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Article: Swift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13
Title | Swift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13 |
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Authors | |
Keywords | accretion, accretion disks galaxies: individual (NGC 7793) stars: neutron X-rays: binaries X-rays: individual (NGC 7793 P13, CXOU J235750.9-323726) |
Issue Date | 2017 |
Publisher | American 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? |
Abstract | NGC 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 Identifier | http://hdl.handle.net/10722/238709 |
ISSN | 2023 Impact Factor: 8.8 2023 SCImago Journal Rankings: 2.766 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Hu, CP | - |
dc.contributor.author | Li, KL | - |
dc.contributor.author | Kong, AKH | - |
dc.contributor.author | Ng, SCY | - |
dc.contributor.author | Lin, LCC | - |
dc.date.accessioned | 2017-02-20T01:25:01Z | - |
dc.date.available | 2017-02-20T01:25:01Z | - |
dc.date.issued | 2017 | - |
dc.identifier.citation | The Astrophysical Journal Letters, 2017, v. 835 n. 1, p. L9:1-6 | - |
dc.identifier.issn | 2041-8205 | - |
dc.identifier.uri | http://hdl.handle.net/10722/238709 | - |
dc.description.abstract | NGC 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.language | eng | - |
dc.publisher | American Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/2041-8205 | - |
dc.relation.ispartof | The Astrophysical Journal Letters | - |
dc.rights | The Astrophysical Journal Letters. Copyright © American Astronomical Society. | - |
dc.subject | accretion, accretion disks | - |
dc.subject | galaxies: individual (NGC 7793) | - |
dc.subject | stars: neutron | - |
dc.subject | X-rays: binaries | - |
dc.subject | X-rays: individual (NGC 7793 P13, CXOU J235750.9-323726) | - |
dc.title | Swift Detection of a 65 Day X-Ray Period from the Ultraluminous Pulsar NGC 7793 P13 | - |
dc.type | Article | - |
dc.identifier.email | Hu, CP: cphu@hku.hk | - |
dc.identifier.email | Ng, SCY: ncy@bohr.physics.hku.hk | - |
dc.identifier.authority | Ng, SCY=rp01706 | - |
dc.description.nature | postprint | - |
dc.identifier.doi | 10.3847/2041-8213/835/1/L9 | - |
dc.identifier.scopus | eid_2-s2.0-85011269764 | - |
dc.identifier.hkuros | 271330 | - |
dc.identifier.volume | 835 | - |
dc.identifier.issue | 1 | - |
dc.identifier.spage | L9:1 | - |
dc.identifier.epage | 6 | - |
dc.identifier.isi | WOS:000394540500001 | - |
dc.publisher.place | United Kingdom | - |
dc.identifier.issnl | 2041-8205 | - |