Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.229d&link_type=abstract
In JPL Solar Wind Five p 229-240 (SEE N84-13067 03-92)
Astronomy and Astrophysics
Astronomy
Astronomical Spectroscopy, Binary Stars, Cool Stars, Stellar Atmospheres, Stellar Winds, Emission Spectra, Stellar Luminosity, Stellar Magnetic Fields, Stellar Temperature, Wind Velocity
Scientific paper
Sufficient observational material - ultraviolet spectroscopic measures, quantitative optical spectroscopy, and X-ray photometry exists to enable discernment of the presence and character of mass loss in cool stars and to establish meaningful constraints on theoretical models. Two determinants of atmospheric wind structure - temperature and gravity - may suffice in a most superficial way to define the wind and atmospheric structure in a star; however more extensive observations demonstrate the importance of magnetic surface activity and its particular geometrical configuration. Successive observations of an active binary system and a supergiant star reveal that magnetic activity and perhaps mass loss occur on restricted regions of a stellar surface and that long lived structures are present in a wind.
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