TE structure of the wind in gamma CAS

Details TE structure of the wind in gamma CAS TE structure of the wind in gamma CAS

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980esasp.157..145d&link_type=abstract

In ESA 2nd European IUE Conf. P 145-146

Astronomy and Astrophysics

Astronomy

8

B Stars, Iue, Shell Stars, Stellar Winds, Ultraviolet Astronomy, Absorption Spectra, Cassiopeia Constellation, Chromosphere, Emission Spectra, Stellar Coronas, Stellar Spectra, Variable Stars

Scientific paper

UV observations of the wind in gamma Cas, via measure of line displacements, delineate two distinct and nonoverlapping velocity regions where absorbing ions for Si4, C4, N5 are concentrated at about 100 km/sec and 1400 km/sec. Absence of appreciable numbers of these ions absorbing at intermediate velocities suggests the presence of a corona too hot to support such ions in those atmospheric regions where such velocities occur; observed soft X-ray emission at coronal intensities from gamma Cas supports this picture. Visual studies show that the present phase of gamma Cas is moderately strong Be, and not B-shell. This Be-phase UB velocity behavior is contrasted with the present, rising from quasi B-normal, toward Be, phase behavior of 59 Cyg, where only the high velocity regime is observed in superionized species, and only the low velocity regime in photospheric Si4.

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