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  • 1
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    Correction to “Electrons and magnetic fields in the lunar plasma wake” (2011)
    Wiley
    Details
    Publication Date: 2011-07-29
    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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    Magnetic Field and Plasma Observations at Mars: Initial Results of the Mars Global Surveyor Mission (1998)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1998-03-13
    Description: The magnetometer and electron reflectometer investigation (MAG/ER) on the Mars Global Surveyor spacecraft has obtained magnetic field and plasma observations throughout the near-Mars environment, from beyond the influence of Mars to just above the surface (at an altitude of approximately 100 kilometers). The solar wind interaction with Mars is in many ways similar to that at Venus and at an active comet, that is, primarily an ionospheric-atmospheric interaction. No significant planetary magnetic field of global scale has been detected to date (〈2 x 10(21) Gauss-cubic centimeter), but here the discovery of multiple magnetic anomalies of small spatial scale in the crust of Mars is reported.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Acuna -- Connerney -- Wasilewski -- Lin -- Anderson -- Carlson -- McFadden -- Curtis -- Mitchell -- Reme -- Mazelle -- Sauvaud -- d'Uston -- Cros -- Medale -- Bauer -- Cloutier -- Mayhew -- Winterhalter -- Ness -- New York, N.Y. -- Science. 1998 Mar 13;279(5357):1676-80.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉M. H. Acuna, J. E. P. Connerney, P. Wasilewski, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. R. P. Lin, Space Sciences Laboratory and Department of Physics, University of California, Berkeley, CA 94720, USA. K. A. Anderson, C. W. Carlson, J. McFadden, D. W. Curtis, D. Mitchell, Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA. H. Reme, C. Mazelle, J. A. Sauvaud, C. d'Uston, A. Cros, J. L. Medale, Centre d'Etude Spatiale des Rayonnements, 31209 Toulouse Cedex, France. S. J. Bauer, University of Graz and Space Research Institute, A-8010 Graz, Austria. P. Cloutier, Department of Space Physics and Astronomy, Rice University, Houston, TX 77005, USA. M. Mayhew, National Science Foundation, Arlington, VA 22230, USA. D. Winterhalter, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. N. F. Ness, Bartol Research Institute, University of Delaware, Newark, DE 19716, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9497279" 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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  • 3
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    Global distribution of crustal magnetization discovered by the mars global surveyor MAG/ER experiment (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-04-30
    Description: Vector magnetic field observations of the martian crust were acquired by the Mars Global Surveyor (MGS) magnetic field experiment/electron reflectometer (MAG/ER) during the aerobraking and science phasing orbits, at altitudes between approximately 100 and 200 kilometers. Magnetic field sources of multiple scales, strength, and geometry were observed. There is a correlation between the location of the sources and the ancient cratered terrain of the martian highlands. The absence of crustal magnetism near large impact basins such as Hellas and Argyre implies cessation of internal dynamo action during the early Naochian epoch ( approximately 4 billion years ago). Sources with equivalent magnetic moments as large as 1.3 x 10(17) ampere-meter2 in the Terra Sirenum region contribute to the development of an asymmetrical, time-variable obstacle to solar wind flow around Mars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Acuna -- Connerney -- Ness -- Lin -- Mitchell -- Carlson -- McFadden -- Anderson -- Reme -- Mazelle -- Vignes -- Wasilewski -- Cloutier -- New York, N.Y. -- Science. 1999 Apr 30;284(5415):790-3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. Bartol Research Institute, University of Delaware, Newark, DE 19716, USA. Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA. Centre d'Etude Spatiale des Rayonn.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10221908" 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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  • 4
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    Magnetic lineations in the ancient crust of mars (1999)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1999-04-30
    Description: The Mars Global Surveyor spacecraft, in a highly elliptical polar orbit, obtained vector magnetic field measurements above the surface of Mars (altitudes 〉100 kilometers). Crustal magnetization, mainly confined to the most ancient, heavily cratered martian highlands, is frequently organized in east-west-trending linear features, the longest extending over 2000 kilometers. Crustal remanent magnetization exceeds that of terrestrial crust by more than an order of magnitude. Groups of quasi-parallel linear features of alternating magnetic polarity were found. They are reminiscent of similar magnetic features associated with sea floor spreading and crustal genesis on Earth but with a much larger spatial scale. They may be a relic of an era of plate tectonics on Mars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Connerney -- Acuna -- Wasilewski -- Ness -- Reme -- Mazelle -- Vignes -- Lin -- Mitchell -- Cloutier -- New York, N.Y. -- Science. 1999 Apr 30;284(5415):794-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. Bartol Research Institute, University of Delaware, Newark, DE 19716, USA. Centre d'Etude Spatiale des Rayonnements, 31028 Toulouse Cedex 4, France. Space Sciences Laboratory, University.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10221909" 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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  • 5
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    Lunar surface magnetic fields and their interaction with the solar wind: results from lunar prospector (1998)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1998-09-04
    Description: The magnetometer and electron reflectometer experiment on the Lunar Prospector spacecraft has obtained maps of lunar crustal magnetic fields and observed the interaction between the solar wind and regions of strong crustal magnetic fields at high selenographic latitude (30 degreesS to 80 degreesS) and low ( approximately 100 kilometers) altitude. Electron reflection maps of the regions antipodal to the Imbrium and Serenitatis impact basins, extending to 80 degreesS latitude, show that crustal magnetic fields fill most of the antipodal zones of those basins. This finding provides further evidence for the hypothesis that basin-forming impacts result in magnetization of the lunar crust at their antipodes. The crustal magnetic fields of the Imbrium antipode region are strong enough to deflect the solar wind and form a miniature (100 to several hundred kilometers across) magnetosphere, magnetosheath, and bow shock system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lin -- Mitchell -- Curtis -- Anderson -- Carlson -- McFadden -- Acuna -- Hood -- Binder -- New York, N.Y. -- Science. 1998 Sep 4;281(5382):1480-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉R. P. Lin, Space Sciences Laboratory and Physics Department, University of California, Berkeley, CA 94720, USA. D. L. Mitchell, D. W. Curtis, K. A. Anderson, C. W. Carlson, J. McFadden, Space Sciences Laboratory, University of California〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9727969" 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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  • 6
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    Domination of heliosheath pressure by shock-accelerated pickup ions from observations of neutral atoms (2008)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2008-07-04
    Description: The solar wind blows an immense magnetic bubble, the heliosphere, in the local interstellar medium (mostly neutral gas) flowing by the Sun. Recent measurements by Voyager 2 across the termination shock, where the solar wind is slowed to subsonic speeds before entering the heliosheath, found that the shocked solar wind plasma contains only approximately 20 per cent of the energy released by the termination shock, whereas energetic particles above approximately 28 keV contain only approximately 10 per cent; approximately 70 per cent of the energy is unaccounted for, leading to speculation that the unmeasured pickup ions or energetic particles below 28 keV contain the missing energy. Here we report the detection and mapping of heliosheath energetic ( approximately 4-20 keV) neutral atoms produced by charge exchange of suprathermal ions with interstellar neutral atoms. The energetic neutral atoms come from a source approximately 60 degrees wide in longitude straddling the direction of the local interstellar medium. Their energy spectra resemble those of solar wind pickup ions, but with a knee at approximately 11 keV instead of approximately 4 keV, indicating that their parent ions are pickup ions energized by the termination shock. These termination-shock-energized pickup ions contain the missing approximately 70 per cent of the energy dissipated in the termination shock, and they dominate the pressure in the heliosheath.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Wang, Linghua -- Lin, Robert P -- Larson, Davin E -- Luhmann, Janet G -- England -- Nature. 2008 Jul 3;454(7200):81-3. doi: 10.1038/nature07068.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Physics Department, University of California, Berkeley, California 94720-7300, USA. windsound@ssl.berkeley.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18596805" target="_blank"〉PubMed〈/a〉
    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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    A large excess in apparent solar oblateness due to surface magnetism (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-10-04
    Description: The shape of the Sun subtly reflects its rotation and internal flows. The surface rotation rate, approximately 2 kilometers per second at the equator, predicts an oblateness (equator-pole radius difference) of 7.8 milli-arc seconds, or approximately 0.001%. Observations from the Reuven Ramaty High-Energy Solar Spectroscopic Imager satellite show unexpectedly large flattening, relative to the expectation from surface rotation. This excess is dominated by the quadrupole term and gives a total oblateness of 10.77 +/- 0.44 milli-arc seconds. The position of the limb correlates with a sensitive extreme ultraviolet proxy, the 284 angstrom limb brightness. We relate the larger radius values to magnetic elements in the enhanced network and use the correlation to correct for it as a systematic error term in the oblateness measurement. The corrected oblateness of the nonmagnetic Sun is 8.01 +/- 0.14 milli-arc seconds, which is near the value expected from rotation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fivian, Martin D -- Hudson, Hugh S -- Lin, Robert P -- Zahid, H Jabran -- New York, N.Y. -- Science. 2008 Oct 24;322(5901):560-2. doi: 10.1126/science.1160863. Epub 2008 Oct 2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Sciences Laboratory, University of California-Berkeley, Berkeley, CA 94720, USA. mfivian@ssl.berkeley.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18832608" 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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  • 8
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    Terrestrial gamma-ray flashes observed up to 20 MeV (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-02-19
    Description: Terrestrial gamma-ray flashes (TGFs) from Earth's upper atmosphere have been detected with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) satellite. The gamma-ray spectra typically extend up to 10 to 20 megaelectron volts (MeV); a simple bremsstrahlung model suggests that most of the electrons that produce the gamma rays have energies on the order of 20 to 40 MeV. RHESSI detects 10 to 20 TGFs per month, corresponding to approximately 50 per day globally, perhaps many more if they are beamed. Both the frequency of occurrence and maximum photon energy are more than an order of magnitude higher than previously known for these events.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, David M -- Lopez, Liliana I -- Lin, R P -- Barrington-Leigh, Christopher P -- New York, N.Y. -- Science. 2005 Feb 18;307(5712):1085-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Physics Department and Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA. dsmith@scipp.ucsc.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15718466" 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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    The hot plasma environment at jupiter: ulysses results (1992)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1992-09-11
    Description: Measurements of the hot plasma environment during the Ulysses flyby of Jupiter have revealed several new discoveries related to this large rotating astrophysical system. The Jovian magnetosphere was found by Ulysses to be very extended, with the day-side magnetopause located at approximately 105 Jupiter radii. The heavy ion (sulfur, oxygen, and sodium) population in the day-side magnetosphere increased sharply at approximately 86 Jupiter radii. This is somewhat more extended than the "inner" magnetosphere boundary region identified by the Voyager hot plasma measurements. In the day-side magnetosphere, the ion fluxes have the anisotropy direction expected for corotation with the planet, with the magnitude of the anisotropy increasing when the spacecraft becomes more immersed in the hot plasma sheet. The relative abundances of sulfur, oxygen, and sodium to helium decreased somewhat with decreasing radial distance from the planet on the day-side, which suggests that the abundances of the Jupiter-derived species are dependent on latitude. In the dusk-side, high-latitude region, intense fluxes of counter-streaming ions and electrons were discovered from the edge of the plasma sheet to the dusk-side magnetopause. These beams of electrons and ions were found to be very tightly aligned with the magnetic field and to be superimposed on a time- and space-variable isotropic hot plasma background. The currents carried by the measured hot plasma particles are typically approximately 1.6 x 10(-4) microamperes per square meter or approximately 8 x 10(5) amperes per squared Jupiter radius throughout the high-latitude magnetosphere volume. It is likely that the intense particle beams discovered at high Jovian latitudes produce auroras in the polar caps of the planet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lanzerotti, L J -- Armstrong, T P -- Gold, R E -- Anderson, K A -- Krimigis, S M -- Lin, R P -- Pick, M -- Roelof, E C -- Sarris, E T -- Simnett, G M -- Maclennan, C G -- Choo, H T -- Tappin, S J -- New York, N.Y. -- Science. 1992 Sep 11;257(5076):1518-24.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17776161" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 10
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    Evidence for chain molecules enriched in carbon, hydrogen, and oxygen in comet halley (1987)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1987-08-07
    Description: In situ measurements of the composition and spatial distribution of heavy thermal positive ions in the coma of comet Halley were made with the heavy-ion analyzer RPA2-PICCA aboard the Giotto spacecraft. Above 50 atomic mass units an ordered series of mass peaks centered at 61, 75, 91, and 105 atomic mass units were observed. Each peak appears to be composed of three or more closely spaced masses. The abundances decrease and the dissociation rates increase smoothly with increasing mass. These observations suggest the presence of chain molecules that are enriched in carbon, oxygen, and hydrogen, such as polyoxymethylene (polymerized formaldehyde), in comet Halley.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mitchell, D L -- Lin, R P -- Anderson, K A -- Carlson, C W -- Curtis, D W -- Korth, A -- Reme, H -- Sauvaud, J A -- D'Uston, C -- Mendis, D A -- New York, N.Y. -- Science. 1987 Aug 7;237(4815):626-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17758562" 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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