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The Be/X-ray transient 4U0115+63/V635 Cassiopeiae : II. Outburst mechanisms

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The Be/X-ray transient 4U0115+63/V635 Cassiopeiae : II. Outburst mechanisms

dc.contributor.author	Negueruela, I.
dc.contributor.author	Okazaki, O.T.
dc.contributor.author	Fabregat Llueca, Juan
dc.contributor.author	Coe, M.J.
dc.contributor.author	Munari, U.
dc.contributor.author	Tomov, T.
dc.date.accessioned	2010-06-18T08:05:10Z
dc.date.available	2010-06-18T08:05:10Z
dc.date.issued	2001
dc.identifier.citation	NEGUERUELA, I. ; Okazaki, O.T. ; Fabregat Llueca, Juan ; Coe, M.J. ; Munari, U. ; Tomov, T. ; 2001, The Be/X-ray transient 4U0115+63/V635 Cassiopeiae : II. Outburst mechanisms, Astronomy and Astrophysics, vol. 369, no. 1, p. 117-131	en
dc.identifier.uri	http://hdl.handle.net/10550/12992
dc.description.abstract	We present multi-wavelength long-term monitoring observations of V635 Cas, the optical counterpart to the transient X-ray pulsar 4U0115+63. The evolution of emission lines and photometric magnitudes indicates that the Be star undergoes relatively fast ( ~3 - 5yr) quasi-cyclic activity, losing and reforming its circumstellar disc. We show that the general optical, infrared and X-ray behaviour can be explained by the dynamical evolution of the viscous circumstellar disc around the Be star. After each disc-loss episode, the disc starts reforming and grows until it reaches the radius at which the resonant interaction of the neutron star truncates it. At some point, the disc becomes unstable to (presumably radiative) warping and then tilts and starts precessing. The tilting is very large and disc precession leads to a succession of single-peaked and shell profiles in the emission lines. Type II X-ray outbursts take place after the disc has been strongly disturbed and we speculate that the distortion of the disc leads to interaction with the orbiting neutron star. We discuss the implications of these correlated optical/X-ray variations for the different models proposed to explain the occurrence of X-ray outbursts in Be/X-ray binaries. We show that the hypothesis of mass ejection events as the cause of the spectacular variability and the X-ray outbursts is unlikely to be meaningful for any Be/X-ray binary.	en
dc.language.iso	en	en
dc.subject	Circumstellar matter ; Emission-line ; Stars ; 4U 0115+63 ; Binaries ; Neutron ; X-ray	en
dc.title	The Be/X-ray transient 4U0115+63/V635 Cassiopeiae : II. Outburst mechanisms	en
dc.type	journal article	es_ES
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA	en
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia	en
dc.identifier.doi	10.1051/0004-6361:20010077	en
dc.identifier.idgrec	007794	en
dc.type.hasVersion	VoR	es_ES
dc.identifier.url	http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/pdf/2001/13/aa9965.pdf	en