Giant planet formation from disk instability; cooling and heating
| dc.creator | Mayer, Lucio | |
| dc.creator | Wadsley, James | |
| dc.creator | Quinn, Thomas | |
| dc.creator | Stadel, Joachim | |
| dc.date | 2003-11-03 | |
| dc.date | 2003-11-03 | |
| dc.date.accessioned | 2026-07-07T02:11:01Z | |
| dc.date.available | 2026-07-07T02:11:01Z | |
| dc.description | We present the results of high resolution SPH simulations of the evolution of gravitationally unstable protoplanetary disks. We report on calculations in which the disk is evolved using a locally isothermal or adiabatic equation of state (with shock heating), and also on new simulations in which cooling and heating by radiation are explicitly modeled. We find that disks with a minimum Toomre parameter $< 1.4$ fragment into several gravitationally bound protoplanets with masses from below to a few Jupiter masses. This is confirmed also in runs where the disk is given a quiet start, growing gradually in mass over several orbital times. A cooling time comparable to the orbital time is needed to achieve fragmentation, for disk masses in the range $0.08-0.1 M_{\odot}$. After about 30 orbital times, merging between the bound condensations always leads to 2-3 protoplanets on quite eccentric orbits. | |
| dc.description | 8 pages, 2 figures, to appear in the proceedings of the XIXth IAP colloquium "Extrasolar Planets: Today and Tomorrow" held in Paris, France, 2003, June 30 -- July 4, ASP Conf. Series. Images and movies of the simulations can be found at http://www.astro.washington.edu/mayer | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0311048 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0311048 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/6937 | |
| dc.subject | Astrophysics | |
| dc.title | Giant planet formation from disk instability; cooling and heating | |
| dc.type | text |