EDP Sciences
Free access
Volume 440, Number 2, September III 2005
Page(s) 727 - 734
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20042596

A&A 440, 727-734 (2005)
DOI: 10.1051/0004-6361:20042596

Detection of X-ray emission from $\beta$ Pictoris with XMM-Newton: a cool corona, a boundary layer or what?

M. Hempel1, 2, J. Robrade2, J.-U. Ness2, 3 and J. H. M. M. Schmitt2

1  AIU Jena, Schillergäßchen 2-3, 07745 Jena, Germany
    e-mail: marc@astro.uni-jena.de
2  Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
3  Department of Physics, Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK

(Received 22 December 2004 / Accepted 9 May 2005)

$\beta$ Pictoris ( HR 2020 ) is the most prominent prototype of stars with circumstellar disks and has generated particular interest in the framework of young planetary systems. Given its spectral type A5, stellar activity is not expected. Nevertheless, resonance lines of C III and O VI typical for a chromosphere and transition region have been unambiguously detected with FUSE. We present results from an XMM-Newton observation of $\beta$ Pic and find evidence for X-ray emission. In particular, we detected an emission of O VII at 21.6 Å with the MOS detectors. These findings present a challenge for the development of both stellar activity and disk models. We discuss and investigate various models to explain the observed emission including the presence of a cool corona and a boundary layer.

Key words: stars: activity -- stars: circumstellar matter -- stars: individual: HR 2020 -- ultraviolet: stars -- X-rays: stars

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