The Mars crustal magnetic field control of plasma boundary locations and atmospheric loss: MHD prediction and comparison with MAVEN

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  • Xiaohua Fang
    Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
  • Yingjuan Ma
    Department of Earth, Planetary and Space Sciences University of California Los Angeles California USA
  • Kei Masunaga
    Department of Earth and Planetary Science University of Tokyo Tokyo Japan
  • Yaxue Dong
    Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
  • David Brain
    Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
  • Jasper Halekas
    Department of Physics and Astronomy University of Iowa Iowa City Iowa USA
  • Robert Lillis
    Space Sciences Laboratory University of California Berkeley California USA
  • Bruce Jakosky
    Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder Colorado USA
  • Jack Connerney
    NASA Goddard Space Flight Center Greenbelt Maryland USA
  • Joseph Grebowsky
    NASA Goddard Space Flight Center Greenbelt Maryland USA
  • Chuanfei Dong
    Department of Astrophysical Sciences and Princeton Plasma Physics Laboratory Princeton University Princeton New Jersey USA

書誌事項

公開日
2017-04
権利情報
  • http://onlinelibrary.wiley.com/termsAndConditions#vor
DOI
  • 10.1002/2016ja023509
公開者
American Geophysical Union (AGU)

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説明

<jats:title>Abstract</jats:title><jats:p>We present results from a global Mars time‐dependent MHD simulation under constant solar wind and solar radiation impact considering inherent magnetic field variations due to continuous planetary rotation. We calculate the 3‐D shapes and locations of the bow shock (BS) and the induced magnetospheric boundary (IMB) and then examine their dynamic changes with time. We develop a physics‐based, empirical algorithm to effectively summarize the multidimensional crustal field distribution. It is found that by organizing the model results using this new approach, the Mars crustal field shows a clear, significant influence on both the IMB and the BS. Specifically, quantitative relationships have been established between the field distribution and the mean boundary distances and the cross‐section areas in the terminator plane for both of the boundaries. The model‐predicted relationships are further verified by the observations from the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. Our analysis shows that the boundaries are collectively affected by the global crustal field distribution, which, however, cannot be simply parameterized by a local parameter like the widely used subsolar longitude. Our calculations show that the variability of the intrinsic crustal field distribution in Mars‐centered Solar Orbital itself may account for ∼60% of the variation in total atmospheric loss, when external drivers are static. It is found that the crustal field has not only a shielding effect for atmospheric loss but also an escape‐fostering effect by positively affecting the transterminator ion flow cross‐section area.</jats:p>

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