Open AccessShort period line profile and light variations in the Be star ω Orionis
Author(s) -
Balona L.A.,
Aerts C.,
Božić H.,
Guinan E.F.,
Handler G.,
James D.J.,
Kaye A.B.,
Shobbrook R.R.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04831.x
Subject(s) - physics , astrophysics , photometry (optics) , radial velocity , rotation period , spectral line , line (geometry) , be star , astronomy , stars , geometry , mathematics
We present the results of a multisite spectroscopic and photometric campaign on the Be star ω Orionis. From the photometry and radial velocity variation of several spectral lines, we confirm that the star is a variable with period . 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 is considerably smaller than from the metal lines . 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 H β . From this we conclude that the periodic variations are most probably associated with corotating circumstellar material.