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HgMn Stars as Apparent X-Ray Emitters

Published online by Cambridge University Press:  25 May 2016

S. Hubrig  and
T. W. Berghöfer
S. Hubrig
Affiliation:
University of Potsdam, Am Neuen Palais 10, D-14469 Potsdam, Germany
T. W. Berghöfer
Affiliation:
Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450, USA

Extract

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In the ROSAT all-sky survey 11 HgMn stars were detected as soft X-ray emitters (Berghöfer, Schmitt & Cassinelli 1996). Prior to ROSAT, X-ray observations with the Einstein Observatory had suggested that stars in the spectral range B5-A7 are devoid of X-ray emission. Since there is no X-ray emitting mechanism available for these stars (also not for HgMn stars), the usual argument in the case of an X-ray detected star of this spectral type is the existence of an unseen low-mass companion which is responsible for the X-ray emission. However, this hypothesis is not easily testable. Based on high resolution X-ray images taken with the ROSAT HRI, Berghöfer & Schmitt (1994) showed that known visual late-type companions can be disregarded in this context. In almost all cases studied so far (including two HgMn stars in our sample) the X-ray emission is associated with the primary B star.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 217 - 218
Copyright
Copyright © Kluwer 1998 

References

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