The Application of Solar Physics to Mass Loss and Angular Momentum Evolution of Solar-type Pre-Main Sequence Stars

Details The Application of Solar Physics to Mass Loss and Angular Momentum Evolution of Solar-type Pre-Main Sequence Stars The Application of Solar Physics to Mass Loss and Angular Momentum Evolution of Solar-type Pre-Main Sequence Stars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21538201a&link_type=abstract

American Astronomical Society, AAS Meeting #215, #382.01; Bulletin of the American Astronomical Society, Vol. 42, p.592

Physics

Scientific paper

Decades of high cadence, high spatial resolution, multi-wavelength solar observations have shown complex magnetically active regions and associated energetic phenomena such as flares and coronal mass ejections (CMEs). Understanding the physics underlying these phenomena is important for understanding the magnetic nature of the Sun generally, the physics of mass loss specifically, as well as the far-reaching effects of space weather on the denizens of 1 AU. However, for solar-type stars in the pre-main-sequence phase of evolution---which exhibit activity levels up to four orders of magnitude higher than the present-day Sun---events of this nature and their consequences have yet to be fully explored. We present an approach to modeling the activity of young, solar-mass stars that utilizes stellar X-ray flares and scaled-up solar analogs to investigate the problems of mass loss and angular momentum evolution of pre-main-sequence stars. Analyzing a very large database of time associated solar CME and X-ray flare events, we find a correlation between the energy of a flare and the mass ejected by an associated CME, and we have scaled this relationship to the observed flare energies of young stars. We discuss future work to study the effects of these events on pre-main-sequence evolution.
This research is supported by NSF grant AST-0808072.

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