Other
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1135..244g&link_type=abstract
FUTURE DIRECTIONS IN ULTRAVIOLET SPECTROSCOPY: A Conference Inspired by the Accomplishments of the Far Ultraviolet Spectroscopic
Other
3
Binary And Multiple Stars, Photometric, Polarimetric, And Spectroscopic Instrumentation, Chromosphere
Scientific paper
Multi-wavelength studies of solar analogs (G0-G5 V stars) with ages from ~50 Myr to 9 Gyr have been carried out as part of our ongoing Sun in Time program. These studies indicate that the young Sun was rotating over 10× faster than today. As a consequence, it is inferred that young solar-type stars and the young Sun have vigorous magnetic dynamos and correspondingly strong coronal X-ray and transition region/chromospheric FUV-UV (XUV) emissions up to several hundred times stronger than the present Sun. However, the Sun and the solar-type stars spin-down with time as they lose angular momentum via magnetized winds and their magnetic generated activity and emissions significantly decrease. The primary science goals of the program are: to study the solar magnetic dynamo (with rotation as the only variable) and to determine the radiative and magnetic properties of the young Sun (and other solar-type stars). The determination of the XUV spectral irradiances of the young Sun (and stars) can be used to study paleo-planetary atmospheres. The strong XUV radiation and strong particle fluxes (winds) inferred for the young Sun have major implications and impacts on the photochemistry and photo-ionization of paleo-planetary atmospheres. Recent studies of the effects of the active young Sun's enhanced XUV emissions and wind fluxes on the early Earth (as well as on Venus and Mars) are briefly discussed along with the importance of planetary magnetic fields in protecting the young planets' atmospheres from the erosive effects of the young Sun's high levels of magnetic activity. Even though FUSE covers a relatively narrow spectral window in the XUV, the FUV emission lines within this window (such as the H I Lyman series) are significant contributors to the total XUV fluxes of young solar-type stars; also strong emission lines such as O VI 1032 & 1038 Å and C III 976 & 1175 Å provide important diagnostics to study the physical properties of stellar chromospheres and transition regions.
DeWarf Laurence E.
Engle Scott G.
Guinan Edward F.
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