Migration and giant planet formation

By Y. Alibert, C. Mordasini, W. Benz. 2004

161 citations recorded by the source corpus.

We extend the core-accretion model of giant gaseous planets by Pollack et al. (1996) to include migration, disc evolution and gap formation. Starting with a core of a fraction of an Earth's mass located at 8 AU, we end our simulation with the onset of runaway gas accretion when the planet is at 5.5 AU 1 Myr later. This timescale is about a factor ten shorter than the one found by Pollack et al. (1996) even though the disc was less massive initially and viscously evolving. Other initial conditions can lead to even shorter timescales. The reason for this speed-up is found to result from the fact that a moving planet does not deplete its feeding zone to the extend of a static planet. Thus, the uncomfortably long formation timescale associated with the core-accretion scenario can be considerably reduced and brought in much better agreement with the typical disc lifetimes inferred from observations of young circumstellar discs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bc8d172762692747ae06a06dfc0ff99da6edf028

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Citations in the corpus

Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “Faster type I migration partially neutralizes this need, as it allows growth beyond the isolation mass and up to the critical mass by increasing the embryo’s feeding zone (Alibert et al. 2004).”
Ab Initio Equation of State Data for Hydrogen, Helium, and Water and the Internal Structure of Jupiter (2007, background): “…of S, Si, Mg, and Fe while ice refers to a mixture of C, N, O, and H. Due to the core accretion scenario for the formation process of giant planets (Alibert et al. 2004; Pollack et al. 1996), these elements have mainly entered the planetary interior in the form of icy compounds of CH4, NH3, H2O,…”
Intermediate mass black holes in AGN discs – I. Production and growth (2012, methodology): “This process is analagous to the migration of giant planet cores and their feeding zones in protoplanetary disks (Alibert et al. 2004).”
Formation of Giant Planets (2004, background): “Radial migration of the planet can also alter this picture, since the feeding zone can extend into disk regions undepleted of solids (e.g., Alibert et al. 2004; Hasegawa and Pudritz 2012).”
A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, methodology): “The planets are synthesized using an upgraded version (Mordasini et al. 2012b) of the planet formation model originally presented in Alibert et al. (2004).”
Timescale of mass accretion in pre-main-sequence stars (2009, background): “Giant planet formation is much faster (∼ 3 Myr) if planet migration is included (Alibert et al. 2004, 2005).”
Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities (2004, background): “In this case, phase 2 does not exist either (Alibert et al. 2004).”
Models of giant planet formation with migration and disc evolution (2004, background): “As shown in Alibert et al. (2004), modifications in the outer planet boundary conditions due to the gap formation have a small effect.”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “This would explain how Jupiter a creted a several M⊕ core capable of amassing its atmosph before the solar nebula was eliminated (Pollack et al., 1996 Wuchterl et al., 2000; Inaba et al., 2003; Podolak, 20 Hubickyj et al., 2003; Alibert et al., 2004) .”
Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, background): “Therefore changing from the (strongly reduced) type I to (normal) type II results in a net increase of the migration rate and the planet moves into regions of the disks that have not yet been depleted in planetesimals (Alibert et al. 2004).”
Characterization of exoplanets from their formation - I. Models of combined planet formation and evolution (2012, methodology): “We present multiple upgrades of our formation model (introduced first in Alibert et al. 2004).”
Spitzer Observations of the Orion OB1 Association: Disk Census in the Low-Mass Stars (2007, background): “Giant planets are expected to form in this period (Pollack et al. 1996; Alibert et al. 2004).”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, methodology): “The model has been described in detail in several previous works (Alibert et al. 2004, 2005, Mordasini et al. 2012c) with a recent overview in Mordasini et al. (2015).”
Planet formation and migration (2005, background): “Indeed, it is believed that in order for giant planet formation to occur and to be able to fit the observed distribution of extrasolar planets, type I migration rates obtained for a laminar disk have to be reduced by such processes (e.g., Alibert et al 2004).”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “Later extensions and improvements of the core accretion model, such as the inclusion of planetary migration and concurrent disk evolution (Alibert et al. 2004, 2005a) or the use of modified grain opacities in the envelope (Podolak 2003; Hubickj et al. 2005), showed that the core accretion mechanism…”