Issue |
A&A
Volume 417, Number 2, April II 2004
|
|
---|---|---|
Page(s) | 715 - 723 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20031783 | |
Published online | 19 March 2004 |
A new phase of activity of the Herbig Be star HD 200775 in 2001: Evidence for binarity*
1
Pulkovo Observatory, Saint-Petersburg 196140, Russia
2
Isaac Newton Institute of Chile, Saint-Petersburg Branch, Russia
3
Ritter Observatory, Dept. of Physics & Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA
4
Crimean Astrophysical Observatory, Nauchny, Crimea 334413, Ukraine
5
Isaak Newton Institute of Chile, Crimean Branch, Ukraine
6
Special Astrophysical Observatory at Northern Caucasus, Nizhnij Arkhys 357147, Russia
7
CFHT Corporation, 65–1238 Mamalahoa Hwy, Kamuela, HI 96743, Hawaii, USA
Corresponding author: M. A. Pogodin, pogodin@gao.spb.ru
Received:
6
June
2003
Accepted:
18
December
2003
The results of high-resolution spectroscopy of the
Herbig Be star HD 200775 obtained within the framework of a cooperative observing
programme in 2000–2002 are presented. A new high-activity phase of the
object's Hα line occurred in the middle of 2001 in full agreement
with a 3.68-year periodicity predicted by Miroshnichenko et al. ([CITE]).
A complicated picture of the Hα line profile variability near the
activity maximum phase turned out to be very similar to that
observed during the previous one in 1997.
Variations of the radial velocity with the activity phase are detected
in He i, Si ii, and S ii photospheric lines.
The observed phenomena are interpreted in the framework of a model in which
the star, together with its gaseous envelope, is a component of an eccentric
binary system. A preliminary orbital solution is derived, and the system's
parameters are estimated from the radial velocity curves of the Hα
emission line.
We find that the orbital eccentricity is , the mean companion
separation is ~1000
, and the secondary companion is most likely to be
a ~3.5
pre-main sequence object.
We emphasize the importance of coordinated spectroscopic and
interferometric observations at different phases of the object's activity
for further understanding the properties of the system.
Key words: techniques: spectroscopic / stars: circumstellar matter / stars: individual: HD 200775 / stars: binaries: spectroscopic / stars: pre-main sequence
© ESO, 2004
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