The lack of X-ray pulsations in the extreme helium star BD+37°442 and its possible stellar wind X-ray emission

• Published in: Monthly notices of the Royal Astronomical Society 2017-04, Vol.466 (3), p.2918-2921
• Main Authors: Mereghetti, Sandro, La Palombara, Nicola, Tiengo, Andrea, Esposito, Paolo
• Format: Article
• Language: English
• Subjects: Astronomy; Helium; Luminosity; Star & galaxy formation; X-ray astronomy
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stw3335

Abstract We report the results of a new XMM–Newton observation of the helium-rich hot subdwarf BD+37°442 carried out in 2016 February. The possible periodicity at 19 s seen in a 2011 shorter observation is not confirmed, thus dismissing the evidence for a binary nature. This implies that the observed soft X-ray emission, with a luminosity of a few 1031 erg s−1, originates in BD+37°442 itself, rather than in an accreting neutron star companion. The X-ray spectrum is well fit by thermal plasma emission with a temperature of 0.22 keV and non-solar element abundances. Besides the overabundance of He, C and N already known from optical/UV studies, the X-ray spectra indicate also a significant excess of Ne. The soft X-ray spectrum and the ratio of X-ray to bolometric luminosity, LX/LBOL ∼ 2 × 10−7, are similar to those observed in massive early-type stars. This indicates that the mechanisms responsible for plasma shock-heating can work also in the weak stellar winds (mass-loss rates $\dot{M}_{\rm W}\le 10^{-8}$  M⊙ yr−1) of low-mass hot stars.