Formation of Jupiter using opacities based on detailed grain physics

By N. Movshovitz, P. Bodenheimer, M. Podolak, Jack J. Lissauer. 2010

159 citations recorded by the source corpus.

Abstract Numerical simulations, based on the core-nucleated accretion model, are presented for the formation of Jupiter at 5.2 AU in three primordial disks with three different assumed values of the surface density of solid particles. The grain opacities in the envelope of the protoplanet are computed using a detailed model that includes settling and coagulation of grains and that incorporates a recalculation of the grain size distribution at each point in time and space. We generally find lower opacities than the 2% of interstellar values used in previous calculations (Hubickyj, O., Bodenheimer, P., Lissauer, J.J. [2005]. Icarus 179, 415–431; Lissauer, J.J., Hubickyj, O., D’Angelo, G., Bodenheimer, P. [2009]. Icarus 199, 338–350). These lower opacities result in more rapid heat loss from and more rapid contraction of the protoplanetary envelope. For a given surface density of solids, the new calculations result in a substantial speedup in formation time as compared with those previous calculations. Formation times are calculated to be 1.0, 1.9, and 4.0 Myr, and solid core masses are found to be 16.8, 8.9, and 4.7  M ⊕ , for solid surface densities, σ , of 10, 6, and 4 g cm −2 , respectively. For σ  = 10 and σ  = 6 g cm −2 , respectively, these formation times are reduced by more than 50% and more than 80% compared with those in a previously published calculation with the old approximation to the opacity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f4c8703ecc466e1fb26c63e4b541a8b18c303fac

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

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

Citations in the corpus

• FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES (2011, methodology): “Methods Models for the formation and evolution of a planet consisting of a core of heavy elements and a gaseous envelope of solar composition are calculated according to the procedures described by Pollack et al. (1996) and Movshovitz et al. (2010).”
• PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “Rocky composition for the smallest planets supports the core-accretion model of planet formation (Pollack et al. 1996; Lissauer et al. 2009; Movshovitz et al. 2010).”
• 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).”
• SPECTRAL AND PHOTOMETRIC DIAGNOSTICS OF GIANT PLANET FORMATION SCENARIOS (2011, background): “The opacities of grains in the protoplanetary nebula can also have an important influence on the core-accretion formation process (Movshovitz et al. 2010).”
• PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, background): “At fopa = 0, even very low-mass cores can become supercritical and trigger giant planet formation (Movshovitz et al. 2010; Mordasini et al. 2014a).”
• Debris disks as signposts of terrestrial planet formation (2011, background): “…planets underwent a violent phase of scattering but in a 1 Recent calculations of planet formation via core accretion support such an assumption (Movshovitz et al. 2010), though it should be noted that these are subject to substantial uncertainties because the physics of type I migration…”
• TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, background): “Depending on the opacity of the planet envelope, this phase lasts for up to a few Myr (Pollack et al. 1996; Papaloizou & Nelson 2005; Movshovitz et al. 2010).”
• Dynamics of Protoplanetary Disks (2010, background): “Theoretical estimates of the time needed to assemble the core of a gas giant planet (Movshovitz et al. 2010) are, to within uncertain factors of a few, equal to the observed lifetime of protoplanetary gas disks.”
• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, result): “This reduction is rather small compared to the large effect of the opacity in formation calculations without migration (Pollack et al. 1996; Movshovitz et al. 2010).”
• Characterization of exoplanets from their formation - I. Models of combined planet formation and evolution (2012, background): “But this way we allow for direct comparison with numerous previous works that used similar assumptions as, e.g., Pollack et al. (1996), Lissauer et al. (2009), and Movshovitz et al. (2010).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, unknown): “…the cores of gas giants is the core-accretion model, a slow process involving the collision of planetesimals (Safronov & Zvjagina 1969), with giant planets growing massive enough to gravitationally trap light gases (Mizuno 1980; Pollack et al. 1996; Lissauer et al. 2009; Movshovitz et al. 2010).”
• MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “…range from ∼0.1–100 M⊕ over ∼0.05–100 AU.6 In timedependent models, Lacc is a prescribed function of time that enables one to follow the envelope’s quasi-static contraction and mass gain from the nebula (Pollack et al. 1996; Bodenheimer et al. 2000; Movshovitz et al. 2010; Rogers et al. 2011).”