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  • 1
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    Cross-scale coupling in the auroral acceleration region (2011)
    Wiley
    Details
    Publication Date: 2011-10-18
    Description: High resolution imaging within regions of auroral luminosity reveal complex, highly structured dynamic and often vortical forms which evolve on time scales of the order of several seconds and less. These features are inherently multi-scale in nature with different sizes moving and evolving at different rates. Recent analyses have shown how the scale dependency of these motions can provide new insights into the nature of energy transport across scales occurring in current sheets through the auroral acceleration region. However the processes driving this transport and thus facilitating particle acceleration and the formation of bright and dynamic aurora remain unknown. This is a basic issue not only for advancing understanding of auroral arc formation but moreover for understanding dissipation and particle acceleration in current sheets generally. In this Frontier article we show how dedicated space-borne auroral imagery combined with magnetically conjugate field and particle measurements can be used to advance understanding of this universal physical process. By coupling these measurements with numerical simulations we show how flow shear, magnetic reconnection and tearing may launch a cascade toward smaller scales and conspire to form, shape and structure auroral forms. The simulations show that these processes evolve toward a robust scaling of structured magnetic fields (Bx) with wavenumber (ky) perpendicular to the geomagnetic field where Bx2(ky)/Δky ∼ ky−7/3 as observed.
    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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  • 2
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    Ionospheric convection signatures of tail fast flows during substorms and Poleward Boundary Intensifications (PBI) (2011)
    Wiley
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    Publication Date: 2011-04-23
    Description: Tail fast flows have been associated both with the onset of substorms and with auroral Poleward Boundary Intensifications (PBIs) that extend equatorward as streamers. We study here a series of bursts of fast tail flow that occurred on 5 March 2008 when four of the THEMIS probes were aligned in the tail from mid-tail to inner magnetosphere and were in good conjunction with the Sondrestrom Incoherent Scatter Radar. The series of burst are identified as two separate events. We find that the first event is associated with a small substorm onset, and the second with a PBI and then possibly another onset. The ionospheric flow signatures of the substorm and the PBI are distinctly different: the substorm onset is characterized by flow enhancement in the polar cap several minutes before onset and by sudden ionospheric flow reduction at onset, while the PBI is accompanied by a flow enhancement directed primarily equatorward and intruding from the polar cap into the plasma sheet.
    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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  • 3
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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
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  • 4
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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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  • 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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    Tail reconnection triggering substorm onset (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-07-26
    Description: Magnetospheric substorms explosively release solar wind energy previously stored in Earth's magnetotail, encompassing the entire magnetosphere and producing spectacular auroral displays. It has been unclear whether a substorm is triggered by a disruption of the electrical current flowing across the near-Earth magnetotail, at approximately 10 R(E) (R(E): Earth radius, or 6374 kilometers), or by the process of magnetic reconnection typically seen farther out in the magnetotail, at approximately 20 to 30 R(E). We report on simultaneous measurements in the magnetotail at multiple distances, at the time of substorm onset. Reconnection was observed at 20 R(E), at least 1.5 minutes before auroral intensification, at least 2 minutes before substorm expansion, and about 3 minutes before near-Earth current disruption. These results demonstrate that substorms are likely initiated by tail reconnection.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Angelopoulos, Vassilis -- McFadden, James P -- Larson, Davin -- Carlson, Charles W -- Mende, Stephen B -- Frey, Harald -- Phan, Tai -- Sibeck, David G -- Glassmeier, Karl-Heinz -- Auster, Uli -- Donovan, Eric -- Mann, Ian R -- Rae, I Jonathan -- Russell, Christopher T -- Runov, Andrei -- Zhou, Xu-Zhi -- Kepko, Larry -- New York, N.Y. -- Science. 2008 Aug 15;321(5891):931-5. doi: 10.1126/science.1160495. Epub 2008 Jul 24.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Geophysics and Planetary Physics/ESS, University of California at Los Angeles, Los Angeles, CA 90095, USA. vassilis@ucla.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18653845" 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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  • 7
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    Substorm-like magnetospheric response to a discontinuity in the Bx component of interplanetary magnetic field (2012)
    Wiley
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    Publication Date: 2012-04-21
    Description: We examined the magnetospheric magnetic field and plasma responses to an encounter of a discontinuity in the Bx component of interplanetary magnetic field (IMF). The striking variations of simultaneous solar wind dynamic pressure and IMF-Bz were not observed. Furthermore, we found that this IMF-Bx discontinuity was a heliospheric current sheet, separating two high-speed solar wind streams with different velocity and magnetic polarity. In this study, the magnetic field and plasma data were obtained from Time History of Events and Macroscale Interactions during Substorms (THEMIS), Cluster, and GOES to investigate the magnetospheric responses, and those were taken from ACE and Geotail to monitor the solar wind conditions. Simultaneous geomagnetic field variations from the ground observatories and aurora activity from Polar were also examined. When the discontinuity encountered the magnetosphere, THEMIS-D, -E, and THEMIS-A observed abrupt and transient magnetic field and plasma variations in the dawnside near-Earth magnetotail and tail-flank magnetopause. Significant magnetic field perturbations were not observed by Cluster as located in the duskside magnetotail at this time interval. Although simultaneous dipolarization and negative bay variations with Pi2 waves were observed by GOES and the ground observatories, global auroral activities were not found. Around the dawnside tail-flank magnetopause, THEMIS-C and -A experienced the magnetopause crossings due to the magnetopause surface waves induced by Kelvin-Helmholtz instability. These results suggest that the magnetic field and plasma variations in the near-Earth magnetotail and tail-flank magnetopause were caused by moderate substorm-like phenomena and magnetopause surface waves. They also indicate that clear magnetospheric disturbances can be brought even without significant variations in the solar wind.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 8
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    FAST observations of solar illumination and solar cycle dependence of the acceleration of upflowing ion beams on auroral field lines (2013)
    Wiley
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    Publication Date: 2013-05-02
    Description: [1]  We present the magnetic local time, invariant latitude and altitude distribution of upflowing ion beams and the dependence of their occurrence on whether the ionospheric footpoint of the satellite is illuminated or dark and on solar cycle, as indicated by F10.7. The effects of illumination and solar cycle are additive, consistent with the fact that the solar EUV depends on solar cycle and that the ionospheric conditions are dependent on total flux illuminating the footpoint. Consistent with previous studies, the occurrence of upflowing ion beams peaks in the pre-midnight local time sector and the occurrence increases dramatically with altitude over the altitude range of FAST (~700 km to ~4000 km). Solar illumination both reduces the occurrence of ion beams observed by more than a factor of 10 and increases the altitude where the acceleration occurs so that beams are rare below ~4000 km altitude. The effect of the increased solar EUV near solar maximum is almost as large. The inferred potential drops at altitudes below 4000 km, even during dark conditions, are usually less than 1 keV; during sunlit conditions and/or high F10.7, the potentials are usually less than 500 eV. These results place constraints on the altitude of the auroral parallel potential drop and on the relative importance of ionospheric conductivity and plasma density on the acceleration processes. There is no evidence that the statistical results are due to motion of large parallel potential drops to lower latitudes near solar maximum.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 9
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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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  • 10
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    General features of the Comet Halley-solar wind interaction from plasma measurements (1986)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: The Giotto Complete Positive ion, Electron and Ram Negative Ion measurements near Comet Halley plasma experiment identified regions in which the solar wind interaction with the cometary plasma displayed characteristic features. Beginning 4.6 million km from the comet there is an upstream region with sporadic connection to the comet. An electron foreshock is present up to 250,000 km away from the bow shock. A bow shock is detected at 1.15 million km. Between the bow shock and the cometopause the outer regions can be divided into three parts. A cometopause is found at 135,000 km, and a density decrease is detected at 45,000 km from the comet. The detailed plasma features associated with these regions are described.
    Keywords: ASTROPHYSICS
    Type: ESA Proceedings of the 20th ESLAB Symposium on the Exploration of Halley's Comet. Volume 1: Plasma and Gas; p 29-34
    Format: text
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