Solar Wind Asymmetries around magnetic anomalies at the Moon and Mars.

Details Solar Wind Asymmetries around magnetic anomalies at the Moon and Mars. Solar Wind Asymmetries around magnetic anomalies at the Moon and Mars.

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsm21a0528h&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SM21A-0528

Physics

2753 Numerical Modeling, 2756 Planetary Magnetospheres (5443, 5737, 6030), 5440 Magnetic Fields And Magnetism, 6225 Mars, 6250 Moon (1221)

Scientific paper

Magnetic anomalies have been found on both the Moon and Mars, but unlike the Moon, the Martian atmosphere is thick enough to hold off the solar wind through thermal pressure, creating a bow shock. 3D fluid simulations show that magnetic anomalies are important in determining how the solar wind interacts with the Moon and Mars. When no substantial atmosphere is present, as in the case of the Moon, the magnetic anomalies can lead to the formation of a localized shock surface that produces asymmetric solar wind flow over the Moon. These asymmetries can be seen well tail of the Moon. In the case of Mars, where there is a thick atmosphere and distinct ionopause, the magnetic anomalies are still able to modify the solar wind flow and the interaction produces an increase in the scale height of the atmosphere opposite the anomalies and creates a magnetopause within the pre-existing bow shock. The importance of the higher order moments of the anomalous field is reduced in the case of Mars, as the interaction region is further from the source. Disturbances in the solar wind flow deep down the tail, and can be modulated by changes in the interplanetary magnetic field.

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