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dc.contributor.authorReynolds, C.
dc.contributor.authorPunsly, B.
dc.contributor.authorMiniutti, G.
dc.contributor.authorO'Dea, C.
dc.contributor.authorHurley-Walker, Natasha
dc.date.accessioned2017-04-28T13:56:55Z
dc.date.available2017-04-28T13:56:55Z
dc.date.created2017-04-28T09:06:08Z
dc.date.issued2017
dc.identifier.citationReynolds, C. and Punsly, B. and Miniutti, G. and O'Dea, C. and Hurley-Walker, N. 2017. The Relativistic Jet-accretion Flow-wind Connection in Mrk 231. Astrophysical Journal. 836: 155.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/51936
dc.identifier.doi10.3847/1538-4357/836/2/155
dc.description.abstract

Long-term radio monitoring of the broad absorption line (BAL) quasar Mrk 231 at 17.6 GHz detected a strong flare in 2015. This triggered four epochs of Very Long Baseline Array (VLBA) observations from 8.4 to 43 GHz as well as three epochs of X-ray observations with NuSTAR and two with XMM over a 15 week period. Two ejected components were detected by the VLBA observations. A conservative lower bound on the apparent speed of the first ejection is attained by assuming that it was ejected when the flare began, v app > 3.15c. Serendipitous far-UV Hubble Space Telescope observations combined with our long-term radio monitoring seem to indicate that episodes of relativistic ejections suppress flux that is emitted at wavelengths shortward of the peak of the far-UV spectral energy distribution, similar to what has been observed in radio-loud quasars. Episodes of strong jet production also seem to suppress the high-ionization BAL wind seen in weak jet states. We found a statistically significant increase (~25%) of the 3-12 keV flux during the radio flare relative to a quiescent radio state. This is explained by an ultra-fast (~0.06c) X-ray-absorbing photoionized wind that is significantly detected only in the low-radio state (similar to Galactic black holes). Mrk 231 is becoming more radio loud. We found that the putative parsec-scale radio lobe doubled in brightness in nine years. Furthermore, large flares are more frequent, with three major flares occurring at ~2 year intervals.

dc.publisherInstitute of Physics Publishing
dc.titleThe Relativistic Jet-accretion Flow-wind Connection in Mrk 231
dc.typeJournal Article
dcterms.source.volume836
dcterms.source.number2
dcterms.source.issn0004-637X
dcterms.source.titleAstrophysical Journal
curtin.note

Copyright © 2017 The American Astronomical Society. All rights reserved

curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusOpen access


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