The Ultraviolet Light Curve of LMC X‐4: X‐Ray Heating of the O Star and Accretion Disk
We present an archival study of ultraviolet spectra of the X‐ray binary LMC X‐4 obtained with theIUEsatellite. We fit these spectra with models that incorporate the X‐ray heating of the O star and accretion disk. A systematic analysis of the UV continuum confirms the general picture of an O star tha...
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| Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 2002-03, Vol.114 (793), p.340-349 |
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| container_title | Publications of the Astronomical Society of the Pacific |
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| creator | Preciado, Michael E. Boroson, Bram Vrtilek, Saeqa Dil |
| description | We present an archival study of ultraviolet spectra of the X‐ray binary LMC X‐4 obtained with theIUEsatellite. We fit these spectra with models that incorporate the X‐ray heating of the O star and accretion disk. A systematic analysis of the UV continuum confirms the general picture of an O star that fills its Roche lobe and is heated by X‐rays from the neutron star. About 5% of the UV emission arises in an accretion disk, which may precess with a ≈30 day period. We measure the mass transfer through the accretion disk and attempt to relate this quantity to changes in the pulse period and disk precession. The principal source of uncertainty in our model results from the choice of the 30 day disk precession ephemeris. We examine theRXTEAll‐Sky Monitor data for LMC X‐4 to attempt to clarify the variability of the 30 day period. We find no evidence for additional heating of the O star or disk as the result of an X‐ray flare observed withIUEandEXOSATin 1983. |
| doi_str_mv | 10.1086/339254 |
| format | Article |
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We fit these spectra with models that incorporate the X‐ray heating of the O star and accretion disk. A systematic analysis of the UV continuum confirms the general picture of an O star that fills its Roche lobe and is heated by X‐rays from the neutron star. About 5% of the UV emission arises in an accretion disk, which may precess with a ≈30 day period. We measure the mass transfer through the accretion disk and attempt to relate this quantity to changes in the pulse period and disk precession. The principal source of uncertainty in our model results from the choice of the 30 day disk precession ephemeris. We examine theRXTEAll‐Sky Monitor data for LMC X‐4 to attempt to clarify the variability of the 30 day period. 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| issn | 0004-6280 1538-3873 |
| language | eng |
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| source | IOP Publishing Journals; JSTOR Archive Collection A-Z Listing; EZB-FREE-00999 freely available EZB journals; Institute of Physics (IOP) Journals - HEAL-Link; Alma/SFX Local Collection |
| subjects | Accretion disks Ephemerides Mass transfer Neutron stars O stars Precession Stellar flares Stellar luminosities Stellar radii Wavelengths |
| title | The Ultraviolet Light Curve of LMC X‐4: X‐Ray Heating of the O Star and Accretion Disk |
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