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Questions about formation of planetary systems
I understand there are presently two models for the formation of gas giants:
Core Accretion, in which a 10 Earth-mass rocky core forms first, and then attracts hydrogen and helium from the protoplanetary disk. Disk Instability, in which regions of the protoplanetary disk collapse on themselves to form gas giants without rocky cores having to form first. Presumably a lot of computer simulation has been done: Are the number, masses, and orbits of gas giants different from one model to the other, and does this affect the predicted number, type and orbits of terrestrial planets? |
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Questions about formation of planetary systems
"RS" == Roger Stokes writes:
RS I understand there are presently two models for the formation of RS gas giants: Core Accretion, in which a 10 Earth-mass rocky core RS forms first, and then attracts hydrogen and helium from the RS protoplanetary disk. RS Disk Instability, in which regions of the protoplanetary disk RS collapse on themselves to form gas giants without rocky cores RS having to form first. RS Presumably a lot of computer simulation has been done: Are the RS number, masses, and orbits of gas giants different from one model RS to the other, and does this affect the predicted number, type and RS orbits of terrestrial planets? Alan Boss has done a lot of work in this area, e.g., URL: http://adsabs.harvard.edu/cgi-bin/np...AS...202.2402B . As I understand it, the primary driver for the disk instability model is the timescale for formation of a giant planet. Are disks long-lived enough that giant planets form via core accretion? -- Lt. Lazio, HTML police | e-mail: No means no, stop rape. | http://patriot.net/%7Ejlazio/ sci.astro FAQ at http://sciastro.astronomy.net/sci.astro.html |
#3
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Questions about formation of planetary systems
"RS" == Roger Stokes writes:
RS I understand there are presently two models for the formation of RS gas giants: Core Accretion, in which a 10 Earth-mass rocky core RS forms first, and then attracts hydrogen and helium from the RS protoplanetary disk. RS Disk Instability, in which regions of the protoplanetary disk RS collapse on themselves to form gas giants without rocky cores RS having to form first. RS Presumably a lot of computer simulation has been done: Are the RS number, masses, and orbits of gas giants different from one model RS to the other, and does this affect the predicted number, type and RS orbits of terrestrial planets? Alan Boss has done a lot of work in this area, e.g., URL: http://adsabs.harvard.edu/cgi-bin/np...AS...202.2402B . As I understand it, the primary driver for the disk instability model is the timescale for formation of a giant planet. Are disks long-lived enough that giant planets form via core accretion? -- Lt. Lazio, HTML police | e-mail: No means no, stop rape. | http://patriot.net/%7Ejlazio/ sci.astro FAQ at http://sciastro.astronomy.net/sci.astro.html |
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