Planet formation: The case for large efforts on the computational side. (arXiv:1903.04546v1 [astro-ph.EP])

Planet formation: The case for large efforts on the computational side. (arXiv:1903.04546v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lyra_W/0/1/0/all/0/1">Wladimir Lyra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haworth_T/0/1/0/all/0/1">Thomas Haworth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bitsch_B/0/1/0/all/0/1">Bertram Bitsch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casassus_S/0/1/0/all/0/1">Simon Casassus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuello_N/0/1/0/all/0/1">Nicolás Cuello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Currie_T/0/1/0/all/0/1">Thayne Currie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspar_A/0/1/0/all/0/1">Andras Gáspár</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jang_Condell_H/0/1/0/all/0/1">Hannah Jang-Condell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klahr_H/0/1/0/all/0/1">Hubert Klahr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leigh_N/0/1/0/all/0/1">Nathan Leigh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lodato_G/0/1/0/all/0/1">Giuseppe Lodato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Low_M/0/1/0/all/0/1">Mordecai-Mark Mac Low</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maddison_S/0/1/0/all/0/1">Sarah Maddison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mamatsashvili_G/0/1/0/all/0/1">George Mamatsashvili</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McNally_C/0/1/0/all/0/1">Colin McNally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">Andrea Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_S/0/1/0/all/0/1">Sebastián Pérez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sengupta_D/0/1/0/all/0/1">Debanjan Sengupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stamatellos_D/0/1/0/all/0/1">Dimitris Stamatellos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szulagyi_J/0/1/0/all/0/1">Judit Szulágyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Teague_R/0/1/0/all/0/1">Richard Teague</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Turner_N/0/1/0/all/0/1">Neal Turner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umurhan_O/0/1/0/all/0/1">Orkan Umurhan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_J/0/1/0/all/0/1">Jacob White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wootten_A/0/1/0/all/0/1">Al Wootten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alarcon_F/0/1/0/all/0/1">Felipe Alarcon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Apai_D/0/1/0/all/0/1">Daniel Apai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayo_A/0/1/0/all/0/1">Amelia Bayo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergin_E/0/1/0/all/0/1">Edwin Bergin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carrera_D/0/1/0/all/0/1">Daniel Carrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cleeves_I/0/1/0/all/0/1">Ilse Cleeves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cooray_A/0/1/0/all/0/1">Asantha Cooray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golabek_G/0/1/0/all/0/1">Gregor Golabek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gressel_O/0/1/0/all/0/1">Oliver Gressel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gurwell_M/0/1/0/all/0/1">Mark Gurwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krijt_S/0/1/0/all/0/1">Sebastiaan Krijt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hall_C/0/1/0/all/0/1">Cassandra Hall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_R/0/1/0/all/0/1">Ruobing Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Du_F/0/1/0/all/0/1">Fujun Du</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pascucci_I/0/1/0/all/0/1">Ilaria Pascucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilee_J/0/1/0/all/0/1">John Ilee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Izidoro_A/0/1/0/all/0/1">Andre Izidoro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_J/0/1/0/all/0/1">Jes Jorgensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kama_M/0/1/0/all/0/1">Mihkel Kama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mawet_D/0/1/0/all/0/1">Dimitri Mawet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Jinyoung Serena Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leisawitz_D/0/1/0/all/0/1">David Leisawitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lichtenberg_T/0/1/0/all/0/1">Tim Lichtenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marel_N/0/1/0/all/0/1">Nienke van der Marel</a>, et al. (7 additional authors not shown)

Modern astronomy has finally been able to observe protoplanetary disks in
reasonable resolution and detail, unveiling the processes happening during
planet formation. These observed processes are understood under the framework
of disk-planet interaction, a process studied analytically and modeled
numerically for over 40 years. Long a theoreticians’ game, the wealth of
observational data has been allowing for increasingly stringent tests of the
theoretical models. Modeling efforts are crucial to support the interpretation
of direct imaging analyses, not just for potential detections but also to put
meaningful upper limits on mass accretion rates and other physical quantities
in current and future large-scale surveys. This white paper addresses the
questions of what efforts on the computational side are required in the next
decade to advance our theoretical understanding, explain the observational
data, and guide new observations. We identified the nature of accretion, ab
initio planet formation, early evolution, and circumplanetary disks as major
fields of interest in computational planet formation. We recommend that
modelers relax the approximations of alpha-viscosity and isothermal equations
of state, on the grounds that these models use flawed assumptions, even if they
give good visual qualitative agreement with observations. We similarly
recommend that population synthesis move away from 1D hydrodynamics. The
computational resources to reach these goals should be developed during the
next decade, through improvements in algorithms and the hardware for hybrid
CPU/GPU clusters. Coupled with high angular resolution and great line
sensitivity in ground based interferometers, ELTs and JWST, these advances in
computational efforts should allow for large strides in the field in the next
decade.

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