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?

"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?

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"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