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Astron. Astrophys. 347, 932-936 (1999)
The long-period RS Canum Venaticorum binary IM Pegasi
I. Orbital and stellar
parameters *
S.V. Berdyugina,
I. Ilyin and
I. Tuominen
Astronomy Division, University of Oulu, P.O. Box 3000, FIN-90401 Oulu, Finland
Received 30 April 1999 / Accepted 21 May 1999
Abstract
New high-resolution and high signal-to-noise ratio spectroscopic
observations carried out in 1996-1997 are analysed. A total of 85 new
high quality radial velocity measurements are used for determining the
new orbital parameters:
=HJD2450342.883+24.64880E ,
e=0.0,
=-14.09 km s-1,
K1=34.39 km s-1. A model atmosphere analysis of
the averaged spectrum of the star has yielded a self-consistent set of
fundamental parameters of the primary component:
=4450 K, log g =2.4, [M/H]=0.0,
=1.6 km s-1,
v sini =26.5 km s-1. The primary is found to
be a typical K2 III giant with the mass of about
1.5 which has undergone the first
convective mixing on the Red Giant Branch ([C/H]=-0.32, [N/H]=0.30,
C/N=1.15). The unspotted V magnitude of the star of
5 55 is estimated from the observed
variations of the TiO band and quasi-simultaneous photometry.
Combining all parameters, the radius and inclination of the primary as
well as a probable spectral class of the secondary are estimated.
Key words: stars:
abundances
stars: activity
stars: binaries:
spectroscopic
stars: fundamental
parameters
stars: individual:
IM Peg
stars: late-type
* based on observations collected at the 2.6 m telescope of the Crimean Astrophysical Observatory, Ukraine and the Nordic Optical Telescope (NOT), La Palma, Spain
Send offprint requests to: S.V. Berdyugina (sveta@ukko.oulu.fi)
SIMBAD Objects
Contents
© European Southern Observatory (ESO) 1999
Online publication: June 6, 1999
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