Mercury's solar wind interaction during the evolution of the solar radiation and particle environment

Details Mercury's solar wind interaction during the evolution of the solar radiation and particle environment Mercury's solar wind interaction during the evolution of the solar radiation and particle environment

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....12745l&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #12745

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Scientific paper

Astrophysical observations suggest that the young main-sequence Sun rotated about 10 times faster than today and had correspondingly stronger magnetic activity, which triggered higher radiation and particle emission. Quantitative estimates of the solar high-energy flux evolution are only indirectly possible by comparison with solar proxies. Multiwavelength observations in the 0.1 nm to 330 nm spectral region have been collected for a sample of solar proxies, containing stars which represent most of the Sun's main sequence lifetime from 130 Myr to 8.5 Gyr. They show an excellent correlation between the emitted flux and the stellar age. We use a power law relation between rotation periods, X-ray fluxes and solar mass loss for the estimation of the solar wind mass flux evolution during the past 4.5 Gyr ago. Mercury's present exosphere indicate a strong radiation-particle-surface interaction related to the solar particle and radiation environment. Since Mercury is the closest planet to the Sun, its surface was most exposed to enhanced particle- and radiation fluxes than those of any of the other Solar System bodies. To evaluate how such effects may have influenced Mercury's surface, we study the solar wind-magnetospheric interaction with emphasis of the influence of the interplanetary magnetic field particle surface sputtering and photon stimulated desorption processes during the planets history by using the observational data from the Sun in Time programme.

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