990) codes to determine the trajectory, speed, and orbit of the meteor. A subroutine in ASGARD allows for approximate shower identification in single-station detections. The ASGARD output is used in routines to calculate the flux. Before a flux can be calculated, a weather algorithm indicates if sky conditions are clear enough to calculate fluxes, at which point a limiting magnitude algorithm is employed. The limiting stellar magnitude is found using astrometry.net (Lang et al. 2012) to identify stars and translated to the corresponding shower and sporadic limiting meteor magnitude. It is found every 10 minutes and is able to react to quickly changing sky conditions. The extensive testing of these results on the Geminids and Eta Aquariids is shown. The flux involves dividing the number of meteors by the collecting area of the system, over the time interval for which that collecting area is valid. The flux algorithm employed here differs from others currently in use in that it does not make the gross oversimplication of choosing a single height to calculate the collection area of the system. In the MEO system, the volume is broken up into a set of height intervals, with the collecting areas determined by the position of the

  8. The origin and evolution of a near-axis seamount in marginal basin: case study in the South China Sea

    NASA Astrophysics Data System (ADS)

    Yan, Q.; Shi, X.; Wang, L.; Liao, L.; Ren, J.

    2013-12-01

    Volcaniclastic rock on seamount is the product of subaqueous explosive volcanism. The finding of volcaniclastic rocks from the Daimao seamounts and some other seamounts suggests that the top of most seamounts in the South China Sea (SCS) once exceeded the pressure compensation level (PCL), and these rocks are products of subaqueous explosive volcanism. The major element compositional features of these volcaniclastic rocks reflect low-temperature seawater alteration have a significant role on whole rock compositions (by means of secondary altered minerals), but there shows a consistence in trace element compositions between whole rock samples and basaltic lava samples separated from whole rock samples. Trace element compositions, combined with Sr, Nd and Pb isotopic compositions, suggested that similar to alkali basalts from other seamounts in the SCS, all samples are of OIB-like features and Dupal Pb anomaly (an endogenous mantle component). The estimated mean subsidence rate for the Daimao seamount, combined with previous results for other two seamounts, suggested earlier subsidence rate of seamounts is obviously higher than calculated mean subsidence rate. This paper proposed a simplified model for the formation and evolution of the Daimao seamounts as follows. At about 14Ma, basic volcanic edifice framework of the Daimao seamount was formed by subaqueous explosive volcanism whose materials are originated from Hainan mantle plume. Subsequently under shallow-water environment, the seamount received coral-bearing carbonate deposits. Then, due to gravity isostatic compensation, the seamount begins to subside to the site more than 400m water depth at the velocity of 5-30mm/y after receiving a few amounts of carbonate deposits. Finally, the seamount subside to the present site at a slower rate and commences to receive Fe-Mn crust deposits.

  9. Division F Commission 22: Meteors, Meteorites, and Interplanetary Dust

    NASA Astrophysics Data System (ADS)

    Jenniskens, Peter; Borovička, Jiří; Watanabe, Jun-Ichi; Jopek, Tadeusz; Abe, Shinsuke; Consolmagno, Guy J.; Ishiguro, Masateru; Janches, Diego; Ryabova, Galina O.; Vaubaillon, Jérémie; Zhu, Jin

    2016-04-01

    Commission 22 (Meteors, Meteorites and Interplanetary Dust) was established at the first IAU General Assembly held in Rome in 1922, with William Frederick Denning as its first President. Denning was an accountant by profession, but as an amateur astronomer he contributed extensively to meteor science. Commission 22 thus established a pattern that has continued to this day that non-professional astronomers were welcomed and valued and could play a significant role in its affairs. The field of meteors, meteorites and interplanetary dust has played a disproportional role in the astronomical perception of the general public through the majestic displays of our annual meteor showers. Those in the field deployed many techniques uncommon in other fields of astronomy, studying the ``vermin of space'', the small solid bodies that pervade interplanetary space and impact Earth's atmosphere, the surface of the Moon, and that of our satellites in orbit. Over time, the field has tackled a wide array of problems, from predicting the encounter with meteoroid streams, to the origin of our meteorites and the nature of the zodiacal cloud. Commission 22 has played an important role in organizing the field through dedicated meetings, a data centre, and working groups that developed professional-amateur relationships and that organized the nomenclature of meteor showers. The contribution of Commission 22 to the field is perhaps most readily seen in the work of the presidents that followed in the footsteps of Denning.

  10. Catalogue of Meteor Showers and Storms in Korean History

    NASA Astrophysics Data System (ADS)

    Ahn, Sang-Hyeon

    2004-03-01

    We present a more complete and accurate catalogue of astronomical records for meteor showers and meteor storms appeared in primary official Korean history books, such as Samguk-sagi, Koryo-sa, Seungjeongwon-ilgi, and Choson-Wangjo-Sillok. So far the catalogue made by Imoto and Hasegawa in 1958 has been widely used in the international astronomical society. The catalogue is based on a report by Sekiguchi in 1917 that is mainly based on secondary history books. We observed that the catalogue has a number of errors in either dates or sources of the records. We have thoroughly checked the primary official history books, instead of the secondary ones, in order to make a corrected and extended catalogue. The catalogue contains 25 records of meteor storms, four records of intense meteor-showers, and five records of usual showers in Korean history. We also find that some of those records seem to correspond to some presently active meteor showers such as the Leonids, the Perseids, and the ¥ç-Aquarids-Orionids pair. However, a large number of those records do not correspond to such present showers. This catalogue we obtained can be useful for various astrophysical studies in the future.

  11. Largest meteor since Tunguska event explodes above Russian city

    NASA Astrophysics Data System (ADS)

    Showstack, Randy

    2013-02-01

    The meteor that disintegrated in the atmosphere above Chelyabinsk, Russia, on 15 February, injuring more than 1000 people and causing widespread property damage from the shock wave, is the largest such incident since the 1908 Tunguska event in Siberia, according to Paul Chodas, research scientist in the Near-Earth Object (NEO) program office at NASA's Jet Propulsion Laboratory in Pasadena, Calif. During a 15 February teleconference, Chodas said it was an "incredible coincidence" that asteroid DA14 passed safely by Earth on the same day as the Chelyabinsk meteor; the 45-meter-wide asteroid sped by the planet at a distance of just 27,700 kilometers away on its closest approach. He stressed that the meteor was not related to DA14. The meteor "was coming from the wrong direction and at a completely different velocity," he said, noting that the orbit of the meteor went out to the asteroid belt while the orbit of DA14 "is very Earth-like, it does not go out so far."

  12. The fish fauna of Ampère Seamount (NE Atlantic) and the adjacent abyssal plain

    NASA Astrophysics Data System (ADS)

    Christiansen, Bernd; Vieira, Rui P.; Christiansen, Sabine; Denda, Anneke; Oliveira, Frederico; Gonçalves, Jorge M. S.

    2015-03-01

    An inventory of benthic and benthopelagic fishes is presented as a result of two exploratory surveys around Ampère Seamount, between Madeira and the Portuguese mainland, covering water depths from 60 to 4,400 m. A total of 239 fishes were collected using different types of sampling gear. Three chondrichthyan species and 31 teleosts in 21 families were identified. The collections showed a vertical zonation with little overlap, but indications for an affinity of species to certain water masses were only vague. Although most of the species present new records for Ampère Seamount, all of them have been known for the NE Atlantic; endemic species were not found. The comparison with fish communities at other NE Atlantic seamounts indicates that despite a high ichthyofaunal similarity, which supports the "stepping stone" hypothesis of species dispersal, some differences can be attributed to the local features of the seamounts.

  13. Draft Genome Sequence of Mariprofundus ferrooxydans Strain JV-1, Isolated from Loihi Seamount, Hawaii

    PubMed Central

    Fullerton, Heather; Hager, Kevin W.

    2015-01-01

    Mariprofundus ferrooxydans strain JV-1 was isolated in 1998 from Loihi Seamount, Hawaii. Here, we present the draft genome of strain JV-1, which shows similarity to other sequenced Mariprofundus isolates, strains PV-1 and M34. PMID:26450720

  14. 76 FR 8330 - Hawaii Bottomfish and Seamount Groundfish Fisheries; Modification to Advance Notification Period...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-02-14

    ... From the Federal Register Online via the Government Publishing Office DEPARTMENT OF COMMERCE National Oceanic and Atmospheric Administration 50 CFR Part 665 RIN 0648-BA58 Hawaii Bottomfish and Seamount Groundfish Fisheries; Modification to Advance Notification Period for Fishery Closures...

  15. Chemically diverse, sporadic volcanism at seamounts offshore southern and Baja California

    USGS Publications Warehouse

    Davis, A.S.; Gunn, S.H.; Bohrson, W.A.; Gray, L.-B.; Hein, J.R.

    1995-01-01

    Compositions of lavas from seven small to medium-sized seamounts offshore southern and Baja California, include low-K2O tholeiitic, transitional, and mildly to moderately alkalic basalt and their differentiates. The seamounts with these MORB-like lavas are inferred to have formed at or near the spreading center. Based on 40Ar/39Ar laser fusion techniques, MORB-like lava from one of the northern edifices is as old as the underlying oceanic crust (>20 Ma), indicating that it originated at a spreading center. Other seamount lava ages are much younger than the oceanic crust on which they reside. Some of the seamounts with transitional and alkalic lavas may have formed as part of a short, age-progressive chain formed by a short-lived mantle plume. Many others, may have resulted from upwelling mantle diapirs in response to localized extension. -from Authors

  16. Frequency synchronization of blue whale calls near Pioneer Seamount.

    PubMed

    Hoffman, Michael D; Garfield, Newell; Bland, Roger W

    2010-07-01

    Vocalizations of blue whales were recorded with a cabled hydrophone array at Pioneer Seamount, 50 miles off the California coast. Most calls occurred in repeated sequences of two-call pairs (A, then B). The B call is a frequency-modulated tone highly repeatable in form and pitch. A model of this sound is described which permits detecting very small frequency shifts. B calls are found to be aligned in frequency to about one part in 180. This requires very fine pitch discrimination and control over calling frequency, and suggests that synchronizing to a common frequency pattern carries some adaptive advantage. Some possibilities for acoustic sensing by whales requiring this fine frequency resolution are discussed. PMID:20649243

  17. Biogeochemical Cycling of Iron Isotopes at Loihi Seamount

    NASA Astrophysics Data System (ADS)

    Rouxel, O. J.; Edwards, K. J.; Moyer, C. L.; Wheat, G.

    2007-12-01

    It is now well recognized that seafloor hydrothermal systems support diverse and unique biological communities capable of using dissolved chemical species, such as Iron (Fe), as well as mineral substrates as sources of metabolic energy. Deep-sea hydrothermal systems such as the Loihi Seamount hydrothermal field are important examples of environments where both chemical and biological oxidation of Fe can occur simultaneously and provide an ideal system in which to test hypotheses on biotic vs. abiotic origin of iron-oxide formation. Here, we applied Fe isotope systematics of hydrothermal fluids and Fe-oxide precipitates to study biogeochemical cycling of iron and the formation of microbial mats at Loihi seamount. Warm hydrothermal fluids (<60°C) and iron oxide precipitates were recovered using the DSV Jason II during FeMO 2006 cruise. Fe-isotope composition of warm hydrothermal fluids yielded δ56Fe values near 0.1‰ and are indistinguishable from basalt values defined at 0.09‰. Suspended iron oxide particles in the fluids and seafloor iron oxide sediments (microbial mats) recovered in the vicinity of the vents yielded systematically positive δ56Fe values. The enrichment in heavy isotopes between 1.05 to 1.43‰ relative to Fe(II) in vent fluids is slightly higher than those obtained for abiotic Fe oxidation (around 0.9‰) and slightly lower than for bacterial Fe oxidation at circum neutral pH (around 1.5‰). Mass balance considerations also imply that the extent of Fe(II) oxidation is very limited in the vicinity of the vents (<20%) and that most Fe(II) is oxidized later in the water column. These results are consistent with the low oxygen content of seawater (i.e. summit of Loihi is located in the OMZ) and resultant slow kinetics of abiotic Fe oxidation. In contrast, mats supported by very diffuse fluids recovered at the base of the Loihi Seamount (~ 5000m depth) have distinctly negative Fe-isotope values between -0.3 to -1.5‰. These negative values are

  18. Frequency synchronization of blue whale calls near Pioneer Seamount.

    PubMed

    Hoffman, Michael D; Garfield, Newell; Bland, Roger W

    2010-07-01

    Vocalizations of blue whales were recorded with a cabled hydrophone array at Pioneer Seamount, 50 miles off the California coast. Most calls occurred in repeated sequences of two-call pairs (A, then B). The B call is a frequency-modulated tone highly repeatable in form and pitch. A model of this sound is described which permits detecting very small frequency shifts. B calls are found to be aligned in frequency to about one part in 180. This requires very fine pitch discrimination and control over calling frequency, and suggests that synchronizing to a common frequency pattern carries some adaptive advantage. Some possibilities for acoustic sensing by whales requiring this fine frequency resolution are discussed.

  19. Kaitoku seamount and the mystery cloud of 9 april 1984.

    PubMed

    Walker, D A; McCreery, C S; Oliveira, F J

    1985-02-01

    On 9 April 1984, commercial airlines enroute from Tokyo, Japan, to Anchorage, Alaska, reported an unusual mushroom-shaped cloud at about 38.5 degrees N, 146.0 degrees E. On 8 and 9 April the intensity of volcanism from Kaitoku Seamount (26.0 degrees N, 140.8 degrees E), as indicated by T-phase recordings on an array of ocean bottom hydrophones, reached a maximum level and then declined rapidly. An examination was made of the possible relation of the cloud to eruptions of Kaitoku through an analysis of pilot depositions, satellite photos, wind charts, signal strengths and spectra of known man-made underwater explosions, as well as ascent rates of volcanic plumes and cumulonimbus clouds.

  20. The magnetisation of Rosemary Bank Seamount, Rockall Trough, northeast Atlantic

    NASA Astrophysics Data System (ADS)

    Miles, P. R.; Roberts, D. G.

    1981-08-01

    Rosemary Bank is a non-uniformly magnetised seamount in the northern Rockall Trough. The reversely magnetised major component of the anomaly field was simulated by a numerical method and modelled using the Talwani three-dimensional magnetics program. The results suggest a higher Koenigsberger ratio than earlier reported for Rosemary Bank and a remanent magnetisation vector compatible with post-Jurassic formation and probably of a Late Cretaceous to Tertiary age. The limited depth to the base of the model implies that Rosemary Bank post-dates the underlying basement in agreement with a volcanic origin. The residual of the observed anomaly field is interpreted as being caused by normally magnetised bodies within and on top of the bank. This suggests subsequent volcanic activity during an interval of normal polarity.

  1. Extraordinarily high biomass benthic community on Southern Ocean seamounts.

    PubMed

    Thresher, R E; Adkins, J; Fallon, S J; Gowlett-Holmes, K; Althaus, F; Williams, A

    2011-01-01

    We describe a previously unknown assemblage of seamount-associated megabenthos that has by far the highest peak biomass reported in the deep-sea outside of vent communities. The assemblage was found at depths of 2-2.5 km on rocky geomorphic features off the southeast coast of Australia, in an area near the Sub-Antarctic Zone characterised by high rates of surface productivity and carbon export to the deep-ocean. These conditions, and the taxa in the assemblage, are widely distributed around the Southern mid-latitudes, suggesting the high-biomass assemblage is also likely to be widespread. The role of this assemblage in regional ecosystem and carbon dynamics and its sensitivities to anthropogenic impacts are unknown. The discovery highlights the lack of information on deep-sea biota worldwide and the potential for unanticipated impacts of deep-sea exploitation. PMID:22355636

  2. Extraordinarily high biomass benthic community on Southern Ocean seamounts.

    PubMed

    Thresher, R E; Adkins, J; Fallon, S J; Gowlett-Holmes, K; Althaus, F; Williams, A

    2011-01-01

    We describe a previously unknown assemblage of seamount-associated megabenthos that has by far the highest peak biomass reported in the deep-sea outside of vent communities. The assemblage was found at depths of 2-2.5 km on rocky geomorphic features off the southeast coast of Australia, in an area near the Sub-Antarctic Zone characterised by high rates of surface productivity and carbon export to the deep-ocean. These conditions, and the taxa in the assemblage, are widely distributed around the Southern mid-latitudes, suggesting the high-biomass assemblage is also likely to be widespread. The role of this assemblage in regional ecosystem and carbon dynamics and its sensitivities to anthropogenic impacts are unknown. The discovery highlights the lack of information on deep-sea biota worldwide and the potential for unanticipated impacts of deep-sea exploitation.

  3. Composition and origin of hydrothermal ironstones from central Pacific seamounts

    USGS Publications Warehouse

    Hein, J.R.; Hsueh-Wen, Y.; Gunn, S.H.; Gibbs, A.E.; Chung-ho, W.

    1994-01-01

    Ironstones recovered from five Late Cretaceous seamounts in the central Pacific region probably formed during late-stage edifice-building volcanism. Ironstones are dense and compact with the appearance of brown chert. The ironstones are characterized by a goethite mineralogy with FeOOH contents up to 88%, extreme fractionation of Fe and Mn, low trace-element and rare earth element abundances, low Co Zn ratios, and isotopic equilibration temperatures of about 20-45 ??C. These characteristics indicate that the ironstones formed from hydrothermal fluids. Ironstones probably formed below the seawater-seafloor interface, as indicated by their occurrence as a proximal hydrothermal deposit, presence of primary goethite cement, pervasive replacement of rocks by goethite, and absence of interbedded pyro-clastic beds. ?? 1994.

  4. Great Apes

    USGS Publications Warehouse

    Sleeman, Jonathan M.; Cerveny, Shannon

    2014-01-01

    Anesthesia of great apes is often necessary to conduct diagnostic analysis, provide therapeutics, facilitate surgical procedures, and enable transport and translocation for conservation purposes. Due to the stress of remote delivery injection of anesthetic agents, recent studies have focused on oral delivery and/or transmucosal absorption of preanesthetic and anesthetic agents. Maintenance of the airway and provision of oxygen is an important aspect of anesthesia in great ape species. The provision of analgesia is an important aspect of the anesthesia protocol for any procedure involving painful stimuli. Opioids and nonsteroidal anti-inflammatory drugs (NSAIDs) are often administered alone, or in combination to provide multi-modal analgesia. There is increasing conservation management of in situ great ape populations, which has resulted in the development of field anesthesia techniques for free-living great apes for the purposes of translocation, reintroduction into the wild, and clinical interventions.

  5. Meteoric 10Be in soil profiles - A global meta-analysis

    NASA Astrophysics Data System (ADS)

    Graly, Joseph A.; Bierman, Paul R.; Reusser, Lucas J.; Pavich, Milan J.

    2010-12-01

    In order to assess current understanding of meteoric 10Be dynamics and distribution in terrestrial soils, we assembled a database of all published meteoric 10Be soil depth profiles, including 104 profiles from 27 studies in globally diverse locations, collectively containing 679 individual measurements. This allows for the systematic comparison of meteoric 10Be concentration to other soil characteristics and the comparison of profile depth distributions between geologic settings. Percent clay, 9Be, and dithionite-citrate extracted Al positively correlate to meteoric 10Be in more than half of the soils where they were measured, but the lack of significant correlation in other soils suggests that no one soil factor controls meteoric 10Be distribution with depth. Dithionite-citrate extracted Fe and cation exchange capacity are only weakly correlated to meteoric 10Be. Percent organic carbon and pH are not significantly related to meteoric 10Be concentration when all data are complied. The compilation shows that meteoric 10Be concentration is seldom uniform with depth in a soil profile. In young or rapidly eroding soils, maximum meteoric 10Be concentrations are typically found in the uppermost 20 cm. In older, more slowly eroding soils, the highest meteoric 10Be concentrations are found at depth, usually between 50 and 200 cm. We find that the highest measured meteoric 10Be concentration in a soil profile is an important metric, as both the value and the depth of the maximum meteoric 10Be concentration correlate with the total measured meteoric 10Be inventory of the soil profile. In order to refine the use of meteoric 10Be as an estimator of soil erosion rate, we compare near-surface meteoric 10Be concentrations to total meteoric 10Be soil inventories. These trends are used to calibrate models of meteoric 10Be loss by soil erosion. Erosion rates calculated using this method vary based on the assumed depth and timing of erosional events and on the reference data selected.

  6. Meteoric 10Be in soil profiles - A global meta-analysis

    USGS Publications Warehouse

    Graly, Joseph A.; Bierman, Paul R.; Reusser, Lucas J.; Pavich, Milan J.

    2010-01-01

    In order to assess current understanding of meteoric 10Be dynamics and distribution in terrestrial soils, we assembled a database of all published meteoric 10Be soil depth profiles, including 104 profiles from 27 studies in globally diverse locations, collectively containing 679 individual measurements. This allows for the systematic comparison of meteoric 10Be concentration to other soil characteristics and the comparison of profile depth distributions between geologic settings. Percent clay, 9Be, and dithionite-citrate extracted Al positively correlate to meteoric 10Be in more than half of the soils where they were measured, but the lack of significant correlation in other soils suggests that no one soil factor controls meteoric 10Be distribution with depth. Dithionite-citrate extracted Fe and cation exchange capacity are only weakly correlated to meteoric 10Be. Percent organic carbon and pH are not significantly related to meteoric 10Be concentration when all data are complied.The compilation shows that meteoric 10Be concentration is seldom uniform with depth in a soil profile. In young or rapidly eroding soils, maximum meteoric 10Be concentrations are typically found in the uppermost 20 cm. In older, more slowly eroding soils, the highest meteoric 10Be concentrations are found at depth, usually between 50 and 200 cm. We find that the highest measured meteoric 10Be concentration in a soil profile is an important metric, as both the value and the depth of the maximum meteoric 10Be concentration correlate with the total measured meteoric 10Be inventory of the soil profile.In order to refine the use of meteoric 10Be as an estimator of soil erosion rate, we compare near-surface meteoric 10Be concentrations to total meteoric 10Be soil inventories. These trends are used to calibrate models of meteoric 10Be loss by soil erosion. Erosion rates calculated using this method vary based on the assumed depth and timing of erosional events and on the reference data selected.

  7. Seamounts Identified By High-Resolution Imagery Offshore Kenya

    NASA Astrophysics Data System (ADS)

    Henderson, J. F.; Kagasi, J.; Gikuhi, M.; Njuguna, S.

    2008-12-01

    Multibeam bathymetry and 2-D seismic reflection surveys were carried out between 2007 and 2008 by the Government of Kenya for the purpose of delineating Kenya's extended continental shelf beyond the 200 nautical mile boundary, as allowed under Article 76 of the United Nations Convention on the Law of the Sea (UNCLOS). The unique dataset acquired includes areas surveyed for the first time and provides new information on the geological processes of the continental shelf, slope and abyssal plain along the Kenyan passive margin. High-resolution multibeam bathymetry of almost the entire Kenyan continental slope was acquired using two multibeam systems (Kongsberg Simrad EM120 and EM710) aboard the M/V L'Espoir in November/December 2007. A multi-channel seismic survey followed in April/May 2008 (R/V Akademik Alexander Karpinsky) and provided high-resolution seismic reflection profiles. During these surveys, three features interpreted to be seamounts were discovered along Kenya's continental slope at water depths between 2750 and 3500 m. The size of the features varies from 2.5 to 10 km in diameter and 570 to 1740 m in height. The Davie Fracture Zone, a north-south trending transform fault was also identified in the seismic reflection profiles. The ridge, possibly extending from 26°S off south Madagascar to as far north as 2°S, is thought to have been created by the separation and direction of motion of Madagascar from Africa that began in the middle Jurassic. The discovery of these features and the integration of both multibeam bathymetry and seismic reflection profiles provides new information in the study of seamount distribution and their relationship to nearby transform faults.

  8. Volcanic inflation of Axial Seamount since the 1998 eruption

    NASA Astrophysics Data System (ADS)

    Nooner, S. L.; Chadwick, W.

    2010-12-01

    Since 2000, ambient seawater pressure has been precisely measured at five seafloor benchmarks inside the summit caldera at Axial Seamount in order to measure their relative depth and monitor volcanic inflation that has been occurring since an eruption in 1998. A remotely operated vehicle has been used to deploy a mobile pressure recorder (MPR) in campaign-style surveys, with additional seawater pressure data collected at the caldera center with multiyear deployments of continuously recording bottom pressure recorders (BPRs). Our previous measurements at Axial Seamount have shown steady inflation of the caldera center through 2007 and the spatial pattern of uplift has been consistent with magma storage in a shallow reservoir underlying the caldera at a depth of 3.5 km. This is the only location in the world where long-term monitoring of volcanic inflation has been accomplished at a submarine volcano. Here we present the results of new pressure data (both MPR and BPR) collected during a cruise on board the R/V Thomas Thompson in August-September 2010 and using the Jason ROV. Three years have passed since the previous survey, providing enough time to distinguish between two alternative models of inflation and magma recharge for the volcano. This allows us to refine our forecast for the next eruption at Axial and estimate total uplift that has occurred since the 1998 eruption. During the 2010 survey we also deployed new concrete benchmarks to replace our original galvanized steel benchmarks. The new benchmarks are larger and much heavier, and we expect them to be much more durable and stable over long time periods and help keep measurement errors as small as possible. We installed a sixth benchmark at a new site within the caldera, near the Ashes vent field, which will help constrain our modeling of the inflation signal in future years.

  9. Meteoric ion layers in the Martian atmosphere.

    PubMed

    Whalley, Charlotte L; Plane, John M C

    2010-01-01

    Low-lying plasma layers have been observed sporadically in the Martian atmosphere by radio occultation measurements from spacecraft such as the Mars Express Orbiter and the Mars Global Surveyor. These layers are just a few km wide, and tend to occur around 90 km. It has been proposed that the layers consist of metallic ions, for two reasons: they occur in the aerobraking region of the planet where meteoroids ablate; and they resemble sporadic E layers in the terrestrial atmosphere which are known to be composed principally of Fe+ and Mg+ ions. This paper addresses the problem of how metallic ions can persist in a CO2-rich atmosphere, where the ions should be neutralized rapidly by formation of metal-CO2 cluster ions followed by dissociative electron recombination. Laboratory studies using the pulsed laser photolysis/laser induced fluorescence and flow tube/mass spectrometer techniques were used to measure the following rate coefficients: k (Mg+ + CO2 (+ CO2) --> Mg+ x CO2, 190-403 K) = (5.3 +/- 0.7) x 10(-29) (T/300 K)(-1.86 +/- 0.03) cm6 molecule --> 2 s(-1); k(Mg+ x CO2 + O2 --> MgO2(+) + CO2, 297 K) = (2.2 +/- 0.8) x 10(-11) cm3 molecule(-1) s(-1); k(MgO2(+) + O --> MgO(+) + O2, 297 K) = (6.5 +/- 1.8) x 10(-10) cm3 molecule(-1) s(-1); and k(MgO(+) + O --> Mg(+) + O2, 297 K) = (5.9 +/- 2.4) x 10(-10) cm3 molecule(-1) s(-1). A model of magnesium and iron chemistry in the Martian atmosphere was then constructed, which includes meteoric differential ablation rates calculated with the Leeds CABMOD model, photo-ionization, and gas-phase ion-molecule and neutral chemistry. The model shows that nearly all the metallic ions between 70 and 110 km should be Mg+, because the reactions of MgO2+ and MgO+ with atomic O are fast enough to prevent these molecular ions undergoing dissociative electron recombination (unlike the analogous Fe species). There are enough Mg+ ions to form sporadic layers of the observed plasma density, and the layers can have a lifetime against

  10. Letter - Reply: Meteors in Australian Aboriginal Dreamings

    NASA Astrophysics Data System (ADS)

    Hamacher, Duane W.

    2011-06-01

    case in Australia, and along with Gorelli, I encourage WGN readers to get involved in studying meteoritic events in oral traditions. There is a lot of information regarding meteoritical events and phenomena in the literature that is still waiting to be collected and analysed ...and I applaud McBeath for his pursuit to publish this material through the successful Meteor Beliefs Project!

  11. Geophysical investigation of seamounts near the Ogasawara fracture zone, western Pacific

    USGS Publications Warehouse

    Lee, T.-G.; Lee, Kenneth; Hein, J.R.; Moon, J.-W.

    2009-01-01

    This paper provides an analysis of multi-channel seismic data obtained during 2000-2001 on seamounts near the Ogasawara Fracture Zone (OFZ) northwest of the Marshall Islands in the western Pacific. The OFZ is unique in that it is a wide rift zone that includes many seamounts. Seven units are delineated on the basis of acoustic characteristics and depth: three units (I, II, and III) on the summit of seamounts and four units (IV, V, VI, and VII) in basins. Acoustic characteristics of layers on the summit of guyots and dredged samples indicate that the seamounts had been built above sea level by volcanism. This was followed by reef growth along the summit margin, which enabled deposition of shallow-water carbonates on the summit, and finally by subsidence of the edifices. The subsidence depth of the seamounts, estimated from the lower boundary of unit II, ranges between 1,550 and 2,040 m. The thick unit I of the southern seamounts is correlated with proximity to the equatorial high productivity zone, whereas local currents may have strongly affected the distribution of unit I on northern seamounts. A seismic profile in the basin around the Ita Mai Tai and OSM4 seamounts shows an unconformity between units IV and V, which is widespread from the East Mariana Basin to the Pigafetta Basin. Copyright ?? The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB.

  12. Meteoric-like fabrics forming in marine waters. Implications for the use of petrography to identify diagenetic environments

    SciTech Connect

    Melim, L.A.; Swart, P.K.; Maliva, R.G.

    1995-08-01

    Petrographic fabrics have long been used to identify meteoric diagnesis of carbonate sediments. However, on the basis of oxygen isotopic data, we document similar fabrics forming in marine pore fluids in the shallow subsurface of Great Bahama Bank. Therefore, petrographic fabrics alone are not reliable indicators of diagenetic environments, even for shallow-water sediments. In our study, skeletal grainstones show two distinct diagenetic assemblages: either dissolution of aragonitic grains and minimal cementation (high-permeability intervals) or abundant blocky spar cement and neomorphism of aragonitic skeletal grains (low-permeability intervals). These marine-burial fabrics are present as shallow as 110 m below sea level, well above the aragonite compensation depth, a feature that must be considered for models of diagenesis in ancient carbonate sediments. Marine-burial diagenesis may be important in ancient carbonate sediments deposited in moderate water depths or in shallow water during rising sea level where meteoric diagenesis is suppressed. 17 refs., 5 figs.

  13. Meteoroids and Meteors - Observations and Connection to Parent Bodies

    NASA Astrophysics Data System (ADS)

    Abe, Shinsuke

    2009-05-01

    Meteoroid are a small rocky bodies traveling through interplanetary space. Meteors are phenomena caused by the interaction of meteoroids with the Earth's upper atmosphere. In this chapter the author, will briefly discuss observational methods and then concentrate on optical observations of meteors. First, the basic properties of meteor phenomenon in the atmosphere and classification of meteoroids are introduced and then coincidental phenomena, e.g., wake, jets, and train, are mentioned. Scientific observations (imaging and spectroscopy) carried out using various observational techniques allow measuring characteristics of meteoroids, e.g., orbits, density, strength, compositions. All information are potentially useful for investigating parent bodies of meteoroids, such as comets and asteroids. Searching for organics-related CHON and water in meteoroids is of particular interest for astrobiology.

  14. HRO New Radio Meteor Observation for Leonid Peak

    NASA Astrophysics Data System (ADS)

    Maegawa, Kimio

    Radio Meteor Observation(RMO) has advantages of continuation to optical observations which are interrupted by weather conditions and sun light. Amateur astronomers had been observing reflections from meteor trails using VHF(76-90MHz) FM broadcast radiowaves(FRO) since early 1970 in Japan. Recently,they have a problem of interferences caused by other FM radio station newly opened in various locations. I introduce a new Radio Meteor Observation (HRO) using Amateur Radio VHF(50MHz) wave and describe the echo detection capability and 12 month observation results. This method use continuous wave transmission and separate SSB mode reception. Echo signals are detected by FFT analysys and has good airplane echo rejection as well as 1000 times higher sensivity than FRO of same transmitter power. HRO will be useful to determine the peak activity of Leonids.

  15. The Leonid Meteors and Space Shuttle Risk Assessment

    NASA Technical Reports Server (NTRS)

    Pawlowski, James F.; Hebert, Thomas

    2000-01-01

    The November 1999 Leonid meteor shower was videotaped on the grounds of the NASA Johnson Space Center (JSC) and at the JSC Observatory in Cloudcroft, New Mexico. The videotapes were analyzed using a meteor analysis system developed at JSC. The results of the analysis were compared to the Leonid Meteors Mass Distribution Model derived at JSC and used for micrometeoroid and orbital debris risk assessment performed before each Space Shuttle mission. The observed data compared favorably to the model in the .001 to 0.2 gram range but diverged from the model for the smaller masses. We attribute the divergence to optical equipment limitations. These 1999 results will be compared with the 1998 results which were presented at the April 1999 Leonid Multi-Instrument Aircraft Campaign (MAC) Workshop.

  16. Comet Tempel-Tuttle and the Leonid meteors

    NASA Technical Reports Server (NTRS)

    Yeomans, D. K.

    1981-01-01

    The distribution of dust surrounding periodic comet Tempel-Tuttle has been mapped by analyzing the associated Leonid meteor shower data over the 902-1969 interval. The majority of dust ejected from the parent comet evolves to a position lagging the comet and outside the comet's orbit. Hence, it appears that radiation pressure and planetary perturbations, rather than ejection processes, control the dynamic evolution of the Leonid particles. Significant Leonid meteor showers are possible roughly 2500 days before or after the parent comet reaches perihelion, but only if the comet passes closer than 0.025 AU inside or 0.010 AU outside the earth's orbit. Although the conditions in 1998-1999 are optimum for a significant Leonid meteor shower, the event is not certain because the dust particle distribution near the comet is far from uniform. The orbit of comet Tempel-Tuttle has been redetermined for the 1366-1966 observed interval.

  17. PF191012 Myszyniec - highest Orionid meteor ever recorded

    NASA Astrophysics Data System (ADS)

    Olech, A.; Żołaḑek, P.; Wiśniewski, M.; Fietkiewicz, K.; Maciejewski, M.; Tymiński, Z.; Krzyżanowski, T.; Krasnowski, M.; Kwinta, M.; Myszkiewicz, M.; Polakowski, K.; Zarȩba, P.

    2013-09-01

    On the night of Oct. 18/19, 2012, at 00:23 UT, a -14.7 mag Orionid fireball occurred over northeastern Poland. The precise orbit and atmospheric trajectory of the event are presented, based on the data collected by five video stations and one photographic Polish Fireball Network station. The beginning height of the meteor is 168.4 ± 0.6 km, which makes the PF191012 Myszyniec fireball the highest ever observed, well-documented meteor not belonging to the Leonid shower. The ablation became the dominant source of light of the meteor at a height of around 115 km. The thermalization of sputtered particles is suggested to be the source of radiation above that value. The transition height of 115 km is 10-15 km below the transition heights derived for Leonids and might suggest that the material of Leonids is more fragile and probably has smaller bulk density than that of Orionids.

  18. Meteoric sphaerosiderite lines and their use for paleohydrology and paleoclimatology

    USGS Publications Warehouse

    Ludvigson, Greg A.; Gonzalez, Luis A.; Metzger, R.A.; Witzke, B.J.; Brenner, Richard L.; Murillo, A.P.; White, T.S.

    1998-01-01

    Sphaerosiderite, a morphologically distinct millimeter-scale spherulitic siderite (FeCO3), forms predominantly in wetland soils and sediments, and is common in the geologic record. Ancient sphaerosiderites are found in paleosol horizons within coal-bearing stratigraphic intervals and, like their modern counterparts, are interpreted as having formed in water-saturated environments. Here we report on sphaerosiderites from four different stratigraphic units, each of which has highly variable 13C and relatively stable 18O compositions. The unique isotopic trends are analogous to well-documented meteoric calcite lines, which we define here as meteoric sphaerosiderite lines. Meteoric sphaerosiderite lines provide a new means of constraining ground-water ??18O and thus allow evaluation of paleohydrology and paleoclimate in humid continental settings.

  19. Observation error propagation on video meteor orbit determination

    NASA Astrophysics Data System (ADS)

    SonotaCo

    2016-04-01

    A new radiant direction error computation method on SonotaCo Network meteor observation data was tested. It uses single station observation error obtained by reference star measurement and trajectory linearity measurement on each video, as its source error value, and propagates this to the radiant and orbit parameter errors via the Monte Carlo simulation method. The resulting error values on a sample data set showed a reasonable error distribution that makes accuracy-based selecting feasible. A sample set of selected orbits obtained by this method revealed a sharper concentration of shower meteor radiants than we have ever seen before. The simultaneously observed meteor data sets published by the SonotaCo Network will be revised to include this error value on each record and will be publically available along with the computation program in near future.

  20. Altitudinal dependence of meteor radio afterglows measured via optical counterparts

    NASA Astrophysics Data System (ADS)

    Obenberger, K. S.; Holmes, J. M.; Dowell, J. D.; Schinzel, F. K.; Stovall, K.; Sutton, E. K.; Taylor, G. B.

    2016-09-01

    Utilizing the all-sky imaging capabilities of the first station of the Long Wavelength Array along with a host of all-sky optical cameras, we have now observed 44 optical meteor counterparts to radio afterglows. Combining these observations, we have determined the geographic positions of all 44 afterglows. Comparing the number of radio detections as a function of altitude above sea level to the number of expected bright meteors, we find a strong altitudinal dependence characterized by a cutoff below ˜90 km, below which no radio emission occurs, despite the fact that many of the observed optical meteors penetrated well below this altitude. This cutoff suggests that wave damping from electron collisions is an important factor for the evolution of radio afterglows. This finding agrees with the hypothesis that the emission is the result of electron plasma wave emission.

  1. French Meteor Network for High Precision Orbits of Meteoroids

    NASA Technical Reports Server (NTRS)

    Atreya, P.; Vaubaillon, J.; Colas, F.; Bouley, S.; Gaillard, B.; Sauli, I.; Kwon, M. K.

    2011-01-01

    There is a lack of precise meteoroids orbit from video observations as most of the meteor stations use off-the-shelf CCD cameras. Few meteoroids orbit with precise semi-major axis are available using film photographic method. Precise orbits are necessary to compute the dust flux in the Earth s vicinity, and to estimate the ejection time of the meteoroids accurately by comparing them with the theoretical evolution model. We investigate the use of large CCD sensors to observe multi-station meteors and to compute precise orbit of these meteoroids. An ideal spatial and temporal resolution to get an accuracy to those similar of photographic plates are discussed. Various problems faced due to the use of large CCD, such as increasing the spatial and the temporal resolution at the same time and computational problems in finding the meteor position are illustrated.

  2. Constraining the Physical Properties of Meteor Stream Particles by Light Curve Shapes Using the Virtual Meteor Observatory

    NASA Technical Reports Server (NTRS)

    Koschny, D.; Gritsevich, M.; Barentsen, G.

    2011-01-01

    Different authors have produced models for the physical properties of meteoroids based on the shape of a meteor's light curve, typically from short observing campaigns. We here analyze the height profiles and light curves of approx.200 double-station meteors from the Leonids and Perseids using data from the Virtual Meteor Observatory, to demonstrate that with this web-based meteor database it is possible to analyze very large datasets from different authors in a consistent way. We compute the average heights for begin point, maximum luminosity, and end heights for Perseids and Leonids. We also compute the skew of the light curve, usually called the F-parameter. The results compare well with other author's data. We display the average light curve in a novel way to assess the light curve shape in addition to using the F-parameter. While the Perseids show a peaked light curve, the average Leonid light curve has a more flat peak. This indicates that the particle distribution of Leonid meteors can be described by a Gaussian distribution; the Perseids can be described with a power law. The skew for Leonids is smaller than for Perseids, indicating that the Leonids are more fragile than the Perseids.

  3. Fractures, not Plumes, Have Controlled Major Seamount Volcanism in the Pacific over 170 Million Years

    NASA Astrophysics Data System (ADS)

    Natland, J. H.; Winterer, E. L.

    2003-12-01

    The distribution of guyots and atolls and large volcanic islands on the Pacific plate can be used to outline the likely connection between stresses acting on the plate and the gradual development of large, linear volcanic chains over the past 170 Ma. We construe three general periods with different stress regimes in the history of the Pacific plate. 1) During the Jurassic and Early Cretaceous, the Pacific plate was surrounded by ridge segments and there were no major stress alignments within it. Within-plate volcanism thus assumed the scattered arrangement for the condition of no tectonic stress (1), and the large Magellan and Wake seamount clusters formed. Near the eastern boundaries of the plate, complex and shifting patterns of ridge reorganization dictated formation of very long, splayed, near-axis ridges such as Horizon Guyot and Necker Ridge. 2) At about 90 Ma, the growing middle-aged Pacific plate achieved its first persistent stress regime with the formation of subduction boundaries along its western or northwestern margin. The plate was no longer static but began to move over the asthenosphere and into the mantle. Subduction boundaries and the overall direction of subduction are uncertain, but this imparted a general yet not fully stable component of tension across the plate, producing the NNW Gilbert-Marshall, Line and Emperor Seamount ridges, generally orthogonal to the overall direction of least principal stress. The Line Island seamount chain, being near ridge axes, sustained a variable stress regime. It thus has no age progression of rocks dated between 70-90 Ma (2), great width, and a dual orientations of ridges. 3) By 47 Ma, nearly half of the boundaries of the Pacific plate now were trenches spanning from the Aleutians to New Zealand. In addition, northward migration of the Indian plate and Australia caught a major portion of the westerly moving Pacific plate between the northeast corner of the Tonga Trench and the Aleutians. The plate could not

  4. On Meteoric Dust Particles in the Near-Earth Space Environment

    NASA Astrophysics Data System (ADS)

    Mahmoudian, Alireza; Farahani, Majid Mazraeh Ei; Mohebalhojeh, Ali R.; Scales, Wayne

    2016-07-01

    Over 40 metric tons of meteoric dust enters the earth's atmosphere every day. This dust settles and creates natural dust layers in the altitude ranges between 80 and 100 kilometers which spans the earth's upper mesosphere to lower thermosphere. The dust layers in the lower atmosphere have a great impact on climate, human health as well as communication and navigation signals. The main goal of this study is the role of meteoric smoke particles on the formation of Polar Mesospheric Clouds (PMC). Recent rocket experiments have detected the presence of these particles. Since these dust layers are immersed in the earth's upper atmosphere, they become charged due to collection of electrons and ions from the earth's ionospheric plasma. Noctilucent Clouds NLCs are a fascinating visual manifestation of these dust layers. So-called Polar Mesospheric Summer Echoes PMSEs are radar echoes that are a direct consequence of the sub-visible charged dust that exists at altitudes above NLC regions. Polar Mesospheric Summer Echoes (PMSE) are strong echoes that have been typically observed in the frequency range from 50MHz to 1.3GHz and in the altitude about 85km. Unlike PMSE, Polar mesospheric winter echoes (PMWE) are less known. PMWE appear at a lower altitude and is weaker in comparison with PMSE. The focus of this study is on meteoric smoke particles and how they affect PMWE source region. Parameters associated with smoke dust particles such as size distribution, charging characteristics, density and positive or negative charge will be considered. The second part of this presentation will be on the effect of gravity waves on PMC. Full coupling to a turbulent neutral field with a statistical analysis will be discussed. Impact of a neutral turbulence driving field on small amplitude plasma fluctuations in such a configuration and some of the important consequences will be also presented. This has important consequences for electric field and potential measurements on rocket probes as

  5. CAMS newly detected meteor showers and the sporadic background

    NASA Astrophysics Data System (ADS)

    Jenniskens, P.; Nénon, Q.; Gural, P. S.; Albers, J.; Haberman, B.; Johnson, B.; Morales, R.; Grigsby, B. J.; Samuels, D.; Johannink, C.

    2016-03-01

    The Cameras for Allsky Meteor Surveillance (CAMS) video-based meteoroid orbit survey adds 60 newly identified showers to the IAU Working List of Meteor Showers (numbers 427, 445-446, 506-507, and part of 643-750). 28 of these are also detected in the independent SonotaCo survey. In total, 230 meteor showers and shower components are identified in CAMS data, 177 of which are detected in at least two independent surveys. From the power-law size frequency distribution of detected showers, we extrapolate that 36% of all CAMS-observed meteors originated from ∼700 showers above the N = 1 per 110,000 shower limit. 71% of mass falling to Earth from streams arrives on Jupiter-family type orbits. The transient Geminids account for another 15%. All meteoroids not assigned to streams form a sporadic background with highest detected numbers from the apex source, but with 98% of mass falling in from the antihelion source. Even at large ∼7-mm sizes, a Poynting-Robertson drag evolved population is detected, which implies that the Grün et al. collisional lifetimes at these sizes are underestimated by about a factor of 10. While these large grains survive collisions, many fade on a 104-y timescale, possibly because they disintegrate into smaller particles by processes other than collisions, leaving a more resilient population to evolve. The meteors assigned to the various showers are identified in the CAMS Meteoroid Orbit Database 2.0 submitted to the IAU Meteor Data Center, and can be accessed also at

  6. Prospects for meteor shower activity in the venusian atmosphere

    NASA Astrophysics Data System (ADS)

    Christou, Apostolos A.

    2004-03-01

    We investigate the possibility of detectable meteor shower activity in the atmosphere of Venus. We compare the Venus-approaching population of known periodic comets, suspected cometary asteroids and meteor streams with that of the Earth. We find that a similar number of Halley-type comets but a substantially lesser population of Jupiter family comets approach Venus. Parent bodies of prominent meteor showers that might occur at Venus have been determined based on minimum orbital distance. These are: Comets 1P/Halley, parent of the η Aquarid and Orionid streams at the Earth; 45P/Honda-Mrkos-Pajdusakova which currently approaches the venusian orbit to 0.0016 AU; three Halley-type comets (12P/Pons-Brooks, 27P/Crommelin and 122P/de Vico), all intercepting the planet's orbit within a 5-day arc in solar longitude; and Asteroid (3200) Phaethon, parent of the December Geminids at the Earth. In addition, several minor streams and a number of cometary asteroid orbits are found to approach the orbit of Venus sufficiently close to raise the possibility of some activity at that planet. Using an analytical approach described in Adolfsson et al. (Icarus 119 (1996) 144) we show that venusian meteors would be as bright or up to 2 magnitudes brighter than their Earth counterparts and reach maximum luminosity at an altitude range of 100-120, 20-30 km higher than at the Earth, in a predominantly clear region of the atmosphere. We discuss the feasibility of observing venusian showers based on current capabilities and conclude that a downward-looking Venus-orbiting meteor detector would be more suitable for these purposes than Earth-based monitoring. The former would detect a shower of an equivalent Zenithal Hourly Rate of at least several tens of meteors.

  7. Long-time observation of meteor induced layers with ionosonde

    NASA Astrophysics Data System (ADS)

    Yusupov, Kamil; Akchurin, Adel

    2016-07-01

    It is considered that the main theory explaining appearance of sporadic E is the theory of wind shear, which means (includes) the presence and movement of nodes converging tidal wind through the height region of the most frequent occurrence Es (120-140km) [Mathew et. all, 1998]. However, the appearance of intense layers, following its name, are sporadic, and such variability cannot to explain by the influence of tidal waves only. Another indication inconsistency theory of wind shear is the appearance of so-called transient Es layers [Maruiama, 2003]. The distinctive feature of this trace is the high critical frequency (> 5 MHz), a constant height, weak amplitude, all trace semitransparent and short lifetime [Maruiama et. all, 2003 and 2008 and references there]. Because of duration, such layer is opposite to the traditional persistent Es layer, which we do not consider in this paper. Various researchers have used different terms for such spontaneous Es, it is meteor echo, meteor induced Es, spontaneously formed sporadic Es patches resulting of the Fresnel scattering from a region of enhanced plasma density along the meteor trail, transitory Es and transient Es. Since the term transient Es is unstable, to avoid confusion, we will stick to this term. Since meteor echo is not fully satisfy this term by some parameter, we will describe the properties of transient Es based on the ionogram properties and not from physics of its origin. We used data from our ionosonde with one-minute ionogram repetition rate for 2010-2014 years. For processing performed a method are using to select beatings and the ionosphere reflectivity of the layers by means A-, H-and AΣ-map [Akchurin, 2011; Yusupov, 2014]. This maps allow to collect transient Es appearance over a long-time. Such statistics comparison with meteor showers activity showed good agreement. It shows the presence of the transient Es formation mechanism, which coupling with meteors.

  8. A new approach to compute accurate velocity of meteors

    NASA Astrophysics Data System (ADS)

    Egal, Auriane; Gural, Peter; Vaubaillon, Jeremie; Colas, Francois; Thuillot, William

    2016-10-01

    The CABERNET project was designed to push the limits of meteoroid orbit measurements by improving the determination of the meteors' velocities. Indeed, despite of the development of the cameras networks dedicated to the observation of meteors, there is still an important discrepancy between the measured orbits of meteoroids computed and the theoretical results. The gap between the observed and theoretic semi-major axis of the orbits is especially significant; an accurate determination of the orbits of meteoroids therefore largely depends on the computation of the pre-atmospheric velocities. It is then imperative to dig out how to increase the precision of the measurements of the velocity.In this work, we perform an analysis of different methods currently used to compute the velocities and trajectories of the meteors. They are based on the intersecting planes method developed by Ceplecha (1987), the least squares method of Borovicka (1990), and the multi-parameter fitting (MPF) method published by Gural (2012).In order to objectively compare the performances of these techniques, we have simulated realistic meteors ('fakeors') reproducing the different error measurements of many cameras networks. Some fakeors are built following the propagation models studied by Gural (2012), and others created by numerical integrations using the Borovicka et al. 2007 model. Different optimization techniques have also been investigated in order to pick the most suitable one to solve the MPF, and the influence of the geometry of the trajectory on the result is also presented.We will present here the results of an improved implementation of the multi-parameter fitting that allow an accurate orbit computation of meteors with CABERNET. The comparison of different velocities computation seems to show that if the MPF is by far the best method to solve the trajectory and the velocity of a meteor, the ill-conditioning of the costs functions used can lead to large estimate errors for noisy

  9. Isolated communities of Epsilonproteobacteria in hydrothermal vent fluids of the Mariana Arc seamounts.

    PubMed

    Huber, Julie A; Cantin, Holly V; Huse, Susan M; Welch, David B Mark; Sogin, Mitchell L; Butterfield, David A

    2010-09-01

    Low-temperature hydrothermal vent fluids represent access points to diverse microbial communities living in oceanic crust. This study examined the distribution, relative abundance, and diversity of Epsilonproteobacteria in 14 low-temperature vent fluids from five volcanically active seamounts of the Mariana Arc using a 454 tag sequencing approach. Most vent fluids were enriched in cell concentrations compared with background seawater, and quantitative PCR results indicated that all fluids were dominated by bacteria. Operational taxonomic unit-based statistical tools applied to 454 data show that all vents from the northern end of the Mariana Arc grouped together, to the exclusion of southern arc seamounts, which were as distinct from one another as they were from northern seamounts. Statistical analysis also showed a significant relationship between seamount and individual vent groupings, suggesting that community membership may be linked to geographical isolation and not geochemical parameters. However, while there may be large-scale geographic differences, distance is not the distinguishing factor in the microbial community composition. At the local scale, most vents host a distinct population of Epsilonproteobacteria, regardless of seamount location. This suggests that there may be barriers to exchange and dispersal for these vent endemic microorganisms at hydrothermal seamounts of the Mariana Arc. PMID:20533947

  10. Sea-surface and deep-magnetic data at Vavilov Seamount, Tyrrhenian Sea

    NASA Astrophysics Data System (ADS)

    Muccini, Filippo; Cocchi, Luca; Locritani, Marina; Carmisciano, Cosmo

    2016-04-01

    Sea surface and deep magnetic data were acquired at Vavilov seamount, in the Tyrrhenian sea. Vavilov seamount is located in the central portion of the homonymous Vavilov basin. The seamount stands about 2800 meters above the seafloor at 3600 meters depth, with the top at about 800 meters below the sea level. Oceanization of the basin occurred during the Late Miocene-Early Pliocene. The magnetic data were collected in 2011 on board the Nave Ammiraglio Magnaghi by using a Marine Magnetics Seaspy magnetometer. The sea surface magnetic survey was realized with two different grids: the first regional one, with 13 parallel lines about 43 Km long, 3 Km spaced (104° N oriented) and 6 tie control lines about 40 Km long, 5 Km spaced (014° N oriented). The second one was realized to better define the volcanic structure of the seamount, and was achieved by acquiring 12 magnetic parallel lines (104° N), 18 Km long and 1 Km spaced. The deep magnetic data were collected by towing a magnetic sensor coupled with a L3 sidescan sonar Klein 3000. A set of 5 parallel lines were acquired in correspondence of the bathymetric top of the seamount with the sensor flying at about constant depth of 700 meters. These data represents the first near-bottom magnetic data collected for Vavilov seamount and it allows comparison between sea-surface and deep magnetic data.

  11. Isolated communities of Epsilonproteobacteria in hydrothermal vent fluids of the Mariana Arc seamounts.

    PubMed

    Huber, Julie A; Cantin, Holly V; Huse, Susan M; Welch, David B Mark; Sogin, Mitchell L; Butterfield, David A

    2010-09-01

    Low-temperature hydrothermal vent fluids represent access points to diverse microbial communities living in oceanic crust. This study examined the distribution, relative abundance, and diversity of Epsilonproteobacteria in 14 low-temperature vent fluids from five volcanically active seamounts of the Mariana Arc using a 454 tag sequencing approach. Most vent fluids were enriched in cell concentrations compared with background seawater, and quantitative PCR results indicated that all fluids were dominated by bacteria. Operational taxonomic unit-based statistical tools applied to 454 data show that all vents from the northern end of the Mariana Arc grouped together, to the exclusion of southern arc seamounts, which were as distinct from one another as they were from northern seamounts. Statistical analysis also showed a significant relationship between seamount and individual vent groupings, suggesting that community membership may be linked to geographical isolation and not geochemical parameters. However, while there may be large-scale geographic differences, distance is not the distinguishing factor in the microbial community composition. At the local scale, most vents host a distinct population of Epsilonproteobacteria, regardless of seamount location. This suggests that there may be barriers to exchange and dispersal for these vent endemic microorganisms at hydrothermal seamounts of the Mariana Arc.

  12. About comparative models of meteor orbital data for different radars

    NASA Astrophysics Data System (ADS)

    Kolomiyets, Svitlana

    2016-07-01

    There is an electronic data base (~ 250, 000 orbits of faint radar meteors till +12^M) in the Kashcheyev LAB of KhNURE (Kharkiv, Ukraine). It is important if this data base will become open. Two scientific teams (from New Zealand and from Canada) are the principal expert on similar radar dataset (~500,000 and more than 3 million, respectively). The Kharkiv team will prepare the data for implementation in the IAU Meteor Data Centre and the virtual Observatory. We will develop a standard model for comparison of data from different radars.

  13. Automatic Analysis of Radio Meteor Events Using Neural Networks

    NASA Astrophysics Data System (ADS)

    Roman, Victor Ştefan; Buiu, Cătălin

    2015-12-01

    Meteor Scanning Algorithms (MESCAL) is a software application for automatic meteor detection from radio recordings, which uses self-organizing maps and feedforward multi-layered perceptrons. This paper aims to present the theoretical concepts behind this application and the main features of MESCAL, showcasing how radio recordings are handled, prepared for analysis, and used to train the aforementioned neural networks. The neural networks trained using MESCAL allow for valuable detection results, such as high correct detection rates and low false-positive rates, and at the same time offer new possibilities for improving the results.

  14. Software tools for the analysis of video meteors emission spectra

    NASA Astrophysics Data System (ADS)

    Madiedo, J. M.; Toscano, F. M.; Trigo-Rodriguez, J. M.

    2011-10-01

    One of the goals of the SPanish Meteor Network (SPMN) is related to the study of the chemical composition of meteoroids by analyzing the emission spectra resulting from the ablation of these particles of interplanetary matter in the atmosphere. With this aim, some of the CCD video devices we employ to observe the nigh sky are endowed with holographic diffraction gratings, and a continuous monitoring of meteor activity is performed. We have recently developed a new software to analyze these spectra. A description of this computer program is given, and some of the results obtained so far are presented here.

  15. Physics-Based Modeling of Meteor Entry and Breakup

    NASA Technical Reports Server (NTRS)

    Prabhu, Dinesh K.; Agrawal, Parul; Allen, Gary A., Jr.; Bauschlicher, Charles W., Jr.; Brandis, Aaron M.; Chen, Yih-Kang; Jaffe, Richard L.; Palmer, Grant E.; Saunders, David A.; Stern, Eric C.; Tauber, Michael E.; Venkatapathy, Ethiraj

    2015-01-01

    A new research effort at NASA Ames Research Center has been initiated in Planetary Defense, which integrates the disciplines of planetary science, atmospheric entry physics, and physics-based risk assessment. This paper describes work within the new program and is focused on meteor entry and breakup.Over the last six decades significant effort was expended in the US and in Europe to understand meteor entry including ablation, fragmentation and airburst (if any) for various types of meteors ranging from stony to iron spectral types. These efforts have produced primarily empirical mathematical models based on observations. Weaknesses of these models, apart from their empiricism, are reliance on idealized shapes (spheres, cylinders, etc.) and simplified models for thermal response of meteoritic materials to aerodynamic and radiative heating. Furthermore, the fragmentation and energy release of meteors (airburst) is poorly understood.On the other hand, flight of human-made atmospheric entry capsules is well understood. The capsules and their requisite heatshields are designed and margined to survive entry. However, the highest speed Earth entry for capsules is 13 kms (Stardust). Furthermore, Earth entry capsules have never exceeded diameters of 5 m, nor have their peak aerothermal environments exceeded 0.3 atm and 1 kW/sq cm. The aims of the current work are: (i) to define the aerothermal environments for objects with entry velocities from 13 to 20 kms; (ii) to explore various hypotheses of fragmentation and airburst of stony meteors in the near term; (iii) to explore the possibility of performing relevant ground-based tests to verify candidate hypotheses; and (iv) to quantify the energy released in airbursts. The results of the new simulations will be used to anchor said risk assessment analyses. With these aims in mind, state-of-the-art entry capsule design tools are being extended for meteor entries. We describe: (i) applications of current simulation tools to

  16. Physics-Based Modeling of Meteor Entry and Breakup

    NASA Technical Reports Server (NTRS)

    Prabhu, Dinesh K.; Agrawal, Parul; Allen, Gary A.; Brandis, Aaron M.; Chen, Yih-Kanq; Jaffe, Richard L.; Saunders, David A.; Stern, Eric C.; Tauber, Michael E.; Venkatapathy, Ethiraj

    2015-01-01

    A new research effort at NASA Ames Research Center has been initiated in Planetary Defense, which integrates the disciplines of planetary science, atmospheric entry physics, and physics-based risk assessment. This paper describes work within the new program and is focused on meteor entry and breakup. Over the last six decades significant effort was expended in the US and in Europe to understand meteor entry including ablation, fragmentation and airburst (if any) for various types of meteors ranging from stony to iron spectral types. These efforts have produced primarily empirical mathematical models based on observations. Weaknesses of these models, apart from their empiricism, are reliance on idealized shapes (spheres, cylinders, etc.) and simplified models for thermal response of meteoritic materials to aerodynamic and radiative heating. Furthermore, the fragmentation and energy release of meteors (airburst) is poorly understood. On the other hand, flight of human-made atmospheric entry capsules is well understood. The capsules and their requisite heatshields are designed and margined to survive entry. However, the highest speed Earth entry for capsules is less than 13 km/s (Stardust). Furthermore, Earth entry capsules have never exceeded diameters of 5 m, nor have their peak aerothermal environments exceeded 0.3 atm and 1 kW/cm2. The aims of the current work are: (i) to define the aerothermal environments for objects with entry velocities from 13 to greater than 20 km/s; (ii) to explore various hypotheses of fragmentation and airburst of stony meteors in the near term; (iii) to explore the possibility of performing relevant ground-based tests to verify candidate hypotheses; and (iv) to quantify the energy released in airbursts. The results of the new simulations will be used to anchor said risk assessment analyses. With these aims in mind, state-of-the-art entry capsule design tools are being extended for meteor entries. We describe: (i) applications of current

  17. Physics-Based Modeling of Meteor Entry and Breakup

    NASA Technical Reports Server (NTRS)

    Prabhu, Dinesh K.; Agrawal, Parul; Allen, Gary A., Jr.; Bauschlicher, Charles W., Jr.; Brandis, Aaron M.; Chen, Yih-Kanq; Jaffe, Richard L.; Palmer, Grant E.; Saunders, David A.; Stern, Eric C.; Tauber, Michael E.; Venkatapathy, Ethiraj

    2015-01-01

    A new research effort at NASA Ames Research Center has been initiated in Planetary Defense, which integrates the disciplines of planetary science, atmospheric entry physics, and physics-based risk assessment. This paper describes work within the new program and is focused on meteor entry and breakup. Over the last six decades significant effort was expended in the US and in Europe to understand meteor entry including ablation, fragmentation and airburst (if any) for various types of meteors ranging from stony to iron spectral types. These efforts have produced primarily empirical mathematical models based on observations. Weaknesses of these models, apart from their empiricism, are reliance on idealized shapes (spheres, cylinders, etc.) and simplified models for thermal response of meteoritic materials to aerodynamic and radiative heating. Furthermore, the fragmentation and energy release of meteors (airburst) is poorly understood. On the other hand, flight of human-made atmospheric entry capsules is well understood. The capsules and their requisite heat shields are designed and margined to survive entry. However, the highest speed Earth entry for capsules is 13 kms (Stardust). Furthermore, Earth entry capsules have never exceeded diameters of 5 m, nor have their peak aerothermal environments exceeded 0.3 atm and 1 kWcm2. The aims of the current work are: (i) to define the aerothermal environments for objects with entry velocities from 13 to 20 kms; (ii) to explore various hypotheses of fragmentation and airburst of stony meteors in the near term; (iii) to explore the possibility of performing relevant ground-based tests to verify candidate hypotheses; and (iv) to quantify the energy released in airbursts. The results of the new simulations will be used to anchor said risk assessment analyses.With these aims in mind, state-of-the-art entry capsule design tools are being extended for meteor entries. We describe: (i) applications of current simulation tools to

  18. The METEOR trial: no rush to repair a torn meniscus.

    PubMed

    Hwang, Yong Gil; Kwoh, C Kent

    2014-04-01

    It is uncertain whether arthroscopic partial meniscectomy is better than physical therapy in patients who have a symptomatic torn meniscus on top of osteoarthritis of the knee. The Meniscal Repair in Osteoarthritis Research (METEOR) trial concluded that physical therapy is acceptable at first, and that surgery is not routinely needed. In patients assigned to physical therapy who eventually needed surgery, the delay resulting from a trial of conservative management did not impair outcomes at 12 months from the initial presentation. Here, we analyze the background, design, findings, and clinical implications of the METEOR trial. PMID:24692441

  19. The Method of Selection of Major-Shower Meteors Revisited

    NASA Astrophysics Data System (ADS)

    Neslušan, L.; Svoreň, J.; Porubčan, V.

    2013-02-01

    We apply so-called break-point method to select the dense cores of 10 major meteor showers from the photographic, video, and radio-meteor databases. The major showers can well be selected from photographic and video data, in a lesser degree from radio data. The obtained mean characteristics of Quadrantids, Lyrids, η-Aquarids, α-Capricornids, δ-Aquarids N, δ-Aquarids S, Perseids, Orionids, Leonids, and Geminids are presented. A test to indicate the existence of a suspected shower in radio database is suggested.

  20. Modelling meteor phenomena in the atmospheres of the Terrestrial planets.

    NASA Astrophysics Data System (ADS)

    McAuliffe, J.

    The results of a comparative study of meteor phenomena in the atmospheres of the Earth, Mars and Venus are presented. The study has sought to quantify the scientific potential of future off-Earth observational campaigns. A pseudo-thermal meteor ablation model has been developed and shown to be capable of reproducing observed terrestrial light curves. This model has been used to simulate the ablation of meteoroids of 10-9 to 10-1 kg in the atmospheres of the three planets, and the resulting differences in meteor brightness, ablation heights, and durations have been investigated. Cometary meteoroids are found to ablate 5-25 km higher up at Venus than at the Earth with this difference increasing to 15-35 km for dense asteroidal particles. The associated peak brightnesses are found to be on the order 1.0 to 1.5 magnitudes brighter at Venus. Furthermore, steeper atmospheric density gradients at Venusian ablation heights result in meteor visibility times at Venus being on the order of 0.75 times as long as for similar particles at the Earth. Actual visibility times range from 100 ms to 2 seconds. The similar density gradients of the Martian and Terrestrial atmospheres at ablation altitudes result in Martian meteors being only ˜0.1 magnitudes fainter than Terrestrial equivalents. Due to the downward shift of the ablative atmospheric density interval at Mars, cometary meteors reach maximum brightness at altitudes 10-15 km less than would identical particles at the Earth. For asteroidal meteoroids this downward shift in the Martian atmosphere is ˜20 km. Visibility times for identical meteors at the Earth and Mars are found to differ by no more than 0.2 seconds. Surface and orbital observational systems have been simulated in order to estimate the relative detectability of some 20 real, possible and hypothetical showers and storms in all three atmospheres. Mass distributions for Martian and Venusian showers were estimated from the observed characteristics of Terrestrial