Mass loss and coronae of cool stars

Details Mass loss and coronae of cool stars Mass loss and coronae of cool stars

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980esasp.157d..33r&link_type=abstract

In ESA 2nd European IUE Conf. 6 p

Astronomy and Astrophysics

Astronomy

Cool Stars, Giant Stars, Iue, Stellar Coronas, Ultraviolet Astronomy, Disks (Shapes), G Stars, Helium, K Stars, Stellar Mass Accretion, Stellar Mass Ejection, Stellar Winds

Scientific paper

Current knowledge about the occurence of coronae and mass loss in cool stars was reviewed. Observational arguments are advanced, stating that both mass loss phenomena and coronae around cool stars vary in a continuous way from solar-type stars via G and K giants to luminous M supergiants. It is pointed out that IUE observations of cool giants with hot companions are important: the absolute scale of mass loss in red giants can be established more accurately by observing circumstellar lines in the UV spectra of companions; nonclose binary companions with rotating disks, formed by accretion from stellar winds of red giants, may serve to study the formation and structure of accretion disks under well defined conditions.

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