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        Old pre-main-sequence stars. Disc reformation by Bondi-Hoyle accretion

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        Author
        Scicluna, P.
        Rosotti, G.
        Testi, L.
        Dale, James
        Attention
        2299/19044
        Abstract
        Young stars show evidence of accretion discs which evolve quickly and disperse with an e-folding time of ~3 Myr. This is in striking contrast with recent observations that suggest evidence of numerous >30 Myr old stars with an accretion disc in large star-forming complexes. We consider whether these observations of apparently old accretors could be explained by invoking Bondi-Hoyle accretion to rebuild a new disc around these stars during passage through a clumpy molecular cloud. We combine a simple Monte Carlo model to explore the capture of mass by such systems with a viscous evolution model to infer the levels of accretion that would be observed. We find that a significant fraction of stars may capture enough material via the Bondi-Hoyle mechanism to rebuild a disc of mass ≳1 minimum-mass solar nebula, and ≲10% accrete at observable levels at any given time. A significant fraction of the observed old accretors may be explained with our proposed mechanism. Such accretion may provide a chance for a second epoch of planet formation, and have unpredictable consequences for planetary evolution.
        Publication date
        2014-06-09
        Published in
        Astronomy & Astrophysics
        Published version
        https://doi.org/10.1051/0004-6361/201423654
        Other links
        http://hdl.handle.net/2299/19044
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