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Article: Swift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13

TitleSwift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13
Authors
Issue Date2017
PublisherAmerican Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
The Astrophysical Journal Letters, 2017, v. 835 n. 1, p. L9:1-6 How to Cite?
AbstractNGC 7793 P13 is an ultraluminous X-ray source harboring an accreting pulsar. We report on the detection of a ~65 day period X-ray modulation with Swift observations in this system. The modulation period found in the X-ray band is P = 65.05 ± 0.10 days and the profile is asymmetric with a fast rise and a slower decay. On the other hand, the u-band light curve collected by Swift UVOT confirmed an optical modulation with a period of P = 64.24 ± 0.13 days. We explored the phase evolution of the X-ray and optical periodicities and propose two solutions. A superorbital modulation with a period of ~2700–4700 days probably caused by the precession of a warped accretion disk is necessary to interpret the phase drift of the optical data. We further discuss the implication if this ~65 day periodicity is caused by the superorbital modulation. Estimated from the relationship between the spin-orbital and orbital-superorbital periods of known disk-fed high-mass X-ray binaries, the orbital period of P13 is roughly estimated as 3–7 days. In this case, an unknown mechanism with a much longer timescale is needed to interpret the phase drift. Further studies on the stability of these two periodicities with a long-term monitoring could help us to probe their physical origins.
Persistent Identifierhttp://hdl.handle.net/10722/238709
ISSN
2017 Impact Factor: 6.634
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorHu, CP-
dc.contributor.authorLi, KL-
dc.contributor.authorKong, AKH-
dc.contributor.authorNg, SCY-
dc.contributor.authorLin, LCC-
dc.date.accessioned2017-02-20T01:25:01Z-
dc.date.available2017-02-20T01:25:01Z-
dc.date.issued2017-
dc.identifier.citationThe Astrophysical Journal Letters, 2017, v. 835 n. 1, p. L9:1-6-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/238709-
dc.description.abstractNGC 7793 P13 is an ultraluminous X-ray source harboring an accreting pulsar. We report on the detection of a ~65 day period X-ray modulation with Swift observations in this system. The modulation period found in the X-ray band is P = 65.05 ± 0.10 days and the profile is asymmetric with a fast rise and a slower decay. On the other hand, the u-band light curve collected by Swift UVOT confirmed an optical modulation with a period of P = 64.24 ± 0.13 days. We explored the phase evolution of the X-ray and optical periodicities and propose two solutions. A superorbital modulation with a period of ~2700–4700 days probably caused by the precession of a warped accretion disk is necessary to interpret the phase drift of the optical data. We further discuss the implication if this ~65 day periodicity is caused by the superorbital modulation. Estimated from the relationship between the spin-orbital and orbital-superorbital periods of known disk-fed high-mass X-ray binaries, the orbital period of P13 is roughly estimated as 3–7 days. In this case, an unknown mechanism with a much longer timescale is needed to interpret the phase drift. Further studies on the stability of these two periodicities with a long-term monitoring could help us to probe their physical origins.-
dc.languageeng-
dc.publisherAmerican Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/2041-8205-
dc.relation.ispartofThe Astrophysical Journal Letters-
dc.rightsThe Astrophysical Journal Letters. Copyright © American Astronomical Society.-
dc.titleSwift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13-
dc.typeArticle-
dc.identifier.emailHu, CP: cphu@hku.hk-
dc.identifier.emailNg, SCY: ncy@bohr.physics.hku.hk-
dc.identifier.authorityNg, SCY=rp01706-
dc.description.naturepostprint-
dc.identifier.doi10.3847/2041-8213/835/1/L9-
dc.identifier.hkuros271330-
dc.identifier.volume835-
dc.identifier.issue1-
dc.identifier.spageL9:1-
dc.identifier.epage6-
dc.identifier.isiWOS:000394540500001-
dc.publisher.placeUnited Kingdom-

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