1. RRI Digital Repository
  2. 04. Astronomy and Astrophysics
  3. Research Papers (A&A)
Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6999
Full metadata record
DC FieldValueLanguage
dc.contributor.authorFurst, F-
dc.contributor.authorWalton, D.J.-
dc.contributor.authorHeida, M-
dc.contributor.authorHarrison, F.A.-
dc.contributor.authorBarret, D-
dc.contributor.authorBrightman, M-
dc.contributor.authorFabian, A C-
dc.contributor.authorMiddleton, M J-
dc.contributor.authorPinto, C-
dc.contributor.authorRana, V-
dc.contributor.authorTramper, F-
dc.contributor.authorWebb, N-
dc.contributor.authorKretschmar, P-
dc.date.accessioned2018-09-18T15:02:34Z-
dc.date.available2018-09-18T15:02:34Z-
dc.date.issued2018-08-
dc.identifier.citationAstronomy & Astrophysics, 2018, Vol.616, p A186en_US
dc.identifier.issn0004-6361-
dc.identifier.issn1432-0746 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/6999-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractWe present a timing analysis of multiple XMM-Newton and NuSTAR observations of the ultra-luminous pulsar NGC 7793 P13 spread over its 65 d variability period. We use the measured pulse periods to determine the orbital ephemeris, confirm a long orbital period with Porb = 63.9+0.5−0.6 d, and find an eccentricity of e ≤ 0.15. The orbital signature is imprinted on top of a secular spin-up, which seems to get faster as the source becomes brighter. We also analyze data from dense monitoring of the source with Swift and find an optical photometric period of 63.9 ± 0.5 d and an X-ray flux period of 66.8 ± 0.4 d. The optical period is consistent with the orbital period, while the X-ray flux period is significantly longer. We discuss possible reasons for this discrepancy, which could be due to a super-orbital period caused by a precessing accretion disk or an orbital resonance. We put the orbital period of P13 into context with the orbital periods implied for two other ultra-luminous pulsars, M82 X-2 and NGC 5907 ULX, and discuss possible implications for the system parameters.en_US
dc.language.isoenen_US
dc.publisherEDP Sciences for European Southern Observatoryen_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2018A%26A...616A.186Fen_US
dc.relation.urihttps://arxiv.org/abs/1805.05336en_US
dc.relation.urihttps://doi.org/10.1051/0004-6361/201833292en_US
dc.rights2018 European Southern Observatoryen_US
dc.subjectstarsen_US
dc.subjectneutron / X-raysen_US
dc.subjectbinaries / techniquesen_US
dc.subjectradial velocities / accretion / accretion disks / pulsarsen_US
dc.subjectindividualen_US
dc.subjectNGC 7793 P13en_US
dc.titleA tale of two periods: determination of the orbital ephemeris of the super-Eddington pulsar NGC 7793 P13en_US
dc.typeArticleen_US
Appears in Collections:Research Papers (A&A)

Files in This Item:
File Description SizeFormat 
2018_Astronomy and Astrophsics_Vol.616_pA186.pdfRestricted Access1.01 MBAdobe PDFView/Open
2018_Astronomy and Astrophsics_Vol.616_pA186.epubRestricted Access5.35 MBEPUBView/Open
Show simple item record


Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.