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dc.contributor.authorSnios, Bradford
dc.contributor.authorWykes, Sarka
dc.contributor.authorNulsen, Paul E. J.
dc.contributor.authorKraft, Ralph P.
dc.contributor.authorMeyer, Eileen T.
dc.contributor.authorBirkinshaw, Mark
dc.contributor.authorWorrall, Diana M.
dc.contributor.authorHardcastle, Martin J.
dc.contributor.authorRoediger, Elke
dc.contributor.authorForman, William R.
dc.contributor.authorJones, Christine
dc.date.accessioned2019-08-01T16:03:40Z
dc.date.available2019-08-01T16:03:40Z
dc.date.issued2019-02-05
dc.identifier.citationSnios , B , Wykes , S , Nulsen , P E J , Kraft , R P , Meyer , E T , Birkinshaw , M , Worrall , D M , Hardcastle , M J , Roediger , E , Forman , W R & Jones , C 2019 , ' Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A ' , The Astrophysical Journal , vol. 871 , no. 2 , 248 . https://doi.org/10.3847/1538-4357/aafaf3
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 16091095
dc.identifier.otherPURE UUID: 7393b355-5d92-4e35-ab30-8dcf3531068b
dc.identifier.otherArXiv: http://arxiv.org/abs/1901.00509v1
dc.identifier.otherScopus: 85062008250
dc.identifier.urihttp://hdl.handle.net/2299/21525
dc.descriptionAccepted to ApJ, 14 pages, 8 figures, 2 tables
dc.description.abstractWe report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 yr, collective proper motion of 11.3 ± 3.3 mas yr -1 , or 0.68 ± 0.20c, is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material.en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectgalaxies: active
dc.subjectgalaxies: individual (Centaurus A)
dc.subjectgalaxies: jets
dc.subjectX-rays: galaxies
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleVariability and Proper Motion of X-ray Knots in the Jet of Centaurus Aen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85062008250&partnerID=8YFLogxK
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/1538-4357/aafaf3
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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