Hot and cool: two emission-line stars with constrasting behaviours in the same XMM-Newton field^*,**

Y. Nazé¹, G. Rauw¹ and A. ud-Doula²

¹ GAPHE, Département AGO, Université de Liège, Allée du 6 Août 17, Bât. B5C, 4000-Liège, Belgium e-mail: naze@astro.ulg.ac.be
² Department of Physics, Morrisville State College, Morrisville, NY 13408, USA

Received: 14 August 2009
Accepted: 16 November 2009

Abstract

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.