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dc.contributor.authorPunsly, Brian
dc.contributor.authorHardcastle, Martin
dc.contributor.authorHada, Kazuhiro
dc.date.accessioned2018-07-05T16:03:22Z
dc.date.available2018-07-05T16:03:22Z
dc.date.issued2018-06-22
dc.identifier.citationPunsly , B , Hardcastle , M & Hada , K 2018 , ' A New Solution to the Plasma Starved Event Horizon Magnetosphere: Application to the Forked Jet in M87 ' , Astronomy & Astrophysics , vol. 614 , A104 . https://doi.org/10.1051/0004-6361/201732215
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 13209679
dc.identifier.otherPURE UUID: 2798af2a-3f42-4f0b-98a4-2828f9d31ec5
dc.identifier.otherArXiv: http://arxiv.org/abs/1801.03541v1
dc.identifier.otherScopus: 85049586670
dc.identifier.urihttp://hdl.handle.net/2299/20268
dc.description© 2018 ESO. Reproduced with permission from Astronomy & Astrophysics. Content in the UH Research Archive is made available for personal research, educational, and non-commercial purposes only. Unless otherwise stated, all content is protected by copyright, and in the absence of an open license, permissions for further re-use should be sought from the publisher, the author, or other copyright holder.
dc.description.abstractVery Long Baseline Interferometry observations at 86 GHz reveal an almost hollow jet in M87 with a forked morphology. The detailed analysis presented here indicates that the spectral luminosity of the central spine of the jet in M87 is a few percent of that of the surrounding hollow jet 200-400 μ as from the central black hole. Furthermore, recent jet models indicate that a hollow "tubular" jet can explain a wide range of plausible broadband spectra originating from jetted plasma located within ~30 μ as of the central black hole, including the 230 GHz correlated flux detected by the Event Horizon Telescope. Most importantly, these hollow jets from the inner accretion flow have an intrinsic power capable of energizing the global jet out to kiloparsec scales. Thus motivated, this paper considers new models of the event horizon magnetosphere (EHM) in low luminosity accretion systems. Contrary to some models, the spine is not an invisible powerful jet. It is an intrinsically weak jet. In the new EHM solution, the accreted poloidal magnetic flux is weak and the background photon field is weak. It is shown how this accretion scenario naturally results in the dissipation of the accreted poloidal magnetic flux in the EHM not the accumulation of poloidal flux required for a powerful jet. The new solution indicates less large scale poloidal magnetic flux (and jet power) in the EHM than in the surrounding accretion flow and cannot support significant EHM driven jets.en
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectAccretion, accretion disks
dc.subjectBlack hole physics
dc.subjectGalaxies: active
dc.subjectGalaxies: jets
dc.subjectQuasars: general
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleA New Solution to the Plasma Starved Event Horizon Magnetosphere: Application to the Forked Jet in M87en
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=85049586670&partnerID=8YFLogxK
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201732215
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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