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    Limits on planet formation around young pulsars and implications for supernova fallback disks

    Access Status
    Open access via publisher
    Authors
    Kerr, M.
    Johnston, S.
    Hobbs, G.
    Shannon, Ryan
    Date
    2015
    Type
    Journal Article
    
    Metadata
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    Citation
    Kerr, M. and Johnston, S. and Hobbs, G. and Shannon, R. 2015. Limits on planet formation around young pulsars and implications for supernova fallback disks. Astrophysical Journal Letters. 809 (1): pp.1-5.
    Source Title
    Astrophysical Journal Letters
    DOI
    10.1088/2041-8205/809/1/L11
    ISSN
    2041-8205
    School
    Curtin Institute of Radio Astronomy (Physics)
    URI
    http://hdl.handle.net/20.500.11937/36154
    Collection
    • Curtin Research Publications
    Abstract

    We have searched a sample of 151 young, energetic pulsars for periodic variation in pulse time-of-arrival arising from the influence of planetary companions. We are sensitive to objects with masses two orders of magnitude lower than those detectable with optical transit timing, but we find no compelling evidence for pulsar planets. For the older pulsars most likely to host planets, we can rule out Mercury analogs in one third of our sample and planets with masses >0.4 M⨁ and periods ${P}_{b}\lt 1$ year in all but 5% of such systems. If pulsar planets form primarily from supernova fallback disks, these limits imply that such disks do not form, are confined to <0.1 AU radii, are disrupted, or form planets more slowly (>2 Myr) than their protoplanetary counterparts.

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