Time-resolved H-alpha spectroscopy of the Be star PLEIONE during a lunar occultation

Details Time-resolved H-alpha spectroscopy of the Be star PLEIONE during a lunar occultation Time-resolved H-alpha spectroscopy of the Be star PLEIONE during a lunar occultation

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100.1601g&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 100, Nov. 1990, p. 1601-1609.

Astronomy and Astrophysics

Astronomy

21

B Stars, H Alpha Line, Lunar Occultation, Stellar Spectra, Balmer Series, Emission Spectra, Light Curve, Stellar Envelopes, Temporal Resolution

Scientific paper

Low-resolution spectra with a time sampling rate of 7 ms of the H-alpha emission line in the spectrum of the Be star Pleione during the dark limb lunar occultation of 1987 March 6 was obtained. The center of light of the emission envelope was occulted 5.5 + or - 1.1 ms before the continuum light of the star itself which suggests that there is a geometric asymmetry in the envelope. For a Pleiades distance of 128 pc, the difference in occultation times corresponds to a spatial separation of 4-7 times the radius of Pleione between the center of the star and the center of the emission flux distribution. A high-resolution H-alpha spectrum obtained two months earlier displays a double peaked profile with a violet-to-red peak ratio of 1.3. Assuming that the violet and red portions of the emission line can be associated with the parts of the envelope occulted before and after the star, a simple model of the envelope to derive a mean radius of 34-55 stellar radii is used. The asymmetry in the envelope could be due to the gravitational influence of a binary companion recently discovered by speckle interferometry, and it is suggested that the shell episodes observed in Pleione are driven by tidal interactions near periastron.

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