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    The global stability of M33: still a puzzle

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    Author
    Sellwood, J A
    Shen, Juntai
    Li, Zhi
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-07
    Keywords
    galaxies: evolution
    galaxies: kinematics and dynamics
    Local Group
    galaxies: spiral
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    J A Sellwood, Juntai Shen, Zhi Li, The global stability of M33: still a puzzle, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 4, July 2019, Pages 4710–4723, https://doi.org/10.1093/mnras/stz1145
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    © 2019 The Author(s) 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 inner disc of the Local Group galaxy M33 appears to be in settled rotational balance, and near-IR images reveal a mild, large-scale, two-arm spiral pattern with no strong bar. We have constructed N-body models that match all the extensive observational data on the kinematics and surface density of stars and gas in the inner part of M33. We rind that currently favoured models are unstable to the formation of a strong bar of semimajor axis 2 less than or similar to a(B) less than or similar to 3 kpc within 1 Gyr, which changes the dynamical properties of the models to become inconsistent with the current, apparently well-settled, state. The formation of a bar is unaffected by how: the gas component is modelled, by increasing the mass of the nuclear star cluster, or by making the dark matter halo counter-rotate, but it can be prevented by either reducing the mass-to-light ratio of the stars to Y-V similar to 0.6 or Y-K similar to 0.23 in solar units or by increasing the random motions of the stars. Also a shorter and weaker bar results when the halo is rigid and unresponsive. However, all three near-stable models support multi-arm spirals, and not the observed largescale hi-symmetric spiral, A two-arm spiral pattern could perhaps be tidally induced, but such a model would require an implausibly low-mass disc to avoid a bar and there is no visible culprit:. Thus the survival of the current state of this exceptionally well-studied galaxy is not yet understood. We also suspect that many other unbarred galaxies present a similar puzzle.
    ISSN
    0035-8711
    EISSN
    1365-2966
    DOI
    10.1093/mnras/stz1145
    Version
    Final published version
    Sponsors
    Chinese Academy of Sciences President's International Fellowship Initiative [2018VMA0051]; NSF [PHY-1748958]; National Key R&D Program of China [2018YFA0404501]; National Natural Science Foundation of China [11773052, 11761131016, 11333003]; China-Chile joint grant from CASSACA; Newton Advanced Fellowship - Royal Society; Newton Fund
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz1145
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    UA Faculty Publications

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