Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities

By Shigeru Ida, D. Lin. 2004

413 citations recorded by the source corpus.

The apparent dependence of detection frequency of extrasolar planets on the metallicity of their host stars is investigated with Monte Carlo simulations using a deterministic core-accretion planet formation model. According to this model, gas giants formed and acquired their mass Mp through planetesimal coagulation followed by the emergence of cores onto which gas is accreted. These protoplanets migrate and attain their asymptotic semimajor axis a through tidal interaction with their nascent disk. Based on the observed properties of protostellar disks, we generate an Mp-a distribution. Our results reproduce the observed lack of planets with intermediate mass Mp = 10-100 M⊕ and a ≲ 3 AU and with large mass Mp ≳ 103 M⊕ and a ≲ 0.2 AU. Based on the simulated Mp-a distributions, we also evaluate the metallicity dependence of the fraction of stars harboring planets that are detectable with current radial velocity surveys. If protostellar disks attain the same fraction of heavy elements as contained in their host stars, the detection probability around metal-rich stars would be greatly enhanced because protoplanetary cores formed in them can grow to several Earth masses prior to their depletion. These large masses are required for the cores to initiate rapid gas accretion and to transform into giant planets. The theoretically extrapolated metallicity dependence is consistent with the observations. This correlation does not arise naturally in the gravitational-instability scenario. We also suggest other metallicity dependences of the planet distributions that can be tested by ongoing observations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a01da79b948a418e5ae13e4e689d3fce8616159c

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Citations in the corpus

Robust characteristics method for modelling multiphase visco-elasto-plastic thermo-mechanical problems (2007, background): “In future work, such instabilities should be considered in the context of ongoing planetary accretion first in 2D and then in 3D rather than starting from the equilibrium state of a 1D accretion model (e.g. Ida and Lin, 2004).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “One explanation posits that planets are more efficiently formed around stars with higher metallicity because of the higher fraction of solids available in the circumstellar disk (Ida & Lin 2004b).”
A New Planet around an M Dwarf: Revealing a Correlation between Exoplanets and Stellar Mass (2007, background): “This finding can be understood in the context of the core accretion model: increasing the metallicity of star/disk system increases the surface density of solid particulate matter, which leads to an enhanced growth rate for protoplanetary cores (Ida & Lin 2004; Kornet et al. 2005; Ida & Lin 2005a).”
THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION (2010, background): “A zeroth-order prediction of the core-accretion paradigm for giant planet formation is that the frequency of readily detectable giant planets should increase with both increasing stellar metallicity and with increasing stellar mass (Laughlin et al. 2004; Ida & Lin 2004, 2005).”
ON THE METAL RICHNESS OF M DWARFS WITH PLANETS (2009, background): “Stars with higher metallicities have disks containing a greater abundance of refractory material in the form of dust, allowing rocky and icy cores to grow more rapidly (Ida & Lin 2004).”
Spectroscopic parameters for 451 stars in the HARPS GTO planet search program - Stellar [Fe/H] and the frequency of exo-Neptunes (2008, result): “…the few low-mass planets found appear to follow a trend in metallicity that differ from wellestablished relations for giant planets first pointed out by Udry et al. (2006), this result, is supported by planet-formation models based on the core-accretion paradigm (Ida & Lin 2004; Benz et al. 2006).”
Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism (2008, background): “In relativelymassive and/ormetal-rich disks,multiple gas giants are likely to form (e.g., Kokubo & Ida 2002; Ida & Lin 2004a, 2004b, 2008).”
The HARPS search for southern extra-solar planets - XIII. A planetary system with 3 super-Earths (4.2, 6.9, and 9.2 M) (2008, background): “One of the most obvious example of that dialogue between planetary formation theory and observations is illustrated by the comparison of the planetary mass vs semimajor axis (m 2 − a) diagram (Ida & Lin 2004a; Mordasini et al. 2008).”
Hints for a Turnover at the Snow Line in the Giant Planet Occurrence Rate (2018, methodology): “Formation via core accretion and multi cores interaction: The Bern Model As in Ida & Lin (2004b), the GP formation model used in Mordasini (2018) relies on the core accretion paradigm.”
A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: Cold neptunes are common (2009, background): “These discoveries indicate that cold Neptune in orbits beyond the “snowline” (Ida & Lin 2004; Laughlin, Bodenheimer & Adams 2004; Kennedy, Kenyon & Bromley 2006) around late-type stars, are significantly more common than gas giants with frequency of ≥16% at 90% confidence (Gould et al. 2006), which…”
About 30% of Sun-like Stars Have Kepler-like Planetary Systems: A Study of Their Intrinsic Architecture (2018, background): “In the standard core accretion theories (Ida & Lin 2004; Mordasini et al. 2009), in which the cores of these planets are formed at large distances when the gas disk is still fully present, these planets are migrated rapidly to near the inner edge of the proto-planetary disks.”
A correlation between the heavy element content of transiting extrasolar planets and the metallicity of their parent stars (2006, methodology): “…the relation, and the large values of MZ obtained in some cases are surprising and have not been predicted by formation models, either in the framework of the coreinstability model (Ida & Lin 2004; Alibert et al. 2005) or by models involving direct gravitational instability of the gas (Boss 2003).”
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS (2010, methodology): “…grains, coagulation of planetesimals, mergers of protoplanetary embryos, and gas accretion onto super-Earth (i.e., masses in excess of a few Earth-masses) cores, we constructed a population-synthesis model through a series of papers (Ida & Lin 2004a, 2004b, 2005, 2008a, 2008b, hereafter Papers I–”
Spectroscopic metallicities for planet-host stars: Extending the samples (2005, background): “Current models can even reasonably explain the observed [Fe/H] distribution of planet-host star (Ida & Lin 2004a,b).”