The nonradial oscillations of Epsilon Persei. II - Nonlinear characteristics

Details The nonradial oscillations of Epsilon Persei. II - Nonlinear characteristics The nonradial oscillations of Epsilon Persei. II - Nonlinear characteristics

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..768s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 15, 1987, p. 768-793.

Astronomy and Astrophysics

Astrophysics

33

B Stars, Nonlinearity, O Stars, Stellar Models, Stellar Oscillations, Stellar Spectrophotometry, Charge Coupled Devices, Spectral Energy Distribution, Spectrum Analysis, Ubv Spectra

Scientific paper

During five nights in 1984 November the authors obtained over 300 high quality CCD exposures of the Si III λ4552-4574 lines in ɛ Persei (B0.7 III), a star with remarkably large line profile variations. Detailed line profile models have been computed for a sample of over 60 of them, and these show that the variations are described well in the framework of nonradial pulsation (NRP) by two modes, a dominant one described by -m = l = 4 (mean period, 3.85±0.02 hr) and a secondary one by -m = l = 6 (2.25±0.3 hr). This study provides also a definition of the nonlinear properties of NRP waves, which can show extreme variations in amplitude both in time and around the wave pattern. The analysis suggests a simple picture in which a wave becomes marginally supersonic in the stellar atmosphere, develops an increasingly nonsinusoidal waveform, and partially loses its coherence by interfering with itself as it circuits the star.

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