Multi-wavelength studies of the high mass X-ray binaries X Persei (4U0352+309) and OAO1657-415
Multi-wavelength studies of the high mass X-ray binaries X Persei (4U0352+309) and OAO1657-415
This work deals with the study of High-Mass X-ray Binaries using a multi-wavelength approach (optical, infrared and X-ray). It is shown that long-term, multi-wavelength monitoring is perhaps the best method for studying such complex systems, whether in the study of known sources or in the search for optical counterparts.
The unusual Be/X-ray binary system X Persei (4U0352+ 53) is observed undergoing a dramatic phase change event, associated with the loss of the circumstellar disk surrounding Be-type stars. New observations of the underlying primary star, usually obscured by the disk, are presented, allowing detailed estimation of a variety of stellar parameters, including a greatly increased distance. Based on the characteristics of the phase change event observed in 1988-1989, a previously undiscovered phase change (or near-phase change) is proposed for the mid-1970's. Archival data is re-analysed in the light of the proposed disk-loss event, including the apparent influence of disk material on the neutron star companion, where the spin period is observed to decrease as accretion increases.
Detailed observations of the recent phase change are presented, revealing a lack of optical variability in the system when the disk is absent (suggesting the disk, or at least disk forming mechanism, is responsible for the usual 0.8 mags. of V band variability observed in X Per). A search for variability in the Balmer emission line Hα shows no evidence for the pulsar spin period. The infrared excess of X Per is found to be best fit by a 10,000 K blackbody, with a cooler component visible at longer wavelengths. It is proposed that variability in the strength of non-radial pulsations in the primary may have been responsible for the disk-loss and subsequent OB phase.
University of Southampton
1993
Roche, Paul Dominic
(1993)
Multi-wavelength studies of the high mass X-ray binaries X Persei (4U0352+309) and OAO1657-415.
University of Southampton, Doctoral Thesis.
Record type:
Thesis
(Doctoral)
Abstract
This work deals with the study of High-Mass X-ray Binaries using a multi-wavelength approach (optical, infrared and X-ray). It is shown that long-term, multi-wavelength monitoring is perhaps the best method for studying such complex systems, whether in the study of known sources or in the search for optical counterparts.
The unusual Be/X-ray binary system X Persei (4U0352+ 53) is observed undergoing a dramatic phase change event, associated with the loss of the circumstellar disk surrounding Be-type stars. New observations of the underlying primary star, usually obscured by the disk, are presented, allowing detailed estimation of a variety of stellar parameters, including a greatly increased distance. Based on the characteristics of the phase change event observed in 1988-1989, a previously undiscovered phase change (or near-phase change) is proposed for the mid-1970's. Archival data is re-analysed in the light of the proposed disk-loss event, including the apparent influence of disk material on the neutron star companion, where the spin period is observed to decrease as accretion increases.
Detailed observations of the recent phase change are presented, revealing a lack of optical variability in the system when the disk is absent (suggesting the disk, or at least disk forming mechanism, is responsible for the usual 0.8 mags. of V band variability observed in X Per). A search for variability in the Balmer emission line Hα shows no evidence for the pulsar spin period. The infrared excess of X Per is found to be best fit by a 10,000 K blackbody, with a cooler component visible at longer wavelengths. It is proposed that variability in the strength of non-radial pulsations in the primary may have been responsible for the disk-loss and subsequent OB phase.
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Published date: 1993
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Local EPrints ID: 462268
URI: http://eprints.soton.ac.uk/id/eprint/462268
PURE UUID: 2c45be48-9878-48b8-8683-5822e0a8b867
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Date deposited: 04 Jul 2022 19:04
Last modified: 04 Jul 2022 19:04
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Author:
Paul Dominic Roche
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