Envelopes of embedded super-Earths I. Two-dimensional simulations
Autor: | William Béthune, Roman R. Rafikov |
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Přispěvatelé: | Rafikov, Roman [0000-0002-0012-1609], Apollo - University of Cambridge Repository |
Rok vydání: | 2019 |
Předmět: |
Physics
Earth and Planetary Astrophysics (astro-ph.EP) education.field_of_study 010308 nuclear & particles physics Gas giant Population FOS: Physical sciences Astronomy and Astrophysics Astrophysics Protoplanetary disk 01 natural sciences Accretion (astrophysics) Pluto 13. Climate action Space and Planetary Science Planet astro-ph.EP 0103 physical sciences Astrophysics::Earth and Planetary Astrophysics Adiabatic process education 010303 astronomy & astrophysics Astrophysics - Earth and Planetary Astrophysics Envelope (waves) |
DOI: | 10.48550/arxiv.1907.01951 |
Popis: | Measurements of exoplanetary masses and radii have revealed a population of massive super-Earths --- planets sufficiently large that, according to one dimensional models, they should have turned into gas giants. To better understand the origin of these objects, we carry out hydrodynamical simulations of planetary cores embedded in a nascent protoplanetary disk. In this first paper of a series, to gain intuition as well as to develop useful diagnostics, we focus on two-dimensional simulations of the flow around protoplanetary cores. We use the pluto code to study isothermal and adiabatic envelopes around cores of sub- to super-thermal masses, fully resolving the envelope properties down to the core surface. Owing to the conservation of vortensity, envelopes acquire a substantial degree of rotational support when the core mass increases beyond the thermal mass, suggesting a limited applicability of one-dimensional models for describing the envelope structure. The finite size of the core (relatively large for super-Earths) also controls the amount of rotational support in the entire envelope. Steady non-axisymmetric shocks develop in the supersonic envelopes of high-mass cores, triggering mass accretion and turbulent mixing in their interiors. We also examine the influence of the gas self-gravity on the envelope structure. Although it only weakly alters the properties of the envelopes, the gas gravity has significant effect on the properties of the density waves triggered by the core in the protoplanetary disk. Comment: 17 pages, 24 figures; accepted for publication in MNRAS Published by Oxford University Press |
Databáze: | OpenAIRE |
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