TY - GEN
T1 - Planetesimal capture by an evolving giant gaseous protoplanet
AU - Podolak, Morris
AU - Haghighipour, Nader
PY - 2012/8
Y1 - 2012/8
N2 - Both the core-accretion and disk-instability models suggest that at the last stage of the formation of a gas-giant, the core of this object is surrounded by an extended gaseous envelope. At this stage, while the envelope is contracting, planetesimals from the protoplanetary disk may be scattered into the protoplanets atmosphere and deposit some or all of their materials as they interact with the gas. We have carried out extensive simulations of approximately 104 planetesimals interacting with a envelope of a Jupiter-mass protoplanet including effects of gas drag, heating, and the effect of the protoplanets extended mass distribution. Simulations have been carried out for different radii and compositions of planetesimals so that all three processes occur to different degrees. We present the results of our simulations and discuss their implications for the enrichment of ices in giant planets. We also present statistics for the probability of capture (i.e. total mass-deposition) of planetesimals as a function of their size, composition, and closest approach to the center of the protoplanetary body.
AB - Both the core-accretion and disk-instability models suggest that at the last stage of the formation of a gas-giant, the core of this object is surrounded by an extended gaseous envelope. At this stage, while the envelope is contracting, planetesimals from the protoplanetary disk may be scattered into the protoplanets atmosphere and deposit some or all of their materials as they interact with the gas. We have carried out extensive simulations of approximately 104 planetesimals interacting with a envelope of a Jupiter-mass protoplanet including effects of gas drag, heating, and the effect of the protoplanets extended mass distribution. Simulations have been carried out for different radii and compositions of planetesimals so that all three processes occur to different degrees. We present the results of our simulations and discuss their implications for the enrichment of ices in giant planets. We also present statistics for the probability of capture (i.e. total mass-deposition) of planetesimals as a function of their size, composition, and closest approach to the center of the protoplanetary body.
KW - methods: n-body simulations
KW - planets and satellites: formation
KW - solar system: formation
UR - http://www.scopus.com/inward/record.url?scp=84899819606&partnerID=8YFLogxK
U2 - 10.1017/S1743921313012957
DO - 10.1017/S1743921313012957
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AN - SCOPUS:84899819606
SN - 9781107033825
T3 - Proceedings of the International Astronomical Union
SP - 263
EP - 269
BT - Formation, Detection, and Characterization of Extrasolar Habitable Planets
PB - Cambridge University Press
ER -