Interactions Between the Early Martian Dynamo, Surface Water, Atmosphere and Solar Wind

Details Interactions Between the Early Martian Dynamo, Surface Water, Atmosphere and Solar Wind Interactions Between the Early Martian Dynamo, Surface Water, Atmosphere and Solar Wind

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p52a..12l&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #P52A-12

Mathematics

Logic

[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [5405] Planetary Sciences: Solid Surface Planets / Atmospheres, [5729] Planetary Sciences: Fluid Planets / Ionospheres, [6225] Planetary Sciences: Solar System Objects / Mars

Scientific paper

The existence of mid/late Noachian valley networks and extensive erosion in the late Noachian require at least intermittent periods during which martian climatic conditions were more clement than at present. However, the presence of a core dynamo field during the end of heavy bombardment is difficult to reconcile with the lack of observable remanent magnetic anomalies over large impact basins such as Hellas and Argyre. This apparent delay between the cessation of a global magnetic field and the time period showing evidence for surface water, motivates further study of early Mars’ atmospheric loss rates. Using global hybrid particle simulations of the solar wind interaction with an early Martian atmosphere, we investigate rates of atmospheric loss of a hypothesized CO2-dominant atmosphere under standard pressure and temperature conditions. We consider 1, 6, and 10 times nominal EUV conditions, intended to simulate solar wind conditions at present, 3.5, and 3.8 Ga, respectively. We compare the integrated loss rates to temporal uncertainties in the Martian hydrologic history to determine if atmospheric loss rates require a coeval Martian dynamo to maintain conditions amenable to surface water during the late Noachian.

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