Evolution of the Solar Magnetic Activity over Time and Effects on Planetary Atmospheres

Details Evolution of the Solar Magnetic Activity over Time and Effects on Planetary Atmospheres Evolution of the Solar Magnetic Activity over Time and Effects on Planetary Atmospheres

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..219..423g&link_type=abstract

Stars as suns : activity, evolution and planets, Proceedings of the 219th symposium of the International Astronomical Union held

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We report on the results of a multi-wavelength study of solar analogs with ages of ~100 Myr to 9 Gyr. The data for this program cover wavelengths from the X-ray to the Near-IR. The chief science goals are (1) to study the solar magnetic dynamo (with rotation as the only variable) and (2)to determine the radiative and magnetic properties of the young Sun with the purpose of constructing spectral irradiance tables to be used to study and model paleo-planetary atmospheres. This study indicates that the young Sun was extremely active with large flares strong winds and high energy X-ray emissions up to 10000 times stronger than the present Sun. The strong radiation and particle emissions inferred for the young Sun are expected to have major influences on the photochemistry and photo-ionization of paleo planetary atmospheres and can also play an important role in the development of primitive life in the solar system and elsewhere. Some recent results of the effects of the young active Sun's enhanced high energy coronal emissions on the early solar system planets and planets around other solar-like stars will be discussed.

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