Stamatellos, Dimitris (2015) The migration of gas giant planets in gravitationally unstable disks. The Astrophysical Journal Letters, 810 (L11). p. 5. ISSN 2041-8205
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Official URL: http://dx.doi.org/10.1088/2041-8205/810/1/L11
Planets form in the disks of gas and dust that surround young stars. It is not known whether or not gas giant planets on wide orbits form the same way as Jupiter or form by the fragmentation of gravitationally unstable disks. Here we show that a giant planet that has formed in the outer regions of a protostellar disk initially migrates quickly toward the central star (migration timescale ~104 years) while accreting gas from the disk. However, in contrast with previous studies, we find that the planet eventually opens up a gap in the disk and the migration is essentially halted. At the same time, accretion-powered radiative feedback from the planet significantly limits its mass growth, keeping it within the planetary-mass regime, (i.e., below the deuterium burning limit) at least for the initial stages of disk evolution. Giant planets may therefore be able to survive on wide orbits despite their initial fast inward migration, consequently shaping the environment in which terrestrial planets that may harbor life can form.
|Uncontrolled Keywords (separate with ;):||hydrodynamics; planet–disk interactions; planets and satellites formation; planets and satellites gaseous planets; protoplanetary disks|
|Subjects:||Physical sciences > Astronomy|
|Schools:||Faculty of Science and Technology > School of Physical Sciences and Computing > Jeremiah Horrocks Institute|
|Deposited By:||Nuala Jones|
|Deposited On:||19 Nov 2015 10:56|
|Last Modified:||21 Oct 2016 06:56|
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