Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-04T21:50:41.750Z Has data issue: false hasContentIssue false
  • English
  • Français

Multiwavelength observations of the Be-star/X-ray binary EXO2030+375 during outburst

Published online by Cambridge University Press:  26 May 2016

A.J. Norton ,
M.J. Coe ,
C. Everall ,
P. Roche ,
L. Bildsten ,
D. Chakrabarty ,
T.A. Prince ,
M.T. Stollberg  and
R.B. Wilson
A.J. Norton
Affiliation:
Dept. of Physics, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
M.J. Coe
Affiliation:
Astronomy & Space Physics Group, Univ. of Southampton, Southampton SO9 5NH, UK
C. Everall
Affiliation:
Astronomy & Space Physics Group, Univ. of Southampton, Southampton SO9 5NH, UK
P. Roche
Affiliation:
Astronomy & Space Physics Group, Univ. of Southampton, Southampton SO9 5NH, UK
L. Bildsten
Affiliation:
Division of Physics, Mathematics & Astronomy, Caltech, Pasadena, CA 91125, USA
D. Chakrabarty
Affiliation:
Division of Physics, Mathematics & Astronomy, Caltech, Pasadena, CA 91125, USA
T.A. Prince
Affiliation:
Division of Physics, Mathematics & Astronomy, Caltech, Pasadena, CA 91125, USA
M.T. Stollberg
Affiliation:
Department of Physics, University of Alabama, Huntsville, AL 35809, USA
R.B. Wilson
Affiliation:
Space Sciences Lab., NASA Marshall Space Flight Center, Huntsville, AL 35812, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

EXO2030+375 consists of a neutron star in an eccentric 46 day orbit around a 20th magnitude Be-star companion (Coe et al., 1988; Parmar et al., 1989; Stollberg et al., 1993). The Be-star is thought to be surrounded by a shell/disc of material which is responsible for the infrared excess and Balmer emission lines which are characteristic of Be-stars in general. At periastron, the neutron star passes through this circumstellar material, giving rise to enhanced accretion onto the neutron star surface. As a result of this, the X-ray emission (pulsed at the neutron star spin period of 41.8s) increases dramatically, so producing the transient, outburst behaviour which is commonly seen in Be-star / X-ray binaries.

Type
3. X-Ray Observations
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 206 - 207
Copyright
Copyright © Kluwer 1994 

References

Coe, M.J., Longmore, A., Payne, B.J. and Hanson, C.G.: 1988, MNRAS 232, 865 CrossRefGoogle Scholar
Parmar, A.N., White, N.E., Stella, L., Izzo, C. & Ferri, P.: 1989, ApJ 338, 359 CrossRefGoogle Scholar
Stollberg, M.T. et al.: 1993, ‘BATSE Observations of EXO2030+375’ in Friedlander, , Gehrels, & Macomb, , ed(s)., CGRO Symposium, St. Louis , AIP Conf. Proc. 280, 371 CrossRefGoogle Scholar