Short period line profile and light variations in the Be star ? Orionis

Autor(en)

Luis A. Balona, Conny Aerts, Hrvoje Bozic, Edward F. Guinan, Gerald Handler, David J. James, Anthony B Kaye, R R Shobbrook

Abstrakt

We present the results of a multisite spectroscopic and photometric campaign on the Be star ? Orionis. From the photometry and radial velocity variation of several spectral lines, we confirm that the star is a variable with period P = 0.97 d. Only one period can be extracted from both the photometric and radial velocity observations. We find that the projected rotational velocity from the helium lines (v sin i = 173 km s-1) is considerably smaller than from the metal lines (v sin i = 226 km s-1). The line profiles show an excess absorption feature moving from blue to red for half the period and from red to blue for the other half of the period. Another excess absorption feature moves exactly out of phase. The excess absorption features are present in photospheric lines as well as in lines which are significantly affected by circumstellar material, such as Hß. From this we conclude that the periodic variations are most probably associated with corotating circumstellar material.

Organisation(en)

Institut für Astrophysik

Externe Organisation(en)

South African Astronomical Observatory (SAAO), Katholieke Universiteit Leuven, University of Zagreb, Villanova University, Observatoire des sciences de l'univers de Grenoble, Los Alamos National Laboratory, Australian National University

Journal

Monthly Notices of the Royal Astronomical Society

Band

327

Seiten

1288-1296

Anzahl der Seiten

9

ISSN

0035-8711

Publikationsdatum

2001

Peer-reviewed

Ja

ÖFOS 2012

103003 Astronomie

Link zum Portal

https://ucrisportal.univie.ac.at/de/publications/b7ed5cee-c631-41c8-bc53-9bfca27b2581