Dynamics of the photosphere and shells in the Beta Cephei star Gamma Pegasi

Details Dynamics of the photosphere and shells in the Beta Cephei star Gamma Pegasi Dynamics of the photosphere and shells in the Beta Cephei star Gamma Pegasi

May 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...221..861s&link_type=abstract

Astrophysical Journal, Part 1, vol. 221, May 1, 1978, p. 861-868.

Astronomy and Astrophysics

Astrophysics

19

Light Curve, Photosphere, Stellar Atmospheres, Variable Stars, Abundance, Astrodynamics, B Stars, Chromosphere, O Stars, Radial Velocity, Stellar Spectrophotometry

Scientific paper

Results are presented for a high-resolution spectroscopic study of Gamma Peg performed in the Si III line at 4567 A to determine whether the profile variations in this small-amplitude Beta Cephei star would resemble those observed in several sharp-lined early to middle B-type stars. The observations reported give a firm negative answer, since abundant evidence is found that the star is not a spectroscopic nonradial (traveling-wave) pulsator, at least viewed from the sun's aspect. Therefore, LeContel's (1968) shell components in the present data are interpreted in terms of two shells rising and falling in succession into a radially pulsating photosphere. The origin of the shells is considered, the pulsational energy in the photosphere is estimated, and evidence for a small mass outflow in Gamma Peg is cited. It is noted that the shells may be an additional energizing source for the wind in the star's chromosphere and that a standing nonradial wave model viewed pole-on cannot be totally ruled out.

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