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dc.contributor.authorPlotkin, Richard
dc.contributor.authorMiller-Jones, James
dc.contributor.authorChomiuk, L.
dc.contributor.authorStrader, J.
dc.contributor.authorBruzewski, S.
dc.contributor.authorBundas, A.
dc.contributor.authorSmith, K.R.
dc.contributor.authorRuan, J.J.
dc.date.accessioned2020-07-22T13:54:31Z
dc.date.available2020-07-22T13:54:31Z
dc.date.issued2019
dc.identifier.citationPlotkin, R.M. and Miller-Jones, J.C.A. and Chomiuk, L. and Strader, J. and Bruzewski, S. and Bundas, A. and Smith, K.R. et al. 2019. Radio Variability from a Quiescent Stellar-mass Black Hole Jet. Astrophysical Journal. 874 (1): ARTN 13.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/80173
dc.identifier.doi10.3847/1538-4357/ab01cc
dc.description.abstract

© 2019 The American Astronomical Society. All rights reserved. Relativistic outflows are believed to be a common feature of black hole X-ray binaries (BHXBs) at the lowest accretion rates, when they are in their "quiescent" spectral state. However, we still lack a detailed understanding of how quiescent jet emission varies with time. Here we present 24 yr of archival radio observations (from the Very Large Array and the Very Long Baseline Array) of the BHXB V404 Cygni in quiescence (totaling 150 observations from 1.4 to 22 GHz). The observed flux densities follow lognormal distributions with means and standard deviations of (logf v ,σ log f v ) = (-0.53, 0.19) and (-0.53, 0.30) at 4.9 and 8.4 GHz, respectively (where f v is the flux density in units of mJy). As expected, the average radio spectrum is flat with a mean and standard deviation of (α r σ αr ) (0.02, 0.65), where f v ∝ v αr . We find that radio flares that increase the flux density by factors of 2-4 over timescales as short as <10 minutes are commonplace, and that long-term variations (over 10-4000 day timescales) are consistent with shot-noise impulses that decay to stochastic variations on timescales ∼10 days (and perhaps as short as tens of minutes to several hr). We briefly compare the variability characteristics of V404 Cygni to jetted active galactic nuclei, and we conclude with recommendations on how to account for variability when placing quiescent BHXB candidates with radio luminosities comparable to V404 Cygni (LR ≈ 10 28 erg s -1 ) onto the radio/X-ray luminosity plane.

dc.languageEnglish
dc.publisherIOP PUBLISHING LTD
dc.relation.sponsoredbyhttp://purl.org/au-research/grants/arc/FT140101082
dc.subjectScience & Technology
dc.subjectPhysical Sciences
dc.subjectAstronomy & Astrophysics
dc.subjectaccretion, accretion disks
dc.subjectstars: black holes
dc.subjectstars: individual (V404 Cygni)
dc.subjectX-rays: binaries
dc.subjectX-RAY BINARIES
dc.subjectACTIVE GALACTIC NUCLEI
dc.subjectNOVA V404 CYGNI
dc.subjectNEUTRON-STAR
dc.subjectLIGHT CURVES
dc.subjectRELATIVISTIC JETS
dc.subjectFLUX CORRELATION
dc.subjectACCRETION FLOWS
dc.subjectCOMPLETE SAMPLE
dc.subjectXTE J1550-564
dc.titleRadio Variability from a Quiescent Stellar-mass Black Hole Jet
dc.typeJournal Article
dcterms.source.volume874
dcterms.source.number1
dcterms.source.issn0004-637X
dcterms.source.titleAstrophysical Journal
dc.date.updated2020-07-22T13:54:30Z
curtin.note

Copyright © 2019 The American Astronomical Society. All rights reserved.

curtin.departmentSchool of Elec Eng, Comp and Math Sci (EECMS)
curtin.accessStatusOpen access
curtin.facultyFaculty of Science and Engineering
curtin.contributor.orcidMiller-Jones, James [0000-0003-3124-2814]
curtin.contributor.researcheridMiller-Jones, James [B-2411-2013]
curtin.identifier.article-numberARTN 13
dcterms.source.eissn1538-4357
curtin.contributor.scopusauthoridPlotkin, Richard [13205184900]
curtin.contributor.scopusauthoridMiller-Jones, James [10044231400]


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