Volume 449, Number 3, April III 2006
|Page(s)||1151 - 1160|
|Section||Stellar structure and evolution|
|Published online||24 March 2006|
The long period intermediate polar 1RXS J154814.5-452845
INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy e-mail: email@example.com
2 Service d'Astrophysique, DSM/DAPNIA/SAp, CE Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: firstname.lastname@example.org
3 APC, UMR 7164, University Denis Diderot, 2 place Jussieu, 75005 Paris, France
4 LUTH, Observatoire de Paris, Section de Meudon, 92190 Meudon, France e-mail: email@example.com
5 Department of Physics, University of Warwick, Coventry CV4 7AL, UK e-mail: firstname.lastname@example.org
6 Max-Planck-Institüt für Extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany e-mail: email@example.com
7 Observatoire Astronomique, UA 1280 CNRS, 11 rue de l'Université, 67000 Strasbourg, France e-mail: firstname.lastname@example.org
Accepted: 18 December 2005
We present the first time resolved medium resolution optical spectroscopy of the recently identified peculiar Intermediate Polar (IP) 1RXS J154814.5-452845, which allows us to precisely determine the binary orbital period ( ± 0.03 h) and the white dwarf spin period ( ± 0.06 s). This system is then the third just outside the purported ~6–10 h IP orbital period gap and the fifth of the small group of long period IPs, which has a relatively high degree of asynchronism. From the presence of weak red absorption features, we identify the secondary star with a spectral type K2 ± 2 V, which appears to have evolved on the nuclear timescale. From the orbital radial velocities of emission and the red absorption lines a mass ratio ± 0.12 is found. The masses of the components are estimated to be and and the binary inclination . A distance between 540–840 pc is estimated. At this distance, the presence of peculiar absorption features surrounding Balmer emissions cannot be due to the contribution of the white dwarf photosphere and their spin modulation suggests an origin in the magnetically confined accretion flow. The white dwarf is also not accreting at a particularly high rate ( ), for its orbital period. The spin-to-orbit period ratio = 0.02 and the low mass accretion rate suggest that this system is far from spin equilibrium. The magnetic moment of the accreting white dwarf is found to be 1032 G cm3, indicating a low magnetic field system.
Key words: accretion, accretion disks / stars: binaries: close / stars: novae, cataclysmic variables
© ESO, 2006
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