Other
Scientific paper
Aug 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...283..303m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 283, Aug. 1, 1984, p. 303-312.
Other
132
Plasma Interactions, Stellar Rotation, Stellar Winds, Absorption Spectra, Chromosphere, Giant Stars, Hot Stars, Particle Acceleration, Solar Wind, Supergiant Stars, Ultraviolet Spectra
Scientific paper
In a stellar wind, a corotating interaction region (CIR) is formed when a rotating star emits wind in a non-spherically symmetric manner. CIRs have been studied in detail in the solar wind: here, their role in stellar winds is considered. The radial distance at which CIRs form (in terms of the stellar radius) is proportional to the ratio of wind speed to the rotational speed at the stellar surface: in the sun, this ratio is approximately 200, but it may be much smaller than that in other stars. The properties of CIRs appear to be able to account for certain features of 'hybrid stars' (i.e., cool giants with cool winds plus 'warm' lines in their UV spectra), for X-ray emitting structures in hot star winds, and for the appearance of extended chromospheres in cool supergiants.
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