The Effects of Radiative Feedback and Circumplanetary Disk Formation on the Gas Accretion

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The Effects of Radiative Feedback and Circumplanetary Disk Formation on the Gas Accretion

EPSC Abstracts Vol. 13, EPSC-DPS2019-174-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. The effects of radiative feedback and circumplanetary disk formation on the gas accretion Judit Szulagyi Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zürich Abstract 1. Figures The traditional 1D core accretion scenario predicts that in the third and last phase of formation, the planets grow exponentially. In this stage their gaseous envelope collapse onto the core and this launches a runaway accretion of gas. If this were true, the im- plication is that there should be a dichotomy in the planet mass distribution: either planets do not enter the runaway phase and remain < 30MEarth or be- come several times more massive than Jupiter in a short time when entering the runaway phase. This Figure 1: The temperature color-map of a circumplan- is, however, in contrast with the observations. I carry etary disk, with the vertical accretion stream. The high out 3D radiative hydrodynamic simulations of planet temperatures lead to high pressure in the planetary en- formation, which reveals that a circumplanetary disk velope, which will be mainly avoided by the accre- forms around the planetary core. This disk is limit- ational streamlines. This is the visual picture of how ing the accretion to the planet, first, because it breaks the radiative feedback efficiently decreases the accre- the spherical accretion, second, because the circum- tion onto the planet. The accretion rate will scale with planetary disk is heated up by the accretion process. the cooling time/efficiency. Where the material is op- As the planet vicinity is hot, the gas pressure grows tically thick, the accretion is very low. In this regions, and acts against accretion. The accretion rate will de- the formation of massive planets are less likely. Where pend on the cooling timescales, therefore it depends the material is optically thin, the cooling times are very on the opacity. This radiative feedback can signifi- fast, therefore the accretion is efficient and the planet cantly lengthen the planet formation timescale in the can reach high masses. The local changes in opacity in optically thick regions of the circumstellar- and cir- the protoplanetary disk can explain how a large spec- cumplanetary disks. The thermodynamics, especially trum of planetary masses can form, e.g. intermediate the local changes in the opacity will therefore con- mass giants between 30MEarth till Saturn-mass. trol the final masses of planets. The reduced accretion ∼ due to radiative feedback can explain the existence of the intermediate mass giant planets and the rareness of super-Jupiters..

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