EDP Sciences
Free access
Issue A&A
Volume 415, Number 3, March I 2004
Page(s) 1009 - 1019
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20034160

A&A 415, 1009-1019 (2004)
DOI: 10.1051/0004-6361:20034160

BeppoSAX observations of soft X-ray intermediate polars

D. de Martino1, G. Matt2, T. Belloni3, F. Haberl4 and K. Mukai5

1  INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy
2  Dipartimento di Fisica, Universita' degli Studi Roma Tre, Via della Vasca Navale 84, 00146 Roma, Italy
    e-mail: matt@fis.uniroma3.it
3  INAF-Osservatorio Astronomico di Brera, Via Bianchi 46, Merate, Italy
    e-mail: belloni@merate.mi.astro.it

4  Max-Planck-Institüt für Extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany
    e-mail: fwh@mpe.mpg.de
5  Laboratory for High Energy Astrophysics, NASA/GSFC, Code 662, Greenbelt, MD 20771, USA
    e-mail: mukai@milkyway.gsfc.nasa.gov

(Received 5 August 2003 / Accepted 31 October 2003)

We present broad-band (0.1-90 keV) spectral and temporal properties of the three Intermediate Polars, RE 0751+144 (PQ Gem), RX J0558.0+5353 (V405 Aur) and RX J1712.6-2414 (V2400 Oph) based on simultaneous soft and hard X-ray observations with the BeppoSAX satellite. The analysis of their spectra over the wide energy range of BeppoSAX instruments allows us to identify the soft and hard X-ray components and to determine simultaneously their temperatures. The black-body temperatures of the irradiated poles of the white dwarf atmosphere are found to be 60-100 eV, much higher than those found in their synchronous analogues, the Polars. The temperature of the optically thin post-shock plasma is well constrained in RX J1712.6-2414 and in RE 0751+144 (13 and 17 keV) and less precisely determined in RX J0558.0+5353. In the first two systems evidence of subsolar abundances is found, similarly to that estimated in other magnetic Cataclysmic Variables. A Compton reflection component is present in RX J0558.0+5353 and in RE 0751+144 and it is favoured in RX J1712.6-2414. Its origin is likely at the irradiated white dwarf surface. Although these systems share common properties (a soft X-ray component and optical polarized radiation), their X-ray power spectra and light curves at different energies suggest accretion geometries that cannot be reconciled with a single and simple configuration.

Key words: accretion, accretion discs -- binaries: close -- stars: individual: RE 0751+144 (PQ Gem), RX J0558.0+5353 (V405 Aur), RX J1712.6-2414 (V2400 Oph) -- X-rays: binaries

Offprint request: D. de Martino, demartino@na.astro.it

SIMBAD Objects

© ESO 2004

What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.
  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.

Editor-in-Chief: T. Forveille
Letters Editor-in-Chief: J. Alves
Managing Editor: C. Bertout

ISSN: 0004-6361 ; e-ISSN: 1432-0746
Frequency: 12 volumes per year
Published by: EDP Sciences

Mirror sites: CDS | EDP Sciences
  RSS feeds
© The European Southern Observatory (ESO)