Volume 510, February 2010
|Number of page(s)||8|
|Published online||10 February 2010|
GAPHE, Département AGO, Université de Liège, Allée du 6 Août 17, Bât. B5C, 4000-Liège, Belgium e-mail: firstname.lastname@example.org
2 Department of Physics, Morrisville State College, Morrisville, NY 13408, USA
Accepted: 16 November 2009
High-energy emissions are good indicators of peculiar behaviours in stars. We have therefore obtained an XMM-Newton observation of HD 155806 and 1RXS J171502.4-333344, and derived their spectral properties for the first time. The X-ray spectrum of HD 155806 appears soft, even slightly softer than usual for O-type stars (as shown by a comparison with the O9 star HD 155889 in the same XMM-Newton field). It is well-fitted with a two-component thermal model with low temperatures (0.2 and 0.6 keV), and it shows no overluminosity ( = -6.75). The high-resolution spectrum, though noisy, reveals a few broad, symmetric X-ray lines ( km s-1). The X-ray emission is compatible with the wind-shock model and therefore appears unaffected by the putative dense equatorial regions at the origin of the Oe classification. 1RXS J171502.4-333344 is a nearby flaring source of moderate X-ray luminosity ( = -3), with a soft thermal spectrum composed of narrow lines and presenting a larger abundance of elements (e.g. Ne) with a high first ionization potential (FIP) compared to lower-FIP elements. All the evidence indicates a coronal origin for the X-ray emission, in agreement with the dMe classification of this source.
Key words: X-rays: stars / stars: early-type / stars: individual: 1RXS J171502.4-333344 / stars: individual: HD 155806 / stars: emission-line, Be / X-rays: individuals: HD 155889
© ESO, 2010
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