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  • Mars  (2)
  • ddc:551.5  (1)
  • 1
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    The Mini Induced Magnetospheres at Mars (2023)
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    Publication Date: 2023-12-16
    Description: We report on observations made by the Mars Atmosphere and Volatile EvolutioN spacecraft at Mars, in the region of the ion plume. We observe that in some cases, when the number density of oxygen ions is comparable to the density of the solar wind protons interaction between both plasmas leads to formation in the magnetosheath of mini induced magnetospheres possessing all typical features of induced magnetospheres typically observed at Mars or Venus: a pileup of the magnetic field at the head of the ion cloud, magnetospheric cavity, partially void of solar wind protons, draping of the interplanetary magnetic field around the mini obstacle, formation of a magnetic tail with a current sheet, in which protons are accelerated by the magnetic field tensions. These new observations may shed a light on the mechanism of formation of induced magnetospheres.
    Description: Plain Language Summary: There is a class of the induced planetary magnetospheres when the absence of intrinsic magnetic field allows a direct interaction of solar wind with planetary atmospheres/ionospheres. We have shown the existence of mini‐induced magnetospheres at Mars. When the density of the extracted from the ionosphere oxygen ions becomes comparable with the proton density in solar wind mini‐induced magnetospheres with all typical features of the planetary induced magnetospheres arise.
    Description: Key Points: Oxygen ions extracted from the Martian ionosphere interact with shocked solar wind in the magnetosheath. When the ion densities of both plasmas become comparable the mini induced magnetospheres are built. These Magnetospheres possess all typical features of the classical induced magnetospheres.
    Description: NASA
    Description: DFG
    Description: https://pds-ppi.igpp.ucla.edu/mission/MAVEN/MAVEN/MAG
    Description: https://pds-ppi.igpp.ucla.edu/mission/MAVEN/MAVEN/STATIC
    Keywords: ddc:523 ; Mars ; solar wind ; induced magnetosphere ; ionosphere ; magnetic barrier ; magnetic tail
    Language: English
    Type: doc-type:article
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    CITATION GEO-LEO
  • 2
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    Bursty Ion Escape Fluxes at Mars (2021)
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    Publication Date: 2021-07-21
    Description: Based on the Mars Atmosphere and Volatile Evolution measurements we have observed cases when the fluxes of oxygen ions escaping the Martian ionosphere exceed their median values by more than a factor of 100. In the Martian tail very high fluxes of the more energetic (E 〉 30 eV) oxygen ions fill the plasma sheet which then becomes much broader than under conditions with median values of ion fluxes. We have analyzed the occurrence of such events in the upper ionosphere near the terminator plane, which is the main source region of ions in the plasma tail. The maximum values of fluxes of oxygen ions with E 〉 30 eV were observed mostly in the hemisphere where the motional electric field imposed by the solar wind is directed outward from the planet. Although high values of the solar wind dynamic pressure and (or) the motional electric field are favorable for the observation of the extreme values of ion fluxes with E 〉 30 eV, there must also be other factors which initiate these events. In particular, we found a close relation of the maximum ion fluxes with the values of the simultaneously measured fluxes of solar wind penetrating into the upper ionosphere. Direct interaction of both plasmas might be a critical factor for the strong growth of the oxygen ion escape. Very high fluxes of the low‐energy oxygen ions (E 〈 30 eV) are often related with ion “clouds” with anomalously large number density observed in the upper ionosphere.
    Description: Key Points: Fluxes of oxygen ions escaping the Martian ionosphere with values exceeding their median values by more than a factor of 100 are observed. Burst fluxes of the high‐energy oxygen ions are often related with high values of the simultaneously measured fluxes of the solar wind. High fluxes of the low‐energy oxygen ions are often related with over dense ion clouds observed in the top‐side ionosphere of Mars.
    Description: National Aeronautics and Space Administration http://dx.doi.org/10.13039/100000104
    Description: U.S. Department of Education http://dx.doi.org/10.13039/100000138
    Description: Russian Science Foundation http://dx.doi.org/10.13039/501100006769
    Keywords: 523 ; Mars ; ion escape ; MAVEN ; solar wind ; Martian tail ; solar irradiance
    Type: article
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    CITATION GEO-LEO
  • 3
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    Induced Magnetic Fields and Plasma Motions in the Inner Part of the Martian Magnetosphere (2021)
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    Publication Date: 2022-03-24
    Description: Analysis of Mars Atmosphere and Volatile Evolution (MAVEN)/Supra‐Thermal And Thermal Ion Composition observations in the Martian upper atmosphere, bounded at higher altitudes by the shocked solar wind, shows that the draping of interplanetary magnetic field penetrates down to low altitudes (∼200−250 km) and governs dynamics of the ionosphere. The upper ionospheric plasma is driven into motion flowing around Mars similar to the shocked solar wind in the adjacent magnetosheath. Such a fluid‐like motion is accompanied by ion acceleration caused by the bending of the magnetic field, leading to ion extraction and finally to ion pickup. Extraction of ions and their acceleration produces a recoil effect of the bulk ionosphere in the opposite direction. This provides a strong asymmetry in ion dynamics in two different hemispheres, accompanied by wrapping of the magnetic field lines around Mars and respective reconnection.
    Description: Plain Language Summary: Although the Martian magnetosphere is hybrid and contains components of the induced and intrinsic magnetosphere, is possible to display these components by using the specific coordinate systems. Here we study the properties of the induced magnetosphere using the data obtained by MAVEN spacecraft. The interplanetary magnetic field penetrates deep into the Martian ionosphere draping around Mars and drive to the motion dense ionospheric plasma. Draping features and the induced plasma motions occur different in two hemispheres determined by the direction of the motional electric field in the solar wind. Ion acceleration and extraction is accompanied by a recoil effect that leads to a shift and asymmetry of the ionosphere.
    Description: Key Points: Draping of the interplanetary magnetic field around Mars penetrates deep to the ionosphere enveloping the planet and driving the ionosphere to the bulk motion. Draping and motion of the ionospheric plasma is characterized by asymmetry by the direction of the motional electric field in solar wind. Ion acceleration and extraction from the ionosphere is accompanied by a shift of the bulk ionosphere in the opposite direction.
    Description: National Aeronautics and Space Administration http://dx.doi.org/10.13039/100000104
    Description: DFG http://dx.doi.org/10.13039/501100001659
    Description: Russian Science Foundation http://dx.doi.org/10.13039/501100006769
    Keywords: ddc:523 ; ddc:551.5
    Language: English
    Type: doc-type:article
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    CITATION GEO-LEO
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