However, within the explored space of disk parameters, only a small fraction-less than a few percent-of the models predict that the interior planet reaches beyond Almost-Equal-To 4 AU. Planets locked in the 3:2 orbital resonance that start moving outward from within 1-2 AU may reach beyond Almost-Equal-To 5 AU only under favorable conditions. For migrating planets locked in the 3:2 mean motion resonance, there are stalling radii that depend on disk viscosity and on stellar irradiation, when it determines the disk's thermal balance. (LANL), Los Alamos, NM (United States) Sponsoring Org.: USDOE National Aeronautics and Space Administration (NASA) OSTI Identifier: 1716805 Report Number(s): LA-UR-20-20979 Journal ID: ISSN 0035-8711 TRN: US2204787 Grant/Contract Number: 89233218CNA000001 80HQTR19T0071 Resource Type: Accepted Manuscript Journal Name: Monthly Notices of the Royal Astronomical Society Additional Journal Information: Journal Volume: 492 Journal Issue: 4 Journal ID: ISSN 0035-8711 Publisher: Royal Astronomical Society Country of Publication: United States Language: English Subject: 79 ASTRONOMY AND ASTROPHYSICS hydrodynamics planet–disc interactions protoplanetary = and/or by reducing the accretion rate toward the star, and hence depleting the inner disk. Publication Date: Research Org.: Los Alamos National Lab. Nacional Autonoma de Mexico (UNAM), Mexico City (Mexico) Nacional Autonoma de Mexico (UNAM), Ensenada (Mexico) Nacional Autonoma de Mexico (UNAM), Cuernavaca (Mexico) Within its limits, our work suggests that the reversed migration, associated with the resonance capture of Jupiter and Saturn, may be a low-probability evolutionary scenario, so that other planetary systems with giant planets are not expected to have experienced a Grand Tack-like evolutionary path. 2 T d tan F g g ac (6.20) d c c where, T transmitted torque (it is of the. Capture in the 1:2 MMR and inward or (nearly) stalled migration are highly favoured. Hz The excitation frequency equals the frequency of the planet carrier. ![]() This implies that an evolution as that proposed in the Grand Tack model depends on the precise initial orbits of Jupiter and Saturn and on the time-scales for their formation. We find that the evolution of initially compact orbital configurations is dependent on the value of Δa SJ. We also provide an assessment of the planet’s orbital dynamics at different epochs of Saturn’s growth. We study the evolution for different initial separations of the planets’ orbits, Δa SJ, to investigate whether they become captured in mean motion resonance (MMR) and the direction of the subsequent migration of the planet (inwards or outwards). Here, we study the dynamical evolution of Jupiter and Saturn embedded in a gaseous, solar nebula-type disc by means of hydrodynamics simulations with the FARGO2D1D code. He is available from the start in this beta build but can only be used in Time Attack. Planet - be responsible owners of our environment that make a difference by.
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