Planet Formation is Unlikely in Equal-Mass Binary Systems with [CLC][ITAL]a[/ITAL][/CLC] ∼ 50 AU

Nelson, Andrew F.

doi:10.1086/312752

Cited by 152 publications

(258 citation statements)

References 27 publications

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“…Problems could also arise at even earlier stages. Nelson (2000) has for instance shown that, under certain conditions, thermal energy dissipation in gas disks for equal mass binaries could inhibit dust coagulation by raising temperatures above vaporization limit. But, as recognized by the author himself, these results are still preliminary, and a complete study of this problem, taking into account a broader range of physical parameters, has yet to be carried out.…”

Section: Do Planetesimals Really Form?mentioning

confidence: 99%

Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Thébault

Marzari

Scholl

2006

Icarus

158

294

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We investigate classical planetesimal accretion in a binary star system of separation a b ≤50 AU by numerical simulations, with particular focus on the region at a distance of 1 AU from the primary. The planetesimals orbit the primary, are perturbed by the companion and are in addition subjected to a gas drag force. We concentrate on the problem of relative velocities ∆v among planetesimals of different sizes. For various stellar mass ratios and binary orbital parameters we determine regions where ∆v exceed planetesimal escape velocities v esc (thus preventing runaway accretion) or even the threshold velocity v ero for which erosion dominates accretion. Gaseous friction has two crucial effects on the velocity distribution: it damps secular perturbations by forcing periastron alignment of orbits, but at the same time the size-dependence of this orbital alignment induces a significant ∆v increase between bodies of different sizes. This differential phasing effect proves very efficient and almost always increases ∆v to values preventing runaway accretion, except in a narrow e b ≃ 0 domain. The erosion threshold ∆v > v ero is reached in a wide (a b , e b ) space for small < 10 km planetesimals, but in a much more limited region for bigger ≃ 50 km objects. In the intermediate v esc < ∆v < v ero domain, a possible growth mode would be the type II runaway growth identified by Kortenkamp et al. (2001).

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Section: Do Planetesimals Really Form?mentioning

confidence: 99%

Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Thébault

Marzari

Scholl

2006

Icarus

158

294

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“…A stellar companion within 100 AU probably affects the formation of giant planets (e.g., Nelson 2000;Mayer et al 2005;Thébault et al 2006;and others).…”

Section: Introductionmentioning

confidence: 99%

Mean motion resonances and the stability of a circumbinary disk in a triple stellar system

Domingos

Winter

Carruba

2012

A&A

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“…Its shape is expected to be elliptic with varying eccentricity Paardekooper et al 2008;Kley & Nelson 2008). Both these features may alter the dust sedimentation process on the mid plane of the disk and the grain accumulation into planetesimals which might even be inhibited (Nelson 2000). More eccentric trajectories of the grains, dragged by the gas, increase the impact rate but, on the other hand, might lead to destructive collisions by increasing the relative velocity.…”

Section: Introductionmentioning

confidence: 99%

On the eccentricity of self-gravitating circumstellar disks in eccentric binary systems

Marzari¹,

Scholl

Thébault

2009

A&A

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Aims. We study the evolution of circumstellar massive disks around the primary star of a binary system focusing on the computation of disk eccentricity. In particular, we concentrate on its dependence on the binary eccentricity. Self-gravitation is included in our numerical simulations. Our standard model assumes a semimajor axis for the binary of 30 AU, the most probable value according to the present binary statistics. Methods. Two-dimensional hydrodynamical computations are performed with FARGO. Besides the dynamical standard method to determine disk eccentricities, we apply a morphological method which may allow a better comparison with observations. Results. Self-gravitation leads to disks that, on average, have low eccentricity. Moreover, the orientation of the disk computed with the standard dynamical method always librates instead of circulating as in simulations without self-gravitation. The disk eccentricity decreases with the binary eccentricity, a result found also in models without self-gravitation. Conclusions. Disk self-gravitation appears to be an important factor in determining the evolution of a massive disk in a binary system. High eccentricity binaries are not necessarily a hostile environment for planetary accretion.

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Planet Formation is Unlikely in Equal-Mass Binary Systems with [CLC][ITAL]a[/ITAL][/CLC] ∼ 50 AU

Cited by 152 publications

References 27 publications

Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Relative velocities among accreting planetesimals in binary systems: The circumprimary case

Mean motion resonances and the stability of a circumbinary disk in a triple stellar system

On the eccentricity of self-gravitating circumstellar disks in eccentric binary systems

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