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  • 1
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    Suprathermal electron penetration into the inner magnetosphere of Saturn (2016)
    Wiley
    Details
    Publication Date: 2016-06-08
    Description: For most Cassini passes through the inner magnetosphere of Saturn, the hot-electron population (〉 few hundred eV) largely disappears inside of some cut-off L-shell. Anode-and-actuation-angle averages of hot-electron fluxes observed by the Cassini Electron Spectrometer (ELS) are binned into 0.1-R s bins in dipole L to explore the properties of this cutoff distance. The cut-off L-shell is quite variable from pass to pass (on time scales as short as 10-20 h). At energies of 5797 eV, 2054 eV, and 728 eV, 90% of the inner boundary values lie between L ~ 4.7 and 8.4, with a median near L = 6.2, consistent with the range of L values over which discrete interchange injections have been observed, thus strengthening the case that the interchange process is responsible for delivering the bulk of the hot electrons seen in the inner magnetosphere. The occurrence distribution of the inner boundary is more sharply peaked on the night side than at other local times. There is no apparent dependence of the depth of penetration on large-scale solar wind properties. It appears likely that internal processes (magnetic stress on mass-loaded flux tubes) are dominating the injection of hot electrons into the inner magnetosphere.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Search for Saturn's X-ray aurorae at the arrival of a solar wind shock (2013)
    Wiley
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    Publication Date: 2013-01-17
    Description: [1]  After a decade of observations, evidence for X-ray auroral emission from Saturn has yet to be found. By analogy with processes known to take place on Jupiter, Saturnian X-ray aurorae may be expected to be powered by charge exchange (CX) between energetic ions and the planet's atmospheric neutrals; if the ions are of solar origin, the emission should be brightest during episodes of enhanced solar wind (SW). We have explored this possibility by propagating SW parameters measured near the Earth to Saturn, and triggering X-ray observations at the time SW enhancements were expected to reach the planet. This was done in April–May 2011 with the Chandra X-ray Observatory, and we report on two observations carried out at the time when a significant SW disturbance reached Saturn, as indicated by Cassini magnetic field, plasma and radio measurements: variability is observed between the two Chandra datasets, but we do not find evidence for X-ray brightening in the auroral regions. The variability can be explained by scattering of solar X-rays in Saturn's atmosphere during an episode of solar X-ray flaring. We conclude that the strength of any CX auroral X-ray emission on Saturn was below Chandra's detectability threshold. By-products of this investigation are stringent upper limits on the X-ray emission of Titan and Enceladus. The Cassini measurements concurrent with the Chandra observations confirm and pinpoint temporally the arrival of the SW enhancement at Saturn. SW propagation predictions are a useful tool for investigating and interpreting the effects of SW interactions with planetary environments.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    Earth-based detection of Uranus' aurorae (2012)
    Wiley
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    Publication Date: 2012-04-14
    Description: This study is based on multi-planet multi-wavelength observations of planetary aurorae throughout the heliosphere, acquired along the propagation path of a series of consecutive interplanetary shocks. The underlying motivation to track the shocks was to increase the probability of detection of auroral emissions at Uranus. Despite several Earth-based attempts in the past few years, at Far-UV (FUV) and Near-IR (NIR) wavelengths, such emissions have never been unambiguously re-observed since their discovery by Voyager 2 in 1986. Here, we present a campaign of FUV observations of Uranus obtained in November 2011 with the Hubble Space Telescope (HST) during active solar wind conditions. We positively identify auroral signatures in several of these HST measurements, together with some obtained in 1998, representing the first images of Uranus' aurorae. We analyze their characteristics and discuss the implications for the asymmetric Uranian magnetosphere and its highly variable interaction with the solar wind flow from near-solstice (1986) to near-equinox (2011) configurations.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 4
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    Electron heating at Saturn's bow shock (2011)
    Wiley
    Details
    Publication Date: 2011-10-28
    Description: Collisionless shock waves are a widespread phenomenon in both solar system and astrophysical contexts. The nature of energy dissipation at such shocks is of particular interest, especially at high Mach numbers. We use data taken by the Cassini spacecraft to investigate electron heating at Saturn's bow shock, one of the strongest collisionless shocks encountered by spacecraft to date. Measurements of the upstream solar wind ion parameters are scarce due to spacecraft pointing constraints and the absence of an upstream monitor. To address this, we use solar wind speed predictions from the Michigan Solar Wind Model. Since these model predictions are based on near-Earth solar wind measurements, we restrict our analysis to bow shock crossings made by Cassini within ±75 days of apparent opposition of Earth and Saturn. An analysis of the resulting set of 94 crossings made in 2005 and 2007 reveals a positive correlation between the electron temperature increase across the shock and the kinetic energy of an incident proton, where electron heating accounts for between ∼3% and ∼7% of this incident ram energy. This percentage decreases with increasing Alfvén Mach number, a trend that we confirm continues into the hitherto poorly explored high–Mach number regime, up to an Alfvén Mach number of ∼150. This work reveals that further studies of the Saturnian bow shock will bridge the gap between the more modest Mach numbers encountered in near-Earth space and more exotic astrophysical regimes where shock processes play central roles.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 5
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    A new semiempirical model of Saturn's bow shock based on propagated solar wind parameters (2011)
    Wiley
    Details
    Publication Date: 2011-07-02
    Description: A new semiempirical model of Saturn's dayside bow shock is presented. The model uses observations made during the Pioneer 11, Voyager 1, and Voyager 2 flybys as well as data from the first 6 years of the Cassini mission (2004–2010) to derive the average shape of the shock surface and the variation of shock subsolar distance with solar wind dynamic pressure. The 574 bow shock crossings used to construct the model provide good local time coverage of the dayside shock surface up to latitudes of roughly 45°, allowing the three-dimensional shape of the shock surface to be investigated for the first time. Narrowband Langmuir waves observed by the Radio and Plasma Wave Science instrument are combined with propagated solar wind velocities in order to estimate the solar wind dynamic pressure associated with each of the Cassini crossings. An axisymmetric second-order surface is then fit to the resulting crossing distribution, self-consistently accounting for solar wind dynamic pressure variations. The new semiempirical model is compared with existing models of Saturn's bow shock and magnetopause, and the physical implications of the model are discussed. On the basis of these comparisons, it is proposed that the new semiempirical model is the most accurate representation of Saturn's bow shock surface to date.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 6
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    CBP/p300-mediated acetylation of histone H3 on lysine 56 (2009)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2009-03-10
    Description: Acetylation within the globular core domain of histone H3 on lysine 56 (H3K56) has recently been shown to have a critical role in packaging DNA into chromatin following DNA replication and repair in budding yeast. However, the function or occurrence of this specific histone mark has not been studied in multicellular eukaryotes, mainly because the Rtt109 enzyme that is known to mediate acetylation of H3K56 (H3K56ac) is fungal-specific. Here we demonstrate that the histone acetyl transferase CBP (also known as Nejire) in flies and CBP and p300 (Ep300) in humans acetylate H3K56, whereas Drosophila Sir2 and human SIRT1 and SIRT2 deacetylate H3K56ac. The histone chaperones ASF1A in humans and Asf1 in Drosophila are required for acetylation of H3K56 in vivo, whereas the histone chaperone CAF-1 (chromatin assembly factor 1) in humans and Caf1 in Drosophila are required for the incorporation of histones bearing this mark into chromatin. We show that, in response to DNA damage, histones bearing acetylated K56 are assembled into chromatin in Drosophila and human cells, forming foci that colocalize with sites of DNA repair. Furthermore, acetylation of H3K56 is increased in multiple types of cancer, correlating with increased levels of ASF1A in these tumours. Our identification of multiple proteins regulating the levels of H3K56 acetylation in metazoans will allow future studies of this critical and unique histone modification that couples chromatin assembly to DNA synthesis, cell proliferation and cancer.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC2756583/" target="_blank"〉〈img src="https://static.pubmed.gov/portal/portal3rc.fcgi/4089621/img/3977009" border="0"〉〈/a〉   〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC2756583/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Das, Chandrima -- Lucia, M Scott -- Hansen, Kirk C -- Tyler, Jessica K -- CA95641/CA/NCI NIH HHS/ -- GM64475/GM/NIGMS NIH HHS/ -- R01 CA095641/CA/NCI NIH HHS/ -- R01 CA095641-07/CA/NCI NIH HHS/ -- R01 GM064475/GM/NIGMS NIH HHS/ -- R01 GM064475-07/GM/NIGMS NIH HHS/ -- England -- Nature. 2009 May 7;459(7243):113-7. doi: 10.1038/nature07861. Epub 2009 Mar 8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Biochemistry and Molecular Genetics, University of Colorado School of Medicine, PO Box 6511, Aurora Colorado 80045, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19270680" target="_blank"〉PubMed〈/a〉
    Keywords: Acetylation ; Animals ; Cell Cycle Proteins/metabolism ; Cell Line ; Chromosomal Proteins, Non-Histone/metabolism ; DNA Damage/physiology ; Drosophila Proteins/metabolism ; Drosophila melanogaster/*enzymology ; HeLa Cells ; Histone Deacetylases/metabolism ; Histones/*metabolism ; Humans ; Lysine/*metabolism ; Molecular Chaperones/metabolism ; Retinoblastoma-Binding Protein 4 ; Sirtuin 1 ; Sirtuin 2 ; Sirtuins/metabolism ; p300-CBP Transcription Factors/*metabolism
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 7
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    Saturn's variable magnetosphere (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-02-26
    Description: Since the Cassini spacecraft reached Saturn's orbit in 2004, its instruments have been sending back a wealth of data on the planet's magnetosphere (the region dominated by the magnetic field of the planet). In this Viewpoint, we discuss some of these results, which are reported in a collection of reports in this issue. The magnetosphere is shown to be highly variable and influenced by the planet's rotation, sources of plasma within the planetary system, and the solar wind. New insights are also gained into the chemical composition of the magnetosphere, with surprising results. These early results from Cassini's first orbit around Saturn bode well for the future as the spacecraft continues to orbit the planet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gombosi, Tamas I -- Hansen, Kenneth C -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1224-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Center for Space Environment Modeling, Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI 48109, USA. tamas@umich.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731438" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Hydrogen ; Ions ; *Magnetics ; Nitrogen ; *Saturn ; Spacecraft ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    Molecular nitrogen in comet 67P/Churyumov-Gerasimenko indicates a low formation temperature (2015)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2015-03-21
    Description: Molecular nitrogen (N2) is thought to have been the most abundant form of nitrogen in the protosolar nebula. It is the main N-bearing molecule in the atmospheres of Pluto and Triton and probably the main nitrogen reservoir from which the giant planets formed. Yet in comets, often considered the most primitive bodies in the solar system, N2 has not been detected. Here we report the direct in situ measurement of N2 in the Jupiter family comet 67P/Churyumov-Gerasimenko, made by the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis mass spectrometer aboard the Rosetta spacecraft. A N2/CO ratio of (5.70 +/- 0.66) x 10(-3) (2sigma standard deviation of the sampled mean) corresponds to depletion by a factor of ~25.4 +/- 8.9 as compared to the protosolar value. This depletion suggests that cometary grains formed at low-temperature conditions below ~30 kelvin.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Rubin, M -- Altwegg, K -- Balsiger, H -- Bar-Nun, A -- Berthelier, J-J -- Bieler, A -- Bochsler, P -- Briois, C -- Calmonte, U -- Combi, M -- De Keyser, J -- Dhooghe, F -- Eberhardt, P -- Fiethe, B -- Fuselier, S A -- Gasc, S -- Gombosi, T I -- Hansen, K C -- Hassig, M -- Jackel, A -- Kopp, E -- Korth, A -- Le Roy, L -- Mall, U -- Marty, B -- Mousis, O -- Owen, T -- Reme, H -- Semon, T -- Tzou, C-Y -- Waite, J H -- Wurz, P -- New York, N.Y. -- Science. 2015 Apr 10;348(6231):232-5. doi: 10.1126/science.aaa6100. Epub 2015 Mar 19.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. martin.rubin@space.unibe.ch. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Center for Space and Habitability, University of Bern, Sidlerstrasse. 5, CH-3012 Bern, Switzerland. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. ; Department of Geoscience, Tel-Aviv University, Ramat-Aviv, Tel-Aviv, Israel. ; Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS)/Institute Pierre Simon Laplace-CNRS-UPMC-UVSQ, 4 Avenue de Neptune F-94100, Saint-Maur, France. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA. ; Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), UMR 6115 CNRS-Universite d'Orleans, Orleans, France. ; Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA. ; Belgian Institute for Space Aeronomy, Belgisch Instituut voor Ruimte-Aeronomie-Institut d'Aeronomie Spatiale de Belgique (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium. ; Institute of Computer and Network Engineering, Technische Universitat Braunschweig, Hans-Sommer-Strasse 66, D-38106 Braunschweig, Germany. ; Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; Center for Space and Habitability, University of Bern, Sidlerstrasse. 5, CH-3012 Bern, Switzerland. ; Centre de Recherches Petrographiques et Geochimiques (CRPG)-CNRS, Universite de Lorraine, 15 rue Notre Dame des Pauvres, Boite Postale 20, 54501 Vandoeuvre les Nancy, France. ; Aix Marseille Universite, CNRS, Laboratoire d'Astrophysique de Marseille UMR 7326, 13388, Marseille, France. ; Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA. ; Universite de Toulouse; UPS-OMP; Institut de Recherche en Astrophysique et Planetologie (IRAP), Toulouse, France. CNRS; IRAP; 9 Avenue du Colonel Roche, Boite Postale 44346, F-31028 Toulouse Cedex 4, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25791084" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 9
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    Cometary science. Time variability and heterogeneity in the coma of 67P/Churyumov-Gerasimenko (2015)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2015-01-24
    Description: Comets contain the best-preserved material from the beginning of our planetary system. Their nuclei and comae composition reveal clues about physical and chemical conditions during the early solar system when comets formed. ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) onboard the Rosetta spacecraft has measured the coma composition of comet 67P/Churyumov-Gerasimenko with well-sampled time resolution per rotation. Measurements were made over many comet rotation periods and a wide range of latitudes. These measurements show large fluctuations in composition in a heterogeneous coma that has diurnal and possibly seasonal variations in the major outgassing species: water, carbon monoxide, and carbon dioxide. These results indicate a complex coma-nucleus relationship where seasonal variations may be driven by temperature differences just below the comet surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hassig, M -- Altwegg, K -- Balsiger, H -- Bar-Nun, A -- Berthelier, J J -- Bieler, A -- Bochsler, P -- Briois, C -- Calmonte, U -- Combi, M -- De Keyser, J -- Eberhardt, P -- Fiethe, B -- Fuselier, S A -- Galand, M -- Gasc, S -- Gombosi, T I -- Hansen, K C -- Jackel, A -- Keller, H U -- Kopp, E -- Korth, A -- Kuhrt, E -- Le Roy, L -- Mall, U -- Marty, B -- Mousis, O -- Neefs, E -- Owen, T -- Reme, H -- Rubin, M -- Semon, T -- Tornow, C -- Tzou, C-Y -- Waite, J H -- Wurz, P -- New York, N.Y. -- Science. 2015 Jan 23;347(6220):aaa0276. doi: 10.1126/science.aaa0276. Epub 2015 Jan 22.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA. myrtha.haessig@swri.org. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Center for Space and Habitability (CSH), University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. ; Department of Geosciences, Tel-Aviv University, Ramat-Aviv, Tel-Aviv, Israel. ; Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS), Institute Pierre Simon Laplace (IPSL), Centre national de recherche scientifique (CNRS), Universite Pierre et Marie Curie (UPMC), Universite de Versailles Saint-Quentin-en-Yvelines (UVSQ), BP 102, UPMC, 4 Place Jussieu, F-75252 Paris Cedex 05, France. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA. ; Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), UMR 7328 CNRS - Universite d'Orleans, France. ; Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA. ; Belgian Institute for Space Aeronomy (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium. Center for Plasma Astrophysics, KULeuven, Celestijnenlaan 200D, 3001 Heverlee, Belgium. ; Institute of Computer and Network Engineering (IDA), TU Braunschweig, Hans-Sommer-Strasse 66, D-38106 Braunschweig, Germany. ; Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA. ; Department of Physics, Imperial College London, Prince Consort Road, London SW7 2AZ, UK. ; Institute for Geophysics and Extraterrestrial Physics, Technische Universitat (TU) Braunschweig, 38106 Braunschweig, Germany. German Aerospace Center, Institute of Planetary Research, Asteroids and Comets, Rutherfordstrasse 2, 12489 Berlin, Germany. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; German Aerospace Center, Institute of Planetary Research, Asteroids and Comets, Rutherfordstrasse 2, 12489 Berlin, Germany. ; Center for Space and Habitability (CSH), University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. ; Centre de Recherches Petrographiques et Geochimiques (CRPG), 15 Rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre les Nancy, France. ; Aix Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 13388, Marseille, France. ; Engineering Division, BIRA-IASB, Ringlaan 3, B-1180 Brussels, Belgium. ; Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA. ; Universite de Toulouse, Universite Paul Sabathier (UPS), Observatoire de Midi-Pyrenees (OMP), Institut de Recherche en Astrophysique et Planetologie (IRAP), Toulouse, France. CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25613892" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
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    Cometary science. 67P/Churyumov-Gerasimenko, a Jupiter family comet with a high D/H ratio (2014)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2014-12-17
    Description: The provenance of water and organic compounds on Earth and other terrestrial planets has been discussed for a long time without reaching a consensus. One of the best means to distinguish between different scenarios is by determining the deuterium-to-hydrogen (D/H) ratios in the reservoirs for comets and Earth's oceans. Here, we report the direct in situ measurement of the D/H ratio in the Jupiter family comet 67P/Churyumov-Gerasimenko by the ROSINA mass spectrometer aboard the European Space Agency's Rosetta spacecraft, which is found to be (5.3 +/- 0.7) x 10(-4)-that is, approximately three times the terrestrial value. Previous cometary measurements and our new finding suggest a wide range of D/H ratios in the water within Jupiter family objects and preclude the idea that this reservoir is solely composed of Earth ocean-like water.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Altwegg, K -- Balsiger, H -- Bar-Nun, A -- Berthelier, J J -- Bieler, A -- Bochsler, P -- Briois, C -- Calmonte, U -- Combi, M -- De Keyser, J -- Eberhardt, P -- Fiethe, B -- Fuselier, S -- Gasc, S -- Gombosi, T I -- Hansen, K C -- Hassig, M -- Jackel, A -- Kopp, E -- Korth, A -- LeRoy, L -- Mall, U -- Marty, B -- Mousis, O -- Neefs, E -- Owen, T -- Reme, H -- Rubin, M -- Semon, T -- Tzou, C-Y -- Waite, H -- Wurz, P -- New York, N.Y. -- Science. 2015 Jan 23;347(6220):1261952. doi: 10.1126/science.1261952. Epub 2014 Dec 10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. altwegg@space.unibe.ch. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. ; Department of Geosciences, Tel-Aviv University, Ramat-Aviv, Tel-Aviv, Israel. ; Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS), 4 Avenue de Neptune, F-94100 Saint-Maur, France. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA. ; Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), UMR 6115 CNRS-Universite d'Orleans, France. ; Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA. ; Space Physics Division, Belgisch Instituut voor Ruimte-Aeronomie (BIRA)-Institut d'Aeronomie Spatiale de Belgique (IASB), Ringlaan 3, B-1180 Brussels, Belgium. ; Institute of Computer and Network Engineering (IDA), Technicsche Universitat Braunschweig, Hans-Sommer-Strasse 66, D-38106 Braunschweig, Germany. ; Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA. ; Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; Centre de Recherches Petrographiques et Geochimiques, Centre de Recherches Petrographiques et Geochimiques (CRPG)-CNRS, Universite de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre les Nancy, France. ; Universite de Franche-Comte, Institut Univers, Transport, Interfaces, Nanostructures, Atmosphere et Environnement, Molecules (UTINAM), CNRS/Institut National des Sciences de l'Univers (INSU), UMR 6213 Besancon Cedex, France. ; Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA. ; Universite de Toulouse, Universite Paul Sabatier (UPS)-Observatoire Midi-Pyrenees (OMP), Institut de Recherche en Astrophysique et Planetologie (IRAP), Toulouse, France. CNRS, IRAP, 9 Avenue du Colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25501976" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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