Mass loss from solar-type stars

Details Mass loss from solar-type stars Mass loss from solar-type stars

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph..100..587h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 100, Oct. 1985, p. 587-597.

Physics

5

Main Sequence Stars, Solar Wind, Star Clusters, Stellar Mass Ejection, Stellar Winds, T Tauri Stars, Angular Momentum, Balmer Series, Early Stars, Line Spectra

Scientific paper

The present picture of mass loss from solar-type (low-mass) stars is described, with special emphasis on winds from pre-main-sequence stars. Attention is given to winds from T Tauri stars and to angular momentum loss. Prospects are good for further advances in our understanding of the powerful mass loss observed from young stars; ultraviolet spectra obtainable with the Space Telescope should provide better estimates of mass loss rates and a clearer picture of physical conditions in the envelopes of these stars. To understand the mass ejection from old, slowly rotating main-sequence stars, we will have to study the sun.

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