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  • Mars  (2)
  • 1
    Publikationsdatum: 2023-12-16
    Beschreibung: 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.
    Beschreibung: 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.
    Beschreibung: 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.
    Beschreibung: NASA
    Beschreibung: DFG
    Beschreibung: https://pds-ppi.igpp.ucla.edu/mission/MAVEN/MAVEN/MAG
    Beschreibung: https://pds-ppi.igpp.ucla.edu/mission/MAVEN/MAVEN/STATIC
    Schlagwort(e): ddc:523 ; Mars ; solar wind ; induced magnetosphere ; ionosphere ; magnetic barrier ; magnetic tail
    Sprache: Englisch
    Materialart: doc-type:article
    Standort Signatur Erwartet Verfügbarkeit
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  • 2
    Publikationsdatum: 2021-07-21
    Beschreibung: 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.
    Beschreibung: 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.
    Beschreibung: National Aeronautics and Space Administration http://dx.doi.org/10.13039/100000104
    Beschreibung: U.S. Department of Education http://dx.doi.org/10.13039/100000138
    Beschreibung: Russian Science Foundation http://dx.doi.org/10.13039/501100006769
    Schlagwort(e): 523 ; Mars ; ion escape ; MAVEN ; solar wind ; Martian tail ; solar irradiance
    Materialart: article
    Standort Signatur Erwartet Verfügbarkeit
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