Gravitational Capture of Large Interstellar Planetesimals by Collapsing Prestellar Cores
Auteurs : Richard Anderson, Kedron Silsbee
Résumé scientifique
We investigate the capture of free-floating planetesimals by the time-varying gravitational potential of a collapsing prestellar core. We use one-dimensional collapse models to estimate the volume of space from which planetesimals are captured. We combine this calculation with an estimate of the size distribution and velocity dispersion of the free-floating planetesimal population to determine the largest planetesimal that is typically captured, as well as the total mass of all planetesimals captured by a given protostar. We consider two cases: one in which the free-floating planetesimal population comes from the birth cluster of the star, and one in which the planetesimals are captured from the Galactic population of free-floating planetesimals. We find that the details of the collapse matter substantially, with the predicted diameter of the largest captured body from the Galactic population ranging from $2.8$ km to $6.4$ km depending on collapse model, and the largest body from our model birth cluster environment ranging from $70$ km to $1200$ km, for assumed velocity dispersions ranging from 0.7 to 8.5 km/s. The total solid mass captured by this mechanism does not exceed 0.07 Earth masses in all cases. We discuss the effect of these captured objects on the planet formation process, and argue that while the total solid mass captured is likely not significant, the largest captured bodies may grow to planet size via accretion of pebbles present in their host disks. This process may accelerate planet formation, or enable it in disks that have difficulty in forming their own planetesimals.
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Résumé scientifique
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Résumé scientifique
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Résumé scientifique
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Résumé scientifique
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Résumé scientifique
The observed lifetimes of gaseous protoplanetary discs place strong constraints on gas and ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid core responsible for the attraction of the gaseous envelope has to form before gas dissipation in the protoplanetary disc is completed within 1–10 million years. Building up the core by collisions between km-sized planetesimals fails to meet this timescale constraint, especially at wide stellar separations. Nonetheless, gas-giant planets are detected by direct imaging at wide orbital distances. In this paper, we numerically study the growth of cores by the accretion of cm-sized pebbles loosely coupled to the gas. …
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En bref
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Résumé scientifique
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Résumé scientifique
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Les travaux antérieurs sur lesquels il s’appuie
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Résumé scientifique
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Résumé scientifique
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Résumé scientifique
Context. For up to a few millions of years, pebbles must provide a quasi-steady inflow of solids from the outer parts of protoplanetary disks to their inner regions. Aims. We wish to understand how a significant fraction of the pebbles grows into planetesimals instead of being lost to the host star. Methods. We examined analytically how the inward flow of pebbles is affected by the snow line and under which conditions dust-rich (rocky) planetesimals form. When calculating the inward drift of solids that is due to gas drag, we included the back-reaction of the gas to the motion of the solids. Results. We show that in low-viscosity protoplanetary disks (with a monotonous surface density simila…
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