Previous | Session 14 | Next
G.A.H. Walker, J. M. Matthews, R. Kuschnig (University of British Columbia), A.F.J. Moffat (Université de Montréal), S. Rucinski (David Dunlap Observatory), D. B. Guenther (St. Mary's University), D. Sasselov (Harvard-Smithsonian Center for Astrophysics), P. Reegen, W.W. Weiss (University of Vienna), E. Kambe (National Defence Academy, Yokosuka)
\zeta Oph is a rapidly rotating (vsini~400 km s-1) O9 III emission-line star with line profile variations characteristic of sectorial, non-radial pulsations. The MOST photometric satellite observed \zeta Oph for 23 days from 19 May to 11 June 2004. Half second exposures were taken every ten seconds with a 60% useful duty cycle on each satellite orbit. There are several significant peaks between 1.5 and 7.5 c/d in the frequency spectrum which can be identified with radial and non-radial oscillations, and the stellar rotational period. Pulsations of even higher degree can be seen in the profiles of H\beta and the He I lines which were monitored simultaneously at the Dominion Astrophysical, Gunma, and Ondrejov Observatories.
Previous | Session 14 | Next
Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.