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Frequency-dependent time delays for strong outbursts in selected blazars from the MetsÄhovi and UMRAO monitoring data bases – II

dc.contributor.authorPyatunina, T. B.en_US
dc.contributor.authorKudryavtseva, N. A.en_US
dc.contributor.authorGabuzda, D. C.en_US
dc.contributor.authorJorstad, Svetlana G.en_US
dc.contributor.authorAller, Margo F.en_US
dc.contributor.authorAller, Hugh D.en_US
dc.contributor.authorTeräsranta, H.en_US
dc.date.accessioned2010-06-01T19:05:30Z
dc.date.available2010-06-01T19:05:30Z
dc.date.issued2007-10-21en_US
dc.identifier.citationPyatunina, T. B.; Kudryavtseva, N. A.; Gabuzda, D. C.; Jorstad, S. G.; Aller, M. F.; Aller, H. D.; TerÄsranta, H. (2007). "Frequency-dependent time delays for strong outbursts in selected blazars from the MetsÄhovi and UMRAO monitoring data bases – II." Monthly Notices of the Royal Astronomical Society 381(2): 797-808. <http://hdl.handle.net/2027.42/72279>en_US
dc.identifier.issn0035-8711en_US
dc.identifier.issn1365-2966en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/72279
dc.description.abstractWe analyse the radio light curves of the blazars 1308+326, 2223−052 and 2251+158 using University of Michigan Radio Observatory and MetsÄhovi Radio Observatory multifrequency monitoring data combined with high-resolution very long baseline interferometry (VLBI) observations in order to extract the properties of prominent outbursts. The outbursts are classified as ‘core’ and ‘jet’ events according to their behaviour at different frequencies and their associations with features appearing in the VLBI jet. We define the activity cycle for each blazar as the time interval between successive ‘core’ outbursts. The durations of the activity cycle derived in this way are ≥14 yr for 1308+326, ∼12 yr for 2223−052 and 12.4 ± 0.6 yr for 2251+158. We find an unusual frequency dependence for the time profiles for a major flare in 1308+326, which may provide evidence for acceleration or bending of the jet flow in the optically thick part of the emission region. Analysis of these activity cycles, combined with our earlier results, leads us to suggest that more luminous blazars possess shorter activity cycles, consistent with the accretion rates being higher in more powerful sources (relative to the Eddington rate).en_US
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dc.format.extent3109 bytes
dc.format.mimetypeapplication/pdf
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dc.publisherBlackwell Publishing Ltden_US
dc.rights2007 The Authors. Journal compilation © 2007 RASen_US
dc.subject.otherGalaxies: Activeen_US
dc.subject.otherGalaxies: Jetsen_US
dc.subject.otherQuasars: Individual: 1308+326en_US
dc.subject.otherQuasars: Individual: 2223−052 (3C 446)en_US
dc.subject.otherQuasars: Individual: 2251+158 (3C454.3)en_US
dc.titleFrequency-dependent time delays for strong outbursts in selected blazars from the MetsÄhovi and UMRAO monitoring data bases – IIen_US
dc.typeArticleen_US
dc.subject.hlbsecondlevelAstronomyen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.contributor.affiliationumAstronomy Department, University of Michigan, Ann Arbor, MI 48109, USAen_US
dc.contributor.affiliationotherInstitute of Applied Astronomy of the RAS, Zhdanovskaya St 8, 197110, St Petersburg, Russiaen_US
dc.contributor.affiliationotherMax-Plank-Institut fÜr Radioastronomie, Auf dem HÜgel 69, 53121 Bonn, Germanyen_US
dc.contributor.affiliationotherSt Petersburg State University, Universitetskii pr. 28, Petrodvoretz, 198504, St Petersburg, Russiaen_US
dc.contributor.affiliationotherPhysics Department, University College Cork, Cork, Irelanden_US
dc.contributor.affiliationotherInstitute for Astrophysical Research, Boston University, Boston, MA 02215, USAen_US
dc.contributor.affiliationotherMetsÄhovi Radio Observatory, Helsinki University of Technology, Finlanden_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/72279/1/j.1365-2966.2007.12281.x.pdf
dc.identifier.doi10.1111/j.1365-2966.2007.12281.xen_US
dc.identifier.sourceMonthly Notices of the Royal Astronomical Societyen_US
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