Orbital Migration and Mass Accretion of Protoplanets in Three‐dimensional Global Computations with Nested Grids

D’Angelo, Gennaro; Kley, W.; Henning, Thomas

doi:10.1086/367555

Cited by 243 publications

(289 citation statements)

References 30 publications

(59 reference statements)

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“…8), in good agreement with Nelson et al (2000), D'Angelo & Kley (2003) and a simple estimate of the viscous time scale. Note that due to the initial gap clearing phase the planet has already migrated to r = 9.43 after 535 orbits.…”

Section: Planet Calibration Run: Modelsupporting

confidence: 81%

Giant planet formation in stellar clusters: the effects of stellar fly-bys

Fragner¹,

Nelson²

2009

A&A

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Context. The majority of stars in the Galaxy are thought to have formed within stellar clusters, resulting in occasional close encounters between stars during the epoch of planet formation. Encounters between young stars which possess protoplanetary discs will cause significant modification of the disc structure, and perturb any planets forming within the disc. Aims. The primary aim of this work is to examine the effect of parabolic stellar encounters on the evolution of a Jovian-mass giant planet forming within a protoplanetary disc. We consider the effect on both the mass accretion and the migration history as a function of encounter distance. Methods. We use a grid-based hydrodynamics code to perform 2D simulations of a system consisting of a giant planet embedded within a gaseous disc orbiting around a star, which is perturbed by a passing star on a prograde, parabolic orbit. The disc model extends out to 50 AU, and parabolic encounters are considered with impact parameters ranging from 100−250 AU. Results. In agreement with previous work, we find that the disc is significantly tidally truncated for encounters <150 AU, and the removal of angular momentum from the disc by the passing star causes a substantial inflow of gas through the disc. The gap formed by the embedded planet becomes flooded with gas, causing the gas accretion rate onto the planet to increase abruptly. Gas flow through the gap, and into the inner disc, causes the positive inner disc torques exerted on the planet to increase, resulting in a sustained period of outward migration. For weaker interactions, corresponding to an encounter distance of ≥250 AU, we find that the planet-disc system experiences minimal perturbation. Conclusions. Our results indicate that stellar fly-bys in young clusters may significantly modify the masses and orbital parameters of giant planets forming within protostellar discs. Planets that undergo such encounters are expected to be more massive, and to orbit with larger semimajor axes, than planets in systems which have not experienced parabolic encounters.

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Section: Planet Calibration Run: Modelsupporting

confidence: 81%

Giant planet formation in stellar clusters: the effects of stellar fly-bys

Fragner¹,

Nelson²

2009

A&A

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“…The empirical formula for the accretion rate based on local two-dimensional isothermal hydrodynamic simulations (TW02) can be different from that derived based on more realistic simulations including, for example, three-dimensional accretion flow ( D'Angelo et al 2003;Bate et al 2003), a nonisothermal equation of state (TW02), and a magnetic field (Machida et al 2006). The modification would change the form of div , which would yield quantitatively different results.…”

Section: Remarks On the Uncertainties In The Modelmentioning

confidence: 99%

A Systematic Study of the Final Masses of Gas Giant Planets

Tanigawa

Ikoma

2007

ApJ

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We construct an analytic model for the gas accretion rate onto planets embedded in protoplanetary disks as a function of planetary mass, viscosity, scale height, and unperturbed surface density, and systematically study the long-term accretion and final masses of gas giant planets. We first derive an analytical formula for the surface density profile near the planetary orbit from considerations of the balance of force and dynamical stability. Using it in the empirical formula of normalized gas accretion rate that is derived based on hydrodynamic simulations, we then simulate the mass evolution of gas giant planets in viscously evolving disks. We finally determine the final mass as a function of semimajor axis of the planet. We find that the disk can be divided into three regions characterized by different processes by which the final mass is determined. In the inner region, the planet grows quickly and forms a deep gap to suppress the growth by itself before disk dissipation. The final mass shows the same trend as the mass determined by the viscous condition for gap opening, but is about 10 times larger than that. In the intermediate region, the disk's viscous diffusion limits gas accretion onto planets before deep gap formation. The final mass can be up to the disk mass, when the disk's viscous evolution occurs faster than disk evaporation. In the outer region, planets capture only tiny amounts of gas within the disk lifetime to form Neptune-like planets. We also derive analytic formulae for the final masses in the different regions and the locations of the boundaries, which are helpful to gain a systematic understanding of the masses of gas giant planets.

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“…Subsequent eccentricity damping in the protoplanetary disk may also occur. The distribution of final orbital sizes may result from inward migration and mutual interactions among the planets, in a race against the dissipation of the protoplanetary disk, leaving the planets frozen in their tracks (Armitage et al 2003;Trilling et al 2002;D'Angelo et al 2003; Thommes & Lissauer 2003;Ida & Lin 2004;Alibert et al 2005). …”

Section: Introductionmentioning

confidence: 99%

Five New Multicomponent Planetary Systems

Vogt

Butler

Marcy

et al. 2005

ApJ

234

274

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We report Doppler measurements for six nearby G-and K-type main-sequence stars that show multiple low-mass companions, at least one of which has planetary mass. One system has three planets, the fourth triple-planet system known around a normal star, and another has an extremely low minimum mass of 18 M È . HD 128311 ( K0 V ) has two planets (one previously known) with minimum masses (M sin i) of 2.18M J and 3.21M J and orbital periods of 1.26 and 2.54 yr, suggesting a possible 2:1 resonance. For HD 108874 (G5 V ), the velocities reveal two planets (one previously known) having minimum masses and periods of (M sin i b ¼ 1:36M J , P b ¼ 1:08 yr) and (M sin i c ¼ 1:02M J , P c ¼ 4:4 yr). HD 50499 (G1 V ) has a planet with P ¼ 6:8 yr and M sin i ¼ 1:7M J , and the velocity residuals exhibit a trend of À4.8 m s À1 yr À1 , indicating a more distant companion with P > 10 yr and minimum mass of 2M J . HD 37124 (G4 IV-V ) has three planets, one having M sin i ¼ 0:61M J and P ¼ 154:5 days, as previously known. We find two plausible triple-planet models that fit the data, both having a second planet near P ¼ 840 days, with the more likely model having its third planet in a 6 yr orbit and the other one in a 29 day orbit. For HD 190360, we confirm the planet having P ¼ 7:9 yr and M sin i ¼ 1:5M J as found by the Geneva team, but we find a distinctly noncircular orbit with e ¼ 0:36 AE 0:03, rendering this not an analog of Jupiter as had been reported. Our velocities also reveal a second planet with P ¼ 17:1 days and M sin i ¼ 18:1 M È . HD 217107 (G8 IV) has a previously known ''hot Jupiter'' with M sin i ¼ 1:4M J and P ¼ 7:13 days, and we confirm its high eccentricity, e ¼ 0:13. The velocity residuals reveal an outer companion in an eccentric orbit, having minimum mass of M sin i > 2M J , eccentricity e $ 0:5, and a period P > 8 yr, implying a semimajor axis a > 4 AU and providing an opportunity for direct detection. We have obtained high-precision photometry of five of the six planetary host stars with three of the automated telescopes at Fairborn Observatory. We can rule out significant brightness variations in phase with the radial velocities in most cases, thus supporting planetary reflex motion as the cause of the velocity variations. Transits are ruled out to very shallow limits for HD 217107 and are also shown to be unlikely for the prospective inner planets of the HD 37124 and HD 108874 systems. HD 128311 is photometrically variable with an amplitude of 0.03 mag and a period of 11.53 days, which is much shorter than the orbital periods of its two planetary companions. This rotation period explains the origin of periodic velocity residuals to the two-planet model of this star. All of the planetary systems here would be further constrained with astrometry by the Space Interferometry Mission.

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Orbital Migration and Mass Accretion of Protoplanets in Three‐dimensional Global Computations with Nested Grids

Cited by 243 publications

References 30 publications

Giant planet formation in stellar clusters: the effects of stellar fly-bys

Giant planet formation in stellar clusters: the effects of stellar fly-bys

A Systematic Study of the Final Masses of Gas Giant Planets

Five New Multicomponent Planetary Systems

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