Volume 429, Number 1, January I 2005
|Page(s)||309 - 316|
|Section||Stellar structure and evolution|
|Published online||13 December 2004|
Orbital period variation in close binaries from radial velocity data and magnetic activity cycles *,**
II. HR 1099
INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, Città Universitaria, 95123 Catania, Italy e-mail: firstname.lastname@example.org
Accepted: 1 September 2004
We studied orbital period changes in the non-eclipsing close binary HR 1099, one of the most bright members of the RS CVn class of magnetically active binary systems. Intermediate-resolution optical spectroscopy and IUE archive spectra were used to build radial-velocity curves yielding epochs of superior conjunction with an accuracy of 0.01 days. The final database ranged from 1976 to 2002 and allowed us a better assessment of the amplitude of the orbital period variation and its timescale. On the basis of such results, the mechanisms proposed to explain the observed period change were briefly discussed giving further support to the possible connection between the orbital period modulation and the change of the gravitational quadrupole moment of the K1 subgiant component, in the framework of the model elaborated by Lanza et al. ([CITE]).
Key words: stars: binaries: close / stars: activity / stars: binaries spectroscopic / stars: individual: HR 1099
© ESO, 2005
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.