Volume 407, Number 3, September I 2003
|Page(s)||987 - 998|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
The near-synchronous polar V1432 Aql (RX J1940.1–1025): Accretion geometry and synchronization time scale
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
2 Institut für Theoretische Physik und Astrophysik, Universität Kiel, Leibnizstr. 15, 24098 Kiel, Germany
3 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, 85748 Garching, Germany
4 Integral Science Data Centre, 16 Chemin d'Ecogia, 1290 Versoix, Switzerland
5 Sternwarte Sonneberg, Sternwartestr. 32, 96515 Sonneberg, Germany
6 Center for Astrophysics and Space Science (CASS), Univ. California, San Diego, California, USA
Corresponding author: R. Staubert, email@example.com
Accepted: 28 May 2003
The magnetic Cataclysmic Variable (mCV) V1432 Aql (RX J1940.1–1025) belongs to the four-member subclass of near-synchronous polars with a slight non-synchronism (<2%) between the spin period of the white dwarf and the binary period. In these systems the accretion geometry changes periodically with phase of the beat cycle. We present the application of a dipole accretion model for near-synchronous systems developed by Geckeler & Staubert (1997a) to extended optical and X-ray data. We detect a significant secular change of the white dwarf spin period in V1432 Aql of s/s from the optical data set alone. This corresponds to a synchronization time scale yr, comparable to the time scale of 170 yr for V1500 Cyg. The synchronization time scale in V1432 Aql is in excellent agreement with the theoretical prediction from the dominating magnetic torque in near-synchronous systems. We also present period analyses of optical CCD photometry and RXTE X-ray data, which argue against the existence of a 4000 s period and an interpretation of V1432 Aql as an intermediate polar. The dipole accretion model also allows us to constrain the relevant parameters of the accretion geometry in this system: the optical data allow an estimate of the dimensionless parameter , with a lower limit for the threading radius of (68% confidence).
Key words: stars: variables: general / stars: binaries: eclipsing / stars: individual: V1432 Aql; RX J1940.1–1025 / stars: magnetic fields / X-rays: stars
© ESO, 2003
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