Testing the companion hypothesis for the origin of the X-ray emission from intermediate-mass main-sequence stars

Details Testing the companion hypothesis for the origin of the X-ray emission from intermediate-mass main-sequence stars Testing the companion hypothesis for the origin of the X-ray emission from intermediate-mass main-sequence stars

2006-02-23

arxiv.org/abs/astro-ph/0602517v1

Astronomy and Astrophysics

Astrophysics

12 pages; accepted for publication in Astronomy & Astrophysics

Scientific paper

10.1051/0004-6361:20054405

There is no straightforward explanation for intrinsic X-ray emission from intermediate-mass main-sequence stars. Therefore the observed emission is often interpreted in terms of (hypothesized) late-type magnetically active companion stars. We use Chandra imaging observations to spatially resolve in X-rays a sample of main-sequence B-type stars with recently discovered companions at arcsecond separation. 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, can not be discarded. The appropriate scenario in this vein is might 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.

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