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  • 1
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    Expansion and Shrinking of the Martian Topside Ionosphere (2019)
    Wiley
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    Publication Date: 2019
    Description: Abstract The observations made by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft in the topside (≥ 200 km) ionosphere of Mars show that this region is very responsive to the variations of the external (solar EUV flux, solar wind, IMF) and internal (the crustal magnetic field) drivers. With the growth of the solar irradiance the ionosphere broadens while with increase of the solar wind dynamic pressure it shrinks. As a result, the upper ionospheric boundary at solar zenith angles of 60° – 70° can move from ~ 400 to ~ 1200 km. Similar trends are observed at the nightside ionosphere. At Pdyn ≥ 1 – 2 nPa the nightside ionosphere becomes very fragmented and depleted. On the other hand, the ion density in the nightside ionosphere significantly (up to a factor of 10) increases with the rise of the solar EUV flux. Large‐amlplitude motions of the topside ionosphere also occur with variations of the value of the cross‐flow component of the interplanetary magnetic field (IMF). The upper dayside ionosphere at altitudes of more than 300‐400 km is sensitive also to the direction of the cross‐flow component of the IMF or, correspondingly, to the direction of the motional electric field in the solar wind. The ionosphere becomes very asymmetrical with respect to the Vsw × BIMF direction and the asymmetry strongly enhances at the nightside. The topside ionosphere above the areas with strong crustal magnetic field in the dayside southern hemisphere is significantly denser and expands to higher altitudes as compared to the ionosphere above the northern nonmagnetized lowlands. The crustal magnetic field also protects the nightside ionosphere from being filled by plasma transported from the dayside. The draping IMF penetrates deeply into the ionosphere and actively influences its structure. Weak fields and, correspondingly, weak magnetic field forces only slightly affect the ionosphere. With increase of the induced magnetic field strength the transport motions driven by the magnetic field pressure and field tensions seem to be intensified and we observe that the local ion densities at the dayside considerably decrease. A different trend is observed at the nightside. The ion density in the nightside ionosphere above the northern lowlands is higher than in the southern hemisphere indicating that plasma transport from the dayside is the main source of the nightside ionosphere. Non‐stop variations in the solar wind, the IMF and the solar irradiance together with planetary rotation of the crustal magnetic field sources lead to a continuous expansion/shrinking and reconfiguration of the topside ionosphere of Mars.
    Print ISSN: 2169-9380
    Electronic ISSN: 2169-9402
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    The Induced Magnetosphere of Mars: Asymmetrical Topology of the Magnetic Field Lines (2019)
    Wiley
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    Publication Date: 2019
    Description: Abstract An asymmetrical pileup of the interplanetary magnetic field leads to an additional draping of the field lines in the opposite direction to the motional electric field. Such a draping and the associated magnetic field forces push the ionosphere plasma in the transverse direction opening a passage for an ion trail which contains dense and slowly moving plasma. We found that wrapping of the field lines around Mars starts in the hemisphere pointing in the direction of the motional electric field and propagates to the opposite hemisphere where the cross‐flow component of the draped interplanetary magnetic field changes sign in a broad area accompanied by the formation of loops of closed field lines. Reconnection near Mars accompanied by the generation of plasma vortices imposes serious constraints on the ion dynamics and their escape through the tail. The existence of all these features is confirmed by hybrid simulations.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
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  • 3
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    Bursty escape fluxes in plasma sheets of Mars and Venus (2012)
    Wiley
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    Publication Date: 2012-01-11
    Description: High resolution measurements of plasma in the plasma sheets of Mars and Venus performed by almost identical plasma instruments ASPERA-3 on the Mars Express spacecraft and ASPERA-4 on Venus Express reveal similar features of bursty fluxes of escaping planetary ions. A period of bursts lasts about 1–2 min. Simultaneous magnetic field measurements on Venus Express show that these burst-like features arise due to flapping motions of the plasma sheet. Their occurrence can be related to large-amplitude waves propagating on the plasma sheet surface and launched by reconnection in the magnetic tails.
    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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    Magnetic fields in the Mars ionosphere of a non crustal origin. Magnetization features. (2014)
    Wiley
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    Publication Date: 2014-09-10
    Description: The magnetic field observations by the Mars Global Surveyor (MGS) performed on the premapping orbits in the years 1997–1998 in the low-altitude ionosphere of Mars show the existence of a strong ’external’ magnetization not related to the ’internal’ crustal magnetization. A significant increase of the magnetic field strength is observed in the collisional northern ionosphere, at altitudes of ~200 km and at 60°–90° solar zenith angles sampled by MGS. The magnetization features and the magnetic field topology vary significantly with the sector structure of the interplanetary magnetic field (IMF). For B yIMF  〉  0 the magnetic flux tubes transported to altitudes of ~200 km are suddenly straightened releasing their tangential stresses. For B yIMF  〈  0 a rotation of the magnetic field vector by almost 180° occurs. Such an asymmetry in the ionospheric response on Mars is similar to the asymmetry observed on Venus at the periods of low solar activity indicating its universal origin for magnetized ionospheres. It is suggested that the electric currents generated in the collisional ionosphere where the ions become demagnetized while the electrons remain magnetized produce the observed features.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
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  • 5
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    Enhanced atmospheric oxygen outflow on Earth and Mars driven by a corotating interaction region (2012)
    Wiley
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    Publication Date: 2012-03-09
    Description: Solar wind controls nonthermal escape of planetary atmospheric volatiles, regardless of the strength of planetary magnetic fields. For both Earth with a strong dipole and Mars with weak remnant fields, the oxygen ion (O+) outflow has been separately found to be enhanced during corotating interaction region (CIR) passage. Here we compared the enhancements of O+ outflow on Earth and Mars driven by a CIR in January 2008, when Sun, Earth, and Mars were approximately aligned. The CIR propagation was recorded by STEREO, ACE, Cluster, and Mars Express (MEX). During the CIR passage, Cluster observed enhanced flux of upwelling oxygen ions above the Earth's polar region, while MEX detected an increased escape flux of oxygen ions in the Martian magnetosphere. We found that (1) under a solar wind dynamic pressure increase of 2–3 nPa, the rate of increase in Martian O+ outflow flux was 1 order higher than those on Earth; and (2) as a response to the same part of the CIR body, the rate of increase in Martian O+ outflow flux was on the same order as for Earth. The comparison results imply that the dipole effectively prevents coupling of solar wind kinetic energy to planetary ions, and the distance to the Sun is also crucially important for planetary volatile loss in our inner solar system.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 6
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    An Overview of Energetic Particle Measurements in the Jovian Magnetosphere with the EPAC Sensor on Ulysses (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-09-11
    Description: Observations of ions and electrons of probable Jovian origin upstream of Jupiter were observed after a corotating interplanetary particle event. During the passage of Ulysses through the Jovian bow shock, magnetopause, and outer magnetosphere, the fluxes of energetic particles were surprisingly low. During the passage through the "middle magnetosphere," corotating fluxes were observed within the current sheet near the jovimagnetic equato. During the outbound pass, fluxes were variably directed; in the later part of the flyby, they were probably related to high-latitude phenomena.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Keppler, E -- Blake, J B -- Franz, M -- Korth, A -- Krupp, N -- Quenby, J J -- Witte, M -- Woch, J -- New York, N.Y. -- Science. 1992 Sep 11;257(5076):1553-7.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17776167" 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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    The dust halo of Saturn's largest icy moon, Rhea (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-03-08
    Description: Saturn's moon Rhea had been considered massive enough to retain a thin, externally generated atmosphere capable of locally affecting Saturn's magnetosphere. The Cassini spacecraft's in situ observations reveal that energetic electrons are depleted in the moon's vicinity. The absence of a substantial exosphere implies that Rhea's magnetospheric interaction region, rather than being exclusively induced by sputtered gas and its products, likely contains solid material that can absorb magnetospheric particles. Combined observations from several instruments suggest that this material is in the form of grains and boulders up to several decimetres in size and orbits Rhea as an equatorial debris disk. Within this disk may reside denser, discrete rings or arcs of material.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jones, G H -- Roussos, E -- Krupp, N -- Beckmann, U -- Coates, A J -- Crary, F -- Dandouras, I -- Dikarev, V -- Dougherty, M K -- Garnier, P -- Hansen, C J -- Hendrix, A R -- Hospodarsky, G B -- Johnson, R E -- Kempf, S -- Khurana, K K -- Krimigis, S M -- Kruger, H -- Kurth, W S -- Lagg, A -- McAndrews, H J -- Mitchell, D G -- Paranicas, C -- Postberg, F -- Russell, C T -- Saur, J -- Seiss, M -- Spahn, F -- Srama, R -- Strobel, D F -- Tokar, R -- Wahlund, J-E -- Wilson, R J -- Woch, J -- Young, D -- New York, N.Y. -- Science. 2008 Mar 7;319(5868):1380-4. doi: 10.1126/science.1151524.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany. ghj@mssl.ucl.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18323452" 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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    Solar wind-induced atmospheric erosion at Mars: first results from ASPERA-3 on Mars Express (2004)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2004-09-28
    Description: The Analyzer of Space Plasma and Energetic Atoms (ASPERA) on board the Mars Express spacecraft found that solar wind plasma and accelerated ionospheric ions may be observed all the way down to the Mars Express pericenter of 270 kilometers above the dayside planetary surface. This is very deep in the ionosphere, implying direct exposure of the martian topside atmosphere to solar wind plasma forcing. The low-altitude penetration of solar wind plasma and the energization of ionospheric plasma may be due to solar wind irregularities or perturbations, to magnetic anomalies at Mars, or both.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lundin, R -- Barabash, S -- Andersson, H -- Holmstrom, M -- Grigoriev, A -- Yamauchi, M -- Sauvaud, J-A -- Fedorov, A -- Budnik, E -- Thocaven, J-J -- Winningham, D -- Frahm, R -- Scherrer, J -- Sharber, J -- Asamura, K -- Hayakawa, H -- Coates, A -- Linder, D R -- Curtis, C -- Hsieh, K C -- Sandel, B R -- Grande, M -- Carter, M -- Reading, D H -- Koskinen, H -- Kallio, E -- Riihela, P -- Schmidt, W -- Sales, T -- Kozyra, J -- Krupp, N -- Woch, J -- Luhmann, J -- McKenna-Lawler, S -- Cerulli-Irelli, R -- Orsini, S -- Maggi, M -- Mura, A -- Milillo, A -- Roelof, E -- Williams, D -- Livi, S -- Brandt, P -- Wurz, P -- Bochsler, P -- New York, N.Y. -- Science. 2004 Sep 24;305(5692):1933-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Swedish Institute of Space Physics, Box 812, S-98 128, Kiruna, Sweden. rickard.lundin@irf.se〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15448263" 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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    Dynamics of Saturn's magnetosphere from MIMI during Cassini's orbital insertion (2005)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2005-02-26
    Description: The Magnetospheric Imaging Instrument (MIMI) onboard the Cassini spacecraft observed the saturnian magnetosphere from January 2004 until Saturn orbit insertion (SOI) on 1 July 2004. The MIMI sensors observed frequent energetic particle activity in interplanetary space for several months before SOI. When the imaging sensor was switched to its energetic neutral atom (ENA) operating mode on 20 February 2004, at approximately 10(3) times Saturn's radius RS (0.43 astronomical units), a weak but persistent signal was observed from the magnetosphere. About 10 days before SOI, the magnetosphere exhibited a day-night asymmetry that varied with an approximately 11-hour periodicity. Once Cassini entered the magnetosphere, in situ measurements showed high concentrations of H+, H2+, O+, OH+, and H2O+ and low concentrations of N+. The radial dependence of ion intensity profiles implies neutral gas densities sufficient to produce high loss rates of trapped ions from the middle and inner magnetosphere. ENA imaging has revealed a radiation belt that resides inward of the D ring and is probably the result of double charge exchange between the main radiation belt and the upper layers of Saturn's exosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krimigis, S M -- Mitchell, D G -- Hamilton, D C -- Krupp, N -- Livi, S -- Roelof, E C -- Dandouras, J -- Armstrong, T P -- Mauk, B H -- Paranicas, C -- Brandt, P C -- Bolton, S -- Cheng, A F -- Choo, T -- Gloeckler, G -- Hayes, J -- Hsieh, K C -- Ip, W-H -- Jaskulek, S -- Keath, E P -- Kirsch, E -- Kusterer, M -- Lagg, A -- Lanzerotti, L J -- Lavallee, D -- Manweiler, J -- McEntire, R W -- Rasmuss, W -- Saur, J -- Turner, F S -- Williams, D J -- Woch, J -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1270-3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. tom.krimigis@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731445" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; *Gases ; Hydrogen ; *Ions ; *Magnetics ; Nitrogen ; Oxygen ; *Saturn ; Spacecraft ; Spectrum Analysis ; *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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  • 10
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    Enceladus' varying imprint on the magnetosphere of Saturn (2006)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2006-03-11
    Description: The bombardment of Saturn's moon Enceladus by 〉20-kiloelectron volt magnetospheric particles causes particle flux depletions in regions magnetically connected to its orbit. Irrespective of magnetospheric activity, proton depletions are persistent, whereas electron depletions are quickly erased by magnetospheric processes. Observations of these signatures by Cassini's Magnetospheric Imaging Instrument allow remote monitoring of Enceladus' gas and dust environments. This reveals substantial outgassing variability at the moon and suggests increased dust concentrations at its Lagrange points. The characteristics of the particle depletions additionally provide key radial diffusion coefficients for energetic electrons and an independent measure of the inner magnetosphere's rotation velocity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jones, G H -- Roussos, E -- Krupp, N -- Paranicas, C -- Woch, J -- Lagg, A -- Mitchell, D G -- Krimigis, S M -- Dougherty, M K -- New York, N.Y. -- Science. 2006 Mar 10;311(5766):1412-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max Planck Institut fur Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. jones@mps.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16527968" target="_blank"〉PubMed〈/a〉
    Keywords: *Atmosphere ; Electrons ; *Extraterrestrial Environment ; Magnetics ; *Saturn
    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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