Discovery and preliminary identification of two retrograde nonradial pulsation modes in the Be star MU Centauri

Details Discovery and preliminary identification of two retrograde nonradial pulsation modes in the Be star MU Centauri Discovery and preliminary identification of two retrograde nonradial pulsation modes in the Be star MU Centauri

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...135..101b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 135, no. 1, June 1984, p. 101-106.

Astronomy and Astrophysics

Astrophysics

71

B Stars, Coupled Modes, Stellar Oscillations, Stellar Spectrophotometry, Variable Stars, Vibration Mode, Absorption Spectra, Angular Velocity, Data Reduction, H Alpha Line, High Resolution, Stellar Models

Scientific paper

High-resolution Reticon spectra of the Be star Mu Cen at Mg II 4481 A show on average three to four about equally spaced weak absorption features moving from positive to negative velocities across the line profile. The asymmetry of the profile as a whole changes in the same direction, but more slowly. The latter variation is periodic with P = 0.505 d which turns out to be five times the period of the weaker absorption features. These effects are interpreted as being due to an l = 10, m = + 10 and an l = 2, m = + 2 mode, respectively. Because of the common angular velocity of the pulsation velocity pattern on the stellar surface, the two modes are believed to be resonantly coupled. It is shown that such coupling is more likely in rapidly rotating stars and that coupling of two retrograde modes is probably favored. Simple model line profile calculations are in satisfactory agreement with the observations. There is some reason to believe that other absorption line profile variable Be stars can be explained by the same model.

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