Persistent Link:
http://hdl.handle.net/10150/617417
Title:
The inner cavity of the circumnuclear disc
Author:
Blank, M.; Morris, M. R.; Frank, A.; Carroll-Nellenback, J. J.; Duschl, W. J.
Affiliation:
Univ Arizona, Steward Observ
Issue Date:
2016-06-21
Publisher:
OXFORD UNIV PRESS
Citation:
The inner cavity of the circumnuclear disc 2016, 459 (2):1721 Monthly Notices of the Royal Astronomical Society
Journal:
Monthly Notices of the Royal Astronomical Society
Rights:
© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Collection Information:
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
Abstract:
The circumnuclear disc (CND) orbiting the Galaxy's central black hole is a reservoir of material that can ultimately provide energy through accretion, or form stars in the presence of the black hole, as evidenced by the stellar cluster that is presently located at the CND's centre. In this paper, we report the results of a computational study of the dynamics of the CND. The results lead us to question two paradigms that are prevalent in previous research on the Galactic Centre. The first is that the disc's inner cavity is maintained by the interaction of the central stellar cluster's strong winds with the disc's inner rim, and secondly, that the presence of unstable clumps in the disc implies that the CND is a transient feature. Our simulations show that, in the absence of a magnetic field, the interaction of the wind with the inner disc rim actually leads to a filling of the inner cavity within a few orbital time-scales, contrary to previous expectations. However, including the effects of magnetic fields stabilizes the inner disc rim against rapid inward migration. Furthermore, this interaction causes instabilities that continuously create clumps that are individually unstable against tidal shearing. Thus the occurrence of such unstable clumps does not necessarily mean that the disc is itself a transient phenomenon. The next steps in this investigation are to explore the effect of the magnetorotational instability on the disc evolution and to test whether the results presented here persist for longer time-scales than those considered here.
ISSN:
0035-8711; 1365-2966
DOI:
10.1093/mnras/stw771
Keywords:
accretion; accretion discs; magnetic fields; MHD; Galaxy: centre; Galaxy: nucleus
Version:
Final published version
Sponsors:
Fulbright Commission
Additional Links:
http://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stw771

Full metadata record

DC FieldValue Language
dc.contributor.authorBlank, M.en
dc.contributor.authorMorris, M. R.en
dc.contributor.authorFrank, A.en
dc.contributor.authorCarroll-Nellenback, J. J.en
dc.contributor.authorDuschl, W. J.en
dc.date.accessioned2016-07-23T00:51:58Z-
dc.date.available2016-07-23T00:51:58Z-
dc.date.issued2016-06-21-
dc.identifier.citationThe inner cavity of the circumnuclear disc 2016, 459 (2):1721 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966-
dc.identifier.doi10.1093/mnras/stw771-
dc.identifier.urihttp://hdl.handle.net/10150/617417-
dc.description.abstractThe circumnuclear disc (CND) orbiting the Galaxy's central black hole is a reservoir of material that can ultimately provide energy through accretion, or form stars in the presence of the black hole, as evidenced by the stellar cluster that is presently located at the CND's centre. In this paper, we report the results of a computational study of the dynamics of the CND. The results lead us to question two paradigms that are prevalent in previous research on the Galactic Centre. The first is that the disc's inner cavity is maintained by the interaction of the central stellar cluster's strong winds with the disc's inner rim, and secondly, that the presence of unstable clumps in the disc implies that the CND is a transient feature. Our simulations show that, in the absence of a magnetic field, the interaction of the wind with the inner disc rim actually leads to a filling of the inner cavity within a few orbital time-scales, contrary to previous expectations. However, including the effects of magnetic fields stabilizes the inner disc rim against rapid inward migration. Furthermore, this interaction causes instabilities that continuously create clumps that are individually unstable against tidal shearing. Thus the occurrence of such unstable clumps does not necessarily mean that the disc is itself a transient phenomenon. The next steps in this investigation are to explore the effect of the magnetorotational instability on the disc evolution and to test whether the results presented here persist for longer time-scales than those considered here.en
dc.description.sponsorshipFulbright Commissionen
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttp://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stw771en
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectaccretionen
dc.subjectaccretion discsen
dc.subjectmagnetic fieldsen
dc.subjectMHDen
dc.subjectGalaxy: centreen
dc.subjectGalaxy: nucleusen
dc.titleThe inner cavity of the circumnuclear discen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
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