Spectroscopic Investigations of Be Stars: Non-radial Pulsation Candidates

Details Spectroscopic Investigations of Be Stars: Non-radial Pulsation Candidates Spectroscopic Investigations of Be Stars: Non-radial Pulsation Candidates

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340920g&link_type=abstract

American Astronomical Society, AAS Meeting #213, #409.20; Bulletin of the American Astronomical Society, Vol. 41, p.211

Astronomy and Astrophysics

Astronomy

Scientific paper

Be stars are rapidly rotating B-type stars that lose mass in an equatorial, circumstellar disk (Porter & Rivinius 2003). An important and as-yet-unanswered question is how this circumstellar material actually leaves the surface of the star. One possible answer is non-radial pulsation (NRP). During an earlier 3-year survey of 128 Be stars, we identified 20 NRP candidates. Using spectra from the Kitt Peak Coude' Feed telescope and the echelle spectrograph on the Cerro Tololo 1.5 m telescope, we more closely investigate these candidates, especially to distinguish if they do show NRP or are binary systems. Such stars will be useful to follow-up on to help answer the question of how Be disks form.
This work has been supported in part by NSF Career grant AST-0349075 and NOAO.

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