Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration

By Shigeru Ida, D. Lin. 2008

382 citations recorded by the source corpus.

In a further development of a deterministic planet formation model (Ida & Lin), we consider the effect of type I migration of protoplanetary embryos due to their tidal interaction with their nascent disks. During the early phase of protostellar disks, although embryos rapidly emerge in regions interior to the ice line, uninhibited type I migration leads to their efficient self-clearing. But embryos continue to form from residual planetesimals, repeatedly migrate inward, and provide a main channel of heavy-element accretion onto their host stars. During the advanced stages of disk evolution (a few Myr), the gas surface density declines to values comparable to or smaller than that of the minimum mass nebula model, and type I migration is no longer effective for Mars-mass embryos. Over wide ranges of initial disk surface densities and type I migration efficiencies, the surviving population of embryos interior to the ice line has a total mass of several M⊕. With this reservoir, there is an adequate inventory of residual embryos to subsequently assemble into rocky planets similar to those around the Sun. However, the onset of efficient gas accretion requires the emergence and retention of cores more massive than a few M⊕ prior to the severe depletion of the disk gas. The formation probability of gas giant planets and hence the predicted mass and semimajor axis distributions of extrasolar gas giants are sensitively determined by the strength of type I migration. We suggest that the distributions consistent with observations can be reproduced only if the actual type I migration timescale is at least an order of magnitude longer than that deduced from linear theories.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7242651aa3deb667a9082f9353c028aad3359907

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In Astronomy and Astrophysics

1. D. Charbonneau
2. Jon Fortney
3. Timothy Morton
4. J. Johnson
5. M. Perryman
6. J. Winn
7. C. Mordasini
8. G. Marcy

Citations in the corpus

• 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).”
• INFRARED SIGNATURES OF DISRUPTED MINOR PLANETS AT WHITE DWARFS (2009, background): “Apparently, the assembly of planets from planetesimals is inefficient, and stars possess complex populations of orbiting material (see Ida & Lin 2008 and references therein).”
• TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “Alternatively, the 1AU jump may be indicative of a pile-up of planets at the typical orbital distance within which migration becomes inefficient due to either the presence of the ice line or a “dead zone” near 1AU (e.g. Ida & Lin 2008).”
• MIGRATION THEN ASSEMBLY: FORMATION OF NEPTUNE-MASS PLANETS INSIDE 1 AU (2011, result): “This is in contrast to the results of the predominant planet population synthesis models (e.g., Ida & Lin 2008; Mordasini et al. 2009), which predict that this mass range (10–50 M⊕) should be liberally populated with partially accreted giant planet cores (“hot Neptunes”) that have migrated in from…”
• The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, background): “The details ofthe mass-orbital period distribution are important because they contain information about the planet formation process (Armitage et al. 2002; Ida & Lin 2004a, 2004b, 2005, 2008a, 2008b; Alibert et al. 2005; Rice & Armitage 2005; Kornet & Wolf 2006).”
• Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “As the mass of the star increases, the snow line, at or beyond which most planets are thought to form, is located increasingly further out (asnow ∝ Mα∗ , with α between 1 and 2 (Ida & Lin 2008; Kennedy & Kenyon 2008a).”
• The HARPS search for southern extra-solar planets - XVII. Super-Earth and Neptune-mass planets in multiple planet systems HD 47 186 and HD 181 433 (2008, background): “Planetary formation simulations based on the core-accretion scenario, completed by Ida & Lin (2004a, 2008) also predict a bimodal distribution from gaseous giants to Super-Earth planets, and furthermore a paucity of extrasolar planets with masses in the range 10–100 M⊕.”
• Lithium depletion and the rotational history of exoplanet host stars (2008, background): “Such long-lived disks may be a necessary condition for planet formation and/or migration around young solar-type stars, at least for the class of giant exoplanets detected sofar (Ida & Lin 2008).”
• IDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 PC. I. SPECTROSCOPIC OBSERVATIONS (2009, background): “This is expected to be a key epoch for understanding planet formation, coinciding with the end of giant planet formation and the active phase of terrestrial planet formation (e.g., Mandell et al. 2007; Ida & Lin 2008).”
• Planet-Disk Interaction and Orbital Evolution (2012, background): “Ida & Lin (2008), Mordasini, Alibert & Benz (2009), and Mordasini et al. (2009) consider the effects of type I and type II migration in their population synthesis models.”
• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “Another significant problem for the migration paradigm is the fact that both radial velocity and transit methods find Neptune-mass planets in a part of parameter space that such models predicted to be devoid of planets (Ida & Lin 2008).”
• Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains (2017, background): “…Ogihara, Morbidelli & Guillot 2015a,b) or (2) assembly of planets at moderate or larger distances from the star followed by inward gas-driven migration (Terquem & Papaloizou 2007; Ida & Lin 2008, 2010; McNeil & Nelson 2010; Hellary & Nelson 2012; Cossou et al. 2014; Coleman & Nelson 2014, 2016).”
• EVIDENCE OF POSSIBLE SPIN–ORBIT MISALIGNMENT ALONG THE LINE OF SIGHT IN TRANSITING EXOPLANET SYSTEMS (2010, background): “Simple models of close-in exoplanet formation involving assembly near the ice line and quiescent migration through a gaseous protoplanetary disk predict that orbits should have only negligible misalignments with the spin of the host star (e.g. Lin et al. 1996; Ida & Lin 2008a,b).”
• PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “The relevant processes, including inward migration, have been simulated numerically both for individual planet growth and for entire populations of planets (Ida & Lin 2004, 2008b; Mordasini et al. 2009a; Schlaufman et al. 2010; Ida & Lin 2010; Alibert et al. 2011).”
• Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, methodology): “Also the population synthesis calculations of Ida & Lin (2004a, 2008) contain a large sub-population of low mass planets.”
• THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “…distribution of disk 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…”
• Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “…with Ida & Lin (2008a) who have found that the fraction of stars with giant planets is a monotonically decreasing function of the type I migration speed, unless the effect of an enhancement of the solid and gas surface density near the iceline due to a “dead zone” is included (Ida & Lin 2008b).”