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2013MNRAS.431.1432N - Mon. Not. R. Astron. Soc., 431, 1432-1438 (2013/May-2)
Hydrogen-losing planets in transition discs around young protostars.
NAYAKSHIN S.
Abstract (from CDS):
Here, we explore another observational implication of the TD hypothesis: dust poor inner accretion flows, which we believe may be relevant to some of the observed millimetre-bright transitional discs around protostars. In our model, a massive protoplanet interrupts the flow of the outer dust-rich disc on its protostar, and at the same time loses a part of its dust-poor envelope into the inner disc. This then powers the observed gas-but-no-dust accretion on to the star. Upon a more detailed investigation, we find that this scenario is quite natural for young massive discs but is less so for older discs, e.g., those whose self-gravitating phase has terminated a fraction of a Myr or more ago. This stems from the fact that TD protoplanets of such an age should have contracted significantly, and so are unlikely to lose much mass. Therefore, we conclude that either (i) the population of `transition discs' with large holes and dust-poor accretion is much younger than generally believed, or (ii) there is a poorly understood stage for late removal of dust-poor envelopes from TD planets; (iii) another explanation for the observations is correct.
Abstract Copyright: © 2013 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)
Journal keyword(s): planets and satellites: formation - planet-disc interactions - protoplanetary discs - stars: formation
Simbad objects: 2
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