Ultraviolet and optical spectral variability in the Be star Gamma Cassiopeiae - A coronal model for the emission

Details Ultraviolet and optical spectral variability in the Be star Gamma Cassiopeiae - A coronal model for the emission Ultraviolet and optical spectral variability in the Be star Gamma Cassiopeiae - A coronal model for the emission

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..157m&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Aug. 15, 1978, p. 157-166. Research supported by the National Research Council of Cana

Astronomy and Astrophysics

Astrophysics

47

Companion Stars, Emission Spectra, Stellar Models, Ultraviolet Spectra, Binary Stars, Far Ultraviolet Radiation, H Alpha Line, Magnesium, Mass Transfer, Metal Ions, Neutron Stars, Orbital Elements, Spectral Line Width, Stellar Mass Accretion, Stellar Rotation, Stellar Winds

Scientific paper

This paper reports the presence of Mg II emission, the probable presence of Si IV emission, and the possible presence of N V absorption in the UV spectrum of the B0.5 IVe star Gamma Cas. Changes in these features on time scales of several months are described. The detached-ring and mass-exchange binary models are briefly discussed and shown to be inadequate for Gamma Cas. An ad hoc generalization of the detailed stellar-wind model of Poeckert and Marlborough (1978) is presented and suggested as being qualitatively compatible with the UV data as well as with photoelectric H-alpha observations and the X-ray outburst observed in 1976. The presence of a 1-solar-mass neutron star companion with an orbital period of about 4 yr is hypothesized.

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