Models of giant planet formation with migration and disc evolution

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

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We present a new model of giant planet formation that extends the core-accretion model of Pollack et al. (1996, Icarus, 124, 62) to include migration, disc evolution and gap formation. We show that taking these effects into account can lead to much more rapid formation of giant planets, making it compatible with the typical disc lifetimes inferred from observations of young circumstellar discs. This speed up is due to the fact that migration prevents the severe depletion of the feeding zone as observed in in situ calculations. Hence, the growing planet is never isolated and it can reach cross-over mass on a much shorter timescale. To illustrate the range of planets that can form in our model, we describe a set of simulations in which we have varied some of the initial parameters and compare the final masses and semi-major axes with those inferred from observed extra-solar planets.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e365ae31ce98215bb65920a932c39ef21522ca02

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Citations in the corpus

Transiting exoplanets from the CoRoT space mission . VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert (2008, background): “Recent improvements of the core-accretion models predict the formation of a wide variety of giant planets (Alibert et al. 2005) with masses up to 10 MJup, depending on the initial conditions.”
Models of Jupiter's growth incorporating thermal and hydrodynamic constraints (2008, background): “…migration is extreme in the sense that the isolation mass of a core within a planetesimal disk is larger for any non-zero migration of the planet, because the radial motion of the planet brings it into regions of the disk that are undepleted of planetesimals (Lissauer 1993; Alibert et al. 2005a).”
Close-in planetesimal formation by pile-up of drifting pebbles (2016, methodology): “Our approach combines semianalytical models of viscous protoplanetary disc evolution that follows the work of Alibert et al. (2005, 2013), dust evolution model based on the approach proposed by Birnstiel et al. (2012), and planetesimal formation via the streaming instability similar to Dra̧żkowska…”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “…planetesimal accretion scenario the accretion of solids continues during the envelope contraction phase (Pollack et al. 1996), and may continue subsequently until the planet’s feeding zone becomes depleted in planetesimals (e.g Alibert et al. 2005), possibly leading to highly enriched atmospheres.”
Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager (2015, unknown): “51 Eri b is close enough to the star that this may be less of a problem, and the addition of migration ( 43 ) or pebbles that experience gas drag ( 44 ) also help overcome this timescale difficulty.”
NEAR-INFRARED SPECTROSCOPY OF THE EXTRASOLAR PLANET HR 8799 b (2010, background): “Giant planets formed through core accretion (Pollack et al. 1996; Alibert et al. 2005a) are generally predicted to have metal-rich atmospheres as a result of planetesimal accretion, the accretion of metal-rich gas, and/or core erosion (Alibert et al. 2005b; Guillot & Hueso 2006; Mousis et al. 2009;…”
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).”
Compositional Imprints in Density–Distance–Time: A Rocky Composition for Close-in Low-mass Exoplanets from the Location of the Valley of Evaporation (2017, methodology): “In all calculations, we set the start of the planetary evolution stage at 10 Myr, because nearly all protoplanetary gas disks have disappeared at about 8 Myr in our planetary formation model (Alibert et al. 2005; Mordasini et al. 2012a,b, 2015).”
Direct Imaging and Spectroscopy of a Planetary-Mass Candidate Companion to a Young Solar Analog (2008, background): “On the other hand, at smaller separations this mechanism could build a∼5 MJupiter planet in 1–5 Myr (Pollack et al. 1996; Alibert et al. 2005), which might then migrate outwards through interactions with a disk or other massive planets (either can be quite rapid; Pepliński et al. 2008; Veras &…”
On the Luminosity of Young Jupiters (2006, unknown): “Baraffe et al. (2006) investigated the evolution of planets with core sizes and heavy element abundances derived from the core accretion models of Alibert et al. (2005).”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, methodology): “The disk model yields for example the outer boundary conditions for the structure equations, the radial slopes of the temperature and surface density for the migration model, or the gas accretion rate in the runaway phase (cf. Alibert et al. 2005 and Paper I).”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…spatial distribution of densities and temperatures; Andrews et al. 2009, 2010; Isella et al. 2009, 2010) and predicts the key characteristics of the exoplanet population (e.g., masses, orbital architectures, atmosphere compositions; Ida & Lin 2004, 2008; Alibert et al. 2005; Mordasini et al. 2009).”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, background): “…Astronomy and Space Physics, Uppsala University, Box 515, 751 20 Uppsala, Sweden yond the “snow line” and migrate inward on a time scale that competes with the lifetime of the protoplanetary disk (Thommes et al. 2008; Ida & Lin 2008; Rice & Armitage 2005; Alibert et al. 2005; Trilling et al. 2002).”
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).”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “…masses, f(Md), has been invoked as a key factor in accounting for the diverse demographic properties of the exoplanets (e.g., Ida & Lin 2004, 2008; Alibert et al. 2005; Mordasini et al. 2009), and scaling trends between Md and other star/disk properties are speculated to generate some of the…”
PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, methodology): “Herein, we simulate the thermal evolution of synthetic planet populations that were obtained from a planet formation code (Alibert et al. 2005; Mordasini et al. 2012a,b).”
The Gemini Deep Planet Survey (2007, background): “Models predict that the timescale for formation of a planet like Jupiter through this process is about 5 Myr (Pollack et al. 1996), or about 1 Myr if migration of the core through the disk is allowed as the planet forms (Alibert et al. 2005).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, methodology): “In the core accretion model, a giant planet is produced from a relatively slow (∼1- 10Myr) collisional growth process that first builds up a large solid core and then rapidly accretes a massive gaseous envelope (e.g., Hubickyj et al. 2005; Alibert et al. 2005).”