The Newtonian potential of thin disks

Huré, Jean-Marc; Hersant, F.

doi:10.1051/0004-6361/201015854

Cited by 11 publications

(5 citation statements)

References 19 publications

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“…At the same time, there may well be a range of parameters such that (𝐻/𝑅) 2 < 𝑀 d /𝑀 ★ < 𝐻/𝑅, in which self-gravity gives a dominant contribution to the rotation curve, while the disc is gravitationally stable (Veronesi et al 2021). It is worth noting that the pressure-less case, for a power law surface density, had been discussed in the context of AGNs by Huré & Hersant (2011).…”

Section: Modeling the Rotation Curvementioning

confidence: 99%

Dynamical mass measurements of two protoplanetary discs

Lodato

Rampinelli

Viscardi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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ALMA observations of line emission from planet forming discs have demonstrated to be an excellent tool to probe the internal disc kinematics, often revealing subtle effects related to important dynamical processes occurring in them, such as turbulence, or the presence of planets, that can be inferred from pressure bumps perturbing the gas motion, or from detection of the planetary wake. In particular, we have recently shown for the case of the massive disc in Elias 2-27 how one can use such kind of observations to measure deviations from Keplerianity induced by the disc self-gravity, thus constraining the total disc mass with good accuracy and independently on mass conversion factors between the tracer used and the total mass. Here, we refine our methodology and extend it to two additional sources, GM Aur and IM Lup, for which archival line observations are available for both the 12CO and the 13CO line. For IM Lup, we are able to obtain a consistent disc mass of Mdisc = 0.1 M⊙, implying a disc-star mass ratio of 0.1 (consistent with the observed spiral structure in the continuum emission) and a gas/dust ratio of ∼65 (consistent with standard assumptions), with a systematic uncertainty by a factor ≃ 2 due to the different methods to extract the rotation curve. For GM Aur, the two lines we use provide slightly inconsistent rotation curves, that cannot be attributed only to a difference in the height of the emitting layer, nor to a vertical temperature stratification. Our best fit disc mass measurement is Mdisc = 0.26 M⊙, implying a disc-star mass ratio of ∼0.35 and a gas/dust ratio of ∼130. Given the complex kinematics in the outer disc of GM Aur and its interaction with the infalling cloud, the CO lines might not well trace the rotation curve and our results for this source should then be considered with some caution.

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Section: Modeling the Rotation Curvementioning

confidence: 99%

Dynamical mass measurements of two protoplanetary discs

Lodato

Rampinelli

Viscardi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…The code also includes the disk gravitational potential acting on the planets expressed in spherical coordinates as (Terquem & Ajmia 2010;Huré & Hersant 2011)…”

Section: Methodsmentioning

confidence: 99%

Resonance capture and long-term evolution of planets in binary star systems

Roisin

Doukhanin

Teyssandier

et al. 2022

A&A

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Aims. The growing population of planets discovered in orbit around one stellar component of a binary star raises the question of the influence of the binary companion on the formation process of planetary systems. The aim of this work is to study the impact of a binary companion on the evolution of two-planet systems during both the type-II migration phase and their long-term evolution after the dissipation of the protoplanetary disk. Methods. We used the symplectic integrator SyMBA, modified to include a wide binary companion. We also included the Type-II migration of giant planets during the protoplanetary disk phase with suitable eccentricity and inclination damping as well as the gravitational potential acting on the planets due to the disk and the nodal precession of the disk induced by the binary companion. We considered various inclinations, eccentricities, and separations of the binary companion. Results. Disk migration allows for the formation of planet pairs in mean-motion resonances despite the presence of the binary companion. When the binary separation is wide (1000 au), the timescale of the perturbations that it raises on the planets is longer than the disk's lifetime and resonant pairs are routinely formed in the 2:1, 5:2, and 3:1 commensurabilities. Provided the planet-planet interaction timescale is smaller than the timescale of binary perturbations, these systems can remain in resonance long after the disk has dissipated. When the binary separation is smaller (250 au), only planets in the 2:1 resonance tend to remain in a resonant state and more chaotic evolutions are observed, as well as more ejections. After those ejections, the remaining planet can become eccentric due to the perturbations from the binary companion in addition, for strongly inclined binary companions, captures in the von Ziepel-Lidov-Kozai resonance can occur. Whereas in systems with two planets, this mechanism is quenched by planet-planet interactions. Our simulations reveal that the interplay between planet-disk, planet-planet, and planet-binary interactions can lead to the formation of resonant pairs of planets which remain stable over timescales much longer than the disk's lifetime.

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“…where (r, ϕ, θ) correspond to the spherical coordinates of the planet, Σ is the disk surface density, ain and aout are the inner and outer edges of the disk and G is the gravitational constant. Following Huré & Hersant (2011), the potential can be expressed as…”

Section: Disk Gravitational Potentialmentioning

confidence: 99%

Planetary migration in precessing disks for S-type wide binaries

Roisin,

Teyssandier,

Libert

2021

Preprint

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The discovery of numerous circumprimary planets in the last few years has brought to the fore the question of planet formation in binary systems. The significant dynamical influence, during the protoplanetary disk phase, of a binary companion on a giant planet has previously been highlighted for wide binary stars. In particular, highly inclined binary companion can induce perturbations on the disk and the planets, through the Lidov-Kozai resonance, which could inhibit the formation process. In this work, we aim to study how the disk gravitational potential acting on the planet and the nodal precession induced by the wide binary companion with separation of 1000 AU on the disk act to suppress the Lidov-Kozai perturbations on a migrating giant planet. We derive new approximate formulas for the evolution of the disk's inclination and longitude of the ascending node, in the case of a rigidly precessing disk with a decreasing mass and perturbed by a wide binary companion, which are suitable for N -body simulations. We carry out 3200 simulations with several eccentricity and inclination values for the binary companion. The gravitational and damping forces exerted by the disk on the planet tend to keep the latter in the midplane of the former, and suppress the effect of the binary companion by preventing the planet from getting locked in the Lidov-Kozai resonance during the disk phase. We also confirm that because of nodal precession induced by the binary, a primordial spin-orbit misalignment could be generated for circumprimary planets with an inclined binary companion.

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The Newtonian potential of thin disks

Cited by 11 publications

References 19 publications

Dynamical mass measurements of two protoplanetary discs

Dynamical mass measurements of two protoplanetary discs

Resonance capture and long-term evolution of planets in binary star systems

Planetary migration in precessing disks for S-type wide binaries

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