X-ray emission from non-magnetic planets: Comparison with Chandra observations

Details X-ray emission from non-magnetic planets: Comparison with Chandra observations X-ray emission from non-magnetic planets: Comparison with Chandra observations

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dppqm2005s&link_type=abstract

American Physical Society, 44th Annual Meeting of the Division of Plasma , abstract #QM2.005

Physics

Scientific paper

On Mars and Venus, there is no obstacle to the solar wind and the supersonic flow comes in direct contact with the planetary ionospheres. On both planets, ther is a sufficiently broad and turbulent dayside layer located at the ionospheric boundary: the plasma mantle. The presence of a hot electron component with energies exceeding 100 eV is typical for the mantle layer. Eenergization in the mantle can be initiated by wave-particle interactions driven by counter streaming plasma populations in the mantle. The goal of this paper is to calculate the X-ray spectrum produced by the energetic electrons. We will do this in two steps. First, we will simulate the dynamics of a beam driven instability using an explicit one-dimensional Darwin particle-in-cell (PIC) code. An output from these simulations will be the accelerated electron spectrum. At Mars and Venus, the energetic electrons will interact (collide) with the neutral gas outflowing from the planets, producing a spectrum of X-rays. We will calculate the spectrum using the ADAS (Atomic Data and Analysis Structure) code. The resulting x-ray spectrum calculations will be compared to the recent observations of Venus by the Chandra X-ray observatory.

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