Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime

By C. Mordasini, Y. Alibert, W. Benz, H. Klahr, Th. Henning. 2012

264 citations recorded by the source corpus.

Context. This is the fourth paper in a series showing the results of planet population synthesis calculations. Aims. Our goal in this paper is to systematically study the effects of important disk properties, namely disk metallicity, mass and lifetime on fundamental planetary properties. Methods. For a large number of protoplanetary disks we calculate a population of planets with our core accretion formation model including planet migration and disk evolution. Results. We find a large number of correlations: Regarding the planetary initial mass function, metallicity, disk mass and disk lifetime have different roles: For high [Fe/H], giant planets are more frequent. For high disk masses, giant planets are more massive. For long disk lifetimes, giant planets are both more frequent and massive. At low metallicities, very massive giant planets cannot form, but otherwise giant planet mass and metallicity are uncorrelated. In contrast, planet masses and disk gas masses are correlated. The sweet spot for giant planet formation is at 5 AU. In- and outside this distance, higher planetesimals surface densities are necessary. Low metallicities can be compensated by high disk masses, and vice versa, but not ad infinitum. At low metallicities, giant planets only form outside the ice line, while at high metallicities, giant planet formation occurs throughout the disk. The extent of migration increases with disk mass and lifetime and usually decreases with metallicity. No clear correlation of metallicity and the semimajor axis of giant planets exists because in low [Fe/H] disks, planets start further out, but migrate more, whereas for high [Fe/H] they start further in, but migrate less. Close-in low mass planets have a lower mean metallicity than Hot Jupiters. Conclusions. The properties of protoplanetary disks are decisive for the properties of planets, and leave many imprints.

View Paper: https://www.semanticscholar.org/paper/ebaf09fe8183ff9e657df3510367b0634d5e959b

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1. Jon Fortney
2. N. Madhusudhan
3. C. Mordasini
4. D. Sing
5. H. Knutson
6. H. Wakeford
7. M. Line
8. M. Perryman

Citations in the corpus

• Characterization of exoplanets from their formation - I. Models of combined planet formation and evolution (2012, background): “…of the core, a new initial profile for the gaseous disk, a new prescription for the photoevaporation of the disk (including external and internal photoevaporation), and finally a realistically low grain opacity for the gaseous envelope (presented in a dedicated work, Mordasini et al. 2012c).”
• The planet search programme at the ESO CES and HARPS - IV. The search for Jupiter analogues around solar-like stars (2012, result): “Such low observed frequencies are compatible with the non-detection of a Jupiteranalogue in our sample and a decreasing frequency of giant planets at larger distances (& 5 AU) is also predicted with core accretion theory (Mordasini et al. 2012).”
• SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, result): “Both results, however, are in full agreement with the expectations from the most recent models of planet formation based on the core-accretion paradigm (e.g. Mordasini et al. 2012, and discussion therein).”
• ALMA SURVEY OF LUPUS PROTOPLANETARY DISKS. I. DUST AND GAS MASSES (2016, background): “This is because core growth is more efficient both in higher-mass disks (e.g., Thommes et al. 2008; Mordasini et al. 2012) and around highermass stars (e.g., Kennedy & Kenyon 2008).”
• An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “Indeed, exoplanet population synthesis models indicate that planetary properties and architectures are dictated by the initial dust and gas content of protoplanetary disks and their subsequent evolution (e.g., Thommes et al. 2008; Mordasini et al. 2012; Bitsch et al. 2015; Mordasini et al. 2016).”
• Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, methodology): “This value has been determined in Mordasini et al. (2012c) by comparison with detailed grain evolution calculations in protoplanetary envelopes (Movshovitz et al. 2010).”
• 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).”
• THE MASS–METALLICITY RELATION FOR GIANT PLANETS (2015, background): “The population synthesis models in Mordasini et al. (2012) also observe and discuss an absence of very massive planets around metal-poor stars.”
• A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, background): “Indeed, planet formation models find that the disk mass strongly impacts the frequency and location of planets that can form, from giants down to Earth-sized planets (e.g., Raymond et al. 2007; Alibert et al. 2011; Mordasini et al. 2012).”
• Radial Migration of Gap-opening Planets in Protoplanetary Disks. I. The Case of a Single Planet (2018, methodology): “It will be a useful tool for the population synthesis calculations because the outcome of these calculations depends strongly on the way in which the planets actually migrate (e.g., Mordasini et al. 2012; Ida et al. 2013).”
• The Complete Transmission Spectrum of WASP-39b with a Precise Water Constraint (2017, background): “Gravitational instability theory suggests that planets will have the same atmospheric metallicity as the central star, while with core accretion theory, lower mass planets will have higher atmospheric metallicity (e.g. Mordasini et al. 2012; Fortney et al. 2013).”
• SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, background): “In addition, the protoplanetary disks around binary stars may have more mass than around single stars, which simulations suggest leads to larger planets (Mordasini et al. 2012).”
• SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, background): “Interestingly, we find that the radius distribution of EGPs with a moderate irradiation is significantly different from the one predicted by Mordasini et al. (2012b).”