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J/ApJ/786/33 Simulations of the late stage of planet formation (Quintana+, 2014)

The effect of planets beyond the ice line on the accretion of volatiles by habitable-zone rocky planets. Quintana E.V., Lissauer J.J. <Astrophys. J., 786, 33 (2014)> =2014ApJ...786...33Q (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Models, evolutionary ; Stars, double and multiple Keywords: astrobiology - planets and satellites: composition - planets and satellites: dynamical evolution and stability - planets and satellites: formation - planets and satellites: terrestrial planets - Abstract: Models of planet formation have shown that giant planets have a large impact on the number, masses, and orbits of terrestrial planets that form. In addition, they play an important role in delivering volatiles from material that formed exterior to the snow line (the region in the disk beyond which water ice can condense) to the inner region of the disk where terrestrial planets can maintain liquid water on their surfaces. We present simulations of the late stages of terrestrial planet formation from a disk of protoplanets around a solar-type star and we include a massive planet (from 1 M{earth} to 1 MJ) in Jupiter's orbit at ∼5.2 AU in all but one set of simulations. Two initial disk models are examined with the same mass distribution and total initial water content, but with different distributions of water content. We compare the accretion rates and final water mass fraction of the planets that form. Remarkably, all of the planets that formed in our simulations without giant planets were water-rich, showing that giant planet companions are not required to deliver volatiles to terrestrial planets in the habitable zone. In contrast, an outer planet at least several times the mass of Earth may be needed to clear distant regions of debris truncating the epoch of frequent large impacts. Observations of exoplanets from radial velocity surveys suggest that outer Jupiter-like planets may be scarce, therefore, the results presented here suggest that there may be more habitable planets residing in our galaxy than previously thought. Description: Chambers (2001Icar..152..205C) found that numerical simulations of the final phases of terrestrial planet growth, which began with a bimodal mass distribution consisting of many Mars-sized embryos embedded in a disk of Moon-sized planetesimals, yielded configurations similar to the inner solar system in many respects. Our simulations begin at this epoch and we follow the evolution of embryos and planetesimals (with a 1:10 mass ratio) as they collide and form into terrestrial planets. Outer planets, if included, are assumed to have already formed. Our model begins with a total disk mass of 4.85 M{earth} and is composed of 26 embryos, each with an initial mass of 0.0933 M{earth} (2.8x10-7 M{earth}) and 260 planetesimals of mass 0.00933 M{earth} (2.8x10-8 M{earth}). All bodies are assumed to have a density of 3 g/cm3. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 35 6407 Final Planets and the Embryos/Planetesimals Each Accreted
See also: J/ApJ/770/90 : Candidate planets in the habitable zones (Gaidos, 2013) J/AJ/151/59 : Catalog of Earth-Like Exoplanet Survey Targets (Chandler+, 2016) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Run Simulation run identifier 10- 14 A5 --- Planet Final planet identifier (EMNN; PLNNN) 16- 20 A5 --- Comp Embryo or planetesimal indentifier (EMNN; PLNNN) 22- 27 F6.4 Mgeo Mass Mass 29- 35 F7.4 AU a Semi-major axis
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 20-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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