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dc.contributor.authorPerlman, Eric S.
dc.contributor.authorGodfrey, L.E.H.
dc.contributor.authorLovell, J.E.J.
dc.contributor.authorBurke-Spolaor, S.
dc.contributor.authorEkers, R.
dc.contributor.authorBicknell, G.V.
dc.contributor.authorBirkinshaw, M.
dc.contributor.authorWorrall, D.M.
dc.contributor.authorJauncey, D.L.
dc.contributor.authorSchwartz, D.A.
dc.date.accessioned2013-08-06T12:25:00Z
dc.date.available2013-08-06T12:25:00Z
dc.date.issued2012-10-20
dc.identifier.citationGodfrey, L. E. H., Lovell, J. E. J., Burke-Spolaor, S., Ekers, R., Bicknell, G. V., Birkinshaw, M., ... & Georganopoulos, M. (2012). Periodic Structure in the Megaparsec-scale Jet of PKS 0637–752. The Astrophysical Journal Letters, 758(2), L27.en_US
dc.identifier.urihttp://hdl.handle.net/11141/65
dc.description.abstractWe present 18 GHz Australia Telescope Compact Array imaging of the megaparsec-scale quasar jet PKS 0637–752 with angular resolution ~0farcs58. We draw attention to a spectacular train of quasi-periodic knots along the inner 11'' of the jet, with average separation ~1.1 arcsec (7.6 kpc projected). We consider two classes of model to explain the periodic knots: those that involve a static pattern through which the jet plasma travels (e.g., stationary shocks) and those that involve modulation of the jet engine. Interpreting the knots as re-confinement shocks implies the jet kinetic power Q jet ~ 1046 erg s–1, but the constant knot separation along the jet is not expected in a realistic external density profile. For models involving modulation of the jet engine, we find that the required modulation period is 2 × 103 yr < τ < 3 × 105 yr. The lower end of this range is applicable if the jet remains highly relativistic on kiloparsec scales, as implied by the IC/CMB model of jet X-ray emission. We suggest that the periodic jet structure in PKS 0637–752 may be analogous to the quasi-periodic jet modulation seen in the microquasar GRS 1915+105, believed to result from limit cycle behavior in an unstable accretion disk. If variations in the accretion rate are driven by a binary black hole, the predicted orbital radius is 0.7 pc lsim a lsim 30 pc, which corresponds to a maximum angular separation of ~0.1-5 mas.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titlePeriodic structure in the megaparsec-scale jet of pks 0637-752en_US
dc.typeArticleen_US
dc.identifier.doi10.1088/2041-8205/758/2/L27


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