Thermal velocity equilibrium in the protoplanetary cloud

Hornung, Peter; Pellat, R.; Barge, P.

doi:10.1016/0019-1035(85)90092-2

Cited by 64 publications

(49 citation statements)

References 9 publications

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“…We solve a set of Fokker-Planck equations to follow the time-evolution of h ik and v ik (Hornung et al 1985;Wetherill & Stewart 1993;Stewart & Ida 2000):…”

Section: A2 Velocity Evolutionmentioning

confidence: 99%

Gravitational Stirring in Planetary Debris Disks

Kenyon

Bromley

2001

The Astronomical Journal

131

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We describe gravitational stirring models of planetary debris disks using a new multi-annulus planetesimal evolution code. The current code includes gravitational stirring and dynamical friction; future studies will include coagulation, fragmentation, Poynting-Robertson drag, and other physical processes. We use the results of our calculations to investigate the physical conditions required for small bodies in a planetesimal disk to reach the shattering velocity and begin a collisional cascade. Our results demonstrate that disks composed primarily of bodies with a single size will not undergo a collisional cascade which produces small dust grains at 30-150 AU on timescales of 1 Gyr or smaller. Disks with a size distribution of bodies reach conditions necessary for a collisional cascade in 10 Myr to 1 Gyr if the disk is at least as massive as a minimum mass solar nebula and if the disk contains objects with radii of 500 km or larger. The estimated 500 Myr survival time for these disks is close to the median age of roughly 400 Myr derived for nearby stars with dusty disks.Comment: 23 pages of text + 16 Figures; to appear in the Astronomical Journal, January 200

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“…We solve a set of Fokker-Planck equations to follow the time-evolution of h ik and v ik (Hornung et al 1985;Wetherill & Stewart 1993;Stewart & Ida 2000):…”

Section: A2 Velocity Evolutionmentioning

confidence: 99%

Gravitational Stirring in Planetary Debris Disks

Kenyon

Bromley

2001

The Astronomical Journal

131

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“…(Hornung, Pellat & Borge 1985, Stewart & Wetherill 1988), where v ∥ and σ ∥ are the velocity and the velocity dispersion in the direction parallel to the plane while v ⊥ and σ ⊥ are those in the perpendicular direction. We suppose that σ ∥ and σ ⊥ are constants and that their ratio is simply taken to be 2:1.…”

Section: Planetary Migration Modelmentioning

confidence: 99%

Migration of giant planets in planetesimal discs

Popolo

Gambera

Ercan

2001

Monthly Notices of the Royal Astronomical Society

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Planets orbiting a planetesimal circumstellar disc can migrate inward from their initial positions because of dynamical friction between planets and planetesimals. The migration rate depends on the disc mass and on its time evolution. Planets that are embedded in long-lived planetesimal discs, having total mass of $10^{-4}-0.01 M_{\odot}$, can migrate inward a large distance and can survive only if the inner disc is truncated or because of tidal interaction with the star. In this case the semi-major axis, a, of the planetary orbit is less than 0.1 AU. Orbits with larger $a$ are obtained for smaller value of the disc mass or for a rapid evolution (depletion) of the disc. This model may explain several of the orbital features of the giant planets that were discovered in last years orbiting nearby stars as well as the metallicity enhancement found in several stars associated with short-period planets.Comment: 21 pages; 6 encapsulated figures. Accepted by MNRA

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“…Corresponding variables were used for relative and center of mass coordinates in a local Cartesian coordinate system by Hornung et al (1985) (see also Stewart and Wetherill 1988) and Brophy et al (1990), but these authors did not use eccentricity or inclination vectors. As in Eq.…”

Section: Formulation For the Evolution Of Velocity Dispersionmentioning

confidence: 99%

Evolution of Particle Velocity Dispersion in a Circumplanetary Disk Due to Inelastic Collisions and Gravitational Interactions

Ohtsuki¹

1999

Icarus

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Thermal velocity equilibrium in the protoplanetary cloud

Cited by 64 publications

References 9 publications

Gravitational Stirring in Planetary Debris Disks

Gravitational Stirring in Planetary Debris Disks

Migration of giant planets in planetesimal discs

Evolution of Particle Velocity Dispersion in a Circumplanetary Disk Due to Inelastic Collisions and Gravitational Interactions

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