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Protons and hydrogen atoms transport in the Martian upper atmosphere with an induced magnetic field
Institute of Astronomy, Russian Academy of Sciences, Moscow.
Institute of Astronomy, Russian Academy of Sciences, Moscow.
Swedish Institute of Space Physics / Institutet för rymdfysik.
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2011 (English)In: Journal of Geophysical Research, ISSN 0148-0227, E-ISSN 2156-2202, Vol. 116, p. A11320-Article in journal (Refereed) Published
Abstract [en]

We have applied the Direct Simulation Monte Carlo method to solve the kinetic equation for the H/H+ transport in the upper Martian atmosphere. We calculate the upward H and H+ fluxes, values that can be measured, and the altitude profile of the energy deposition to be used to understand the energy balance in the Martian atmosphere. The calculations of the upward flux have been made for the Martian atmosphere during solar minimum. We use an energy spectrum of the down moving protons in the altitude range 355–437 km adopted from the Mars Express Analyzer of Space Plasma and Energetic Atoms measurements in the range 700 eV–20 keV. The particle and energy fluxes of the downward moving protons were equal to 3.0 × 106 cm−2 s−1 and 1.4 × 10−2 erg cm−2 s−1. It was found that 22% of particle flux and 12% of the energy flux of the precipitating protons is backscattered by the Martian upper atmosphere, if no induced magnetic field is taken into account in the simulations. If we include a 20 nT horizontal magnetic field, a typical field measured by Mars Global Surveyor in the altitude range of 85–500 km, we find that up to 40%–50% of the energy flux of the precipitating protons is backscattered depending on the velocity distribution of the precipitating protons. We thus conclude that the induced magnetic field plays a crucial role in the transport of charged particles in the upper atmosphere of Mars and, therefore, that it determines the energy deposition of the solar wind.

Place, publisher, year, edition, pages
2011. Vol. 116, p. A11320-
Identifiers
URN: urn:nbn:se:ltu:diva-4651DOI: 10.1029/2011JA017007Local ID: 2a09dce3-3f94-4c56-8034-7a43c634b95fOAI: oai:DiVA.org:ltu-4651DiVA: diva2:977525
Note
Upprättat; 2011; 20121127 (ysko)Available from: 2016-09-29 Created: 2016-09-29 Last updated: 2017-11-24Bibliographically approved

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