Volume 452, Number 3, June IV 2006
|Page(s)||1001 - 1010|
|Published online||06 June 2006|
Testing the companion hypothesis for the origin of the X-ray emission from intermediate-mass main-sequence stars
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: email@example.com
2 European Southern Observatory, Casilla 19001, Santiago 19, Chile
Accepted: 20 February 2006
Context.The X-ray emission from B-type main-sequence stars is a longstanding mystery in stellar coronal research. Since there is no theory at hand that explains intrinsic X-ray emission from intermediate-mass main-sequence stars, the observations have often been interpreted in terms of (unknown) late-type magnetically active companion stars.
Aims.Resolving the hypothesized companions requires high spatial resolution observations in the infrared and in X-rays. We use Chandra imaging observations to spatially resolve a sample of main-sequence B-type stars with recently discovered companions at arcsecond separation.
Methods.Our strategy is to search for X-ray emission at the position of both the B-type primary and the faint companion.
Results.We find that all spatially resolved companions are X-ray emitters, but seven out of eleven intermediate-mass stars are also X-ray sources. If this emission is interpreted in terms of additional sub-arcsecond or spectroscopic companions, this implies a high multiplicity of B-type stars. Firm results on B star multiplicity pending, the alternative, that B stars produce intrinsic X-rays, cannot be discarded. An appropriate scenario would be a magnetically confined wind, as suggested for the X-ray emission of the magnetic Ap star IQ Aur. However, the only Ap star in the Chandra sample is not detected in X-rays, and therefore does not support this picture.
Key words: X-rays: stars / stars: early-type / stars: coronae / stars: activity
© ESO, 2006
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