Oxygen ion escape at Mars in a hybrid model: High energy and low energy ions

Details Oxygen ion escape at Mars in a hybrid model: High energy and low energy ions Oxygen ion escape at Mars in a hybrid model: High energy and low energy ions

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010icar..206..152k&link_type=abstract

Icarus, Volume 206, Issue 1, p. 152-163.

Computer Science

8

Scientific paper

We have studied the escape and energization of several O+ populations and an O2+ population at Mars by using a hybrid model. The quasi-neutral hybrid model, HYB-Mars model, included five oxygen ion populations making it possible to distinguish photoions from oxygen ions originating from charge exchange processes and from the ionosphere. We have identified two high-energy ion components and one low-energy ion component of oxygen. They have different spatial and energy distributions near Mars. The two high-energy oxygen ion components, consisting of a high-energy “beam” and a high-energy “halo”, have different origins. (1) The high-energy (>˜100 eV) “beam” of O+ and O2+ ions are originating from the ionosphere. These ions form a highly asymmetric spatial distribution of escaping oxygen ions with respect to the direction of the convective electric field in the solar wind. (2) The high-energy (>˜100 eV) “halo” component contains O+ ions which are formed from the oxygen neutral exosphere by extreme ultraviolet radiation (EUV) and by charge exchange processes. These energetic halo ions can be found all around Mars. (3) The low energy O+ and O2+ ions (<˜100 eV) form a relatively symmetric spatial distribution around the Mars-Sun line. They originate from the ionosphere and from charge exchange processes between protons and exospheric oxygen atoms. The existence of the low- and the high-energy oxygen components is in agreement with recent in situ plasma measurements made by the ASPERA-3 instrument on the Mars Express mission. The analysis of the escaping oxygen ions suggests that the global energization of escaping planetary ions in the martian tail is controlled by the convective electric field.

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