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Inviscid and viscous flow past embedded planets: implications for planet formation

Published online by Cambridge University Press:  06 January 2014

Chris W. Ormel  and
Ji-Ming Shi
Chris W. Ormel
Affiliation:
Astronomy Department, University of California, Berkeley Berkeley CA 94720 email: [email protected], [email protected]
Ji-Ming Shi
Affiliation:
Astronomy Department, University of California, Berkeley Berkeley CA 94720 email: [email protected], [email protected]
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Abstract

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We have investigated the flow pattern that arises past (proto)planets embedded in the nebula disk during its formation. We consider the regime where the planet mass is large enough to gravitationally perturb the gas (≳0.01 Earth masses), but not too large to open a gap or accrete unlimited amounts of gas from the disk. We consider both inviscid and viscid flows and aim to understand the flow pattern on the scales of the Bondi radius. Having described the flow pattern of the gas, we integrate trajectories of small, solid particles. In agreement with previous findings, we show that the ensuing accretion rates can be high—although, due to radial drift motions, pebble accretion is not necessarily an efficient mechanism.

Keywords

hydrodynamics – methods: analytical – planets and satellites: formation – protoplanetary discs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 173 - 174
Copyright
Copyright © International Astronomical Union 2013 

References

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