Accretional Evolution of a Planetesimal Swarm

Weidenschilling, S. J.; Spaute, D.; Davis, Donald R.; Marzari, F.; Ohtsuki, Keiji

doi:10.1006/icar.1997.5747

Cited by 311 publications

(316 citation statements)

References 40 publications

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“…Thus, as confirmed by many different numerical simulations (e.g. Weidenschilling et al 1997;Kokubo & Ida 2000), runaway bodies emerge with relative separations of their semimajor axis Δ proportional to their semimajor axes a, so Δ/a = const. This situation also prevails later during oligarchic growth stages, although the numerical value of B L increases (Ida & Lin 2004a).…”

Section: Embryo Start Position a Startmentioning

confidence: 59%

“…The initial solid surface density is given by (Hayashi 1981;Weidenschilling et al 1997) where f D/G is the dust-to-gas ratio of the disk, and f R/I is a factor describing the degree of condensation of ices. Its value is set to 1/4 in the regions of the disk for which the initial mid-plane temperature exceeds the sublimation of water ice (T mid > 170 K), and 1 otherwise.…”

Section: Disk Structure and Evolutionmentioning

confidence: 99%

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Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

525

551

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Context. With the high number of extrasolar planets discovered by now, it has become possible to use the properties of this planetary population to constrain theoretical formation models in a statistical sense. This paper is the first in a series in which we carry out a large number of planet population synthesis calculations within the framework of the core accretion scenario. We begin the series with a paper mainly dedicated to the presentation of our approach, but also the discussion of a representative synthetic planetary population of solar like stars. In the second paper we statistically compare the subset of detectable planets to the actual extrasolar planets. In subsequent papers, we shall extend the range of stellar masses and the properties of protoplanetary disks. Aims. The last decade has seen a large observational progress in characterizing both protoplanetary disks, and extrasolar planets. Concurrently, progress was made in developing complex theoretical formation models. The combination of these three developments allows a new kind of study: the synthesis of a population of planets from a model, which is compared with the actual population. Our aim is to obtain a general overview of the population, to check if we quantitatively reproduce the most important observed properties and correlations, and to make predictions about the planets that are not yet observable. Methods. Based as tightly as possible on observational data, we have derived probability distributions for the most important initial conditions for the planetary formation process. We then draw sets of initial conditions from these distributions and obtain the corresponding synthetic planets with our formation model. By repeating this step many times, we synthesize the populations. Results. Although the main purpose of this paper is the description of our methods, we present some key results: we find that the variation of the initial conditions in the limits occurring in nature leads to the formation of planets of wide diversity. This formation process is best visualized in planetary formation tracks in the mass-semimajor axis diagram, where different phases of concurrent growth and migration can be identified. These phases lead to the emergence of sub-populations of planets distinguishable in a mass-semimajor axis diagram. The most important ones are the "failed cores", a vast group of core-dominated low mass planets, the "horizontal branch", a sub-population of Neptune mass planets extending out to 6 AU, and the "main clump", a concentration of giant gaseous planets at around 0.3−2 AU.

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Section: Embryo Start Position a Startmentioning

confidence: 59%

Section: Disk Structure and Evolutionmentioning

confidence: 99%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

525

551

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“…There is now some consensus that planetary embryos of isolation mass M i \ where is the surface density of 4[(na2p M *)3/(3M _ )]1@2, p M embryos and * is their orbital spacing in mutual Hill radii form in D106 yr near 1 AU (e.g., Lissauer 1987). Recent N-body (Kokubo & Ida 1998) and multizone (Weidenschilling et al 1997) simulations of embryo formation indicate that at the end of the middle stage, embryos have spacings of * D 8È10. Within the context of the standard model, the time required to complete the Ðrst two stages (i.e., planetesimal formation and the runaway growth of planetary embryos) is short relative to the nebular lifetime.…”

Section: Discussionmentioning

confidence: 99%

Damping of Terrestrial‐Planet Eccentricities by Density‐Wave Interactions with a Remnant Gas Disk

Agnor

Ward

2002

ApJ

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We examine the damping of terrestrial-planet eccentricities via density-wave interactions with a remnant gas disk that postdated the accretionary epoch. A lower limit is estimated for the gas surface density present in the terrestrial zone required for acoustic damping to be e †ective, and a simple model for describing the diskÏs inÑuence on the planet eccentricities is presented. The results suggest that the terrestrial-planet eccentricities could be reduced from values permitting crossing orbits to the present-day values by a remnant disk with gas surface density of D10~3È10~4 times the minimum-mass solar nebula value and characteristic gas dissipation timescales of 106È107 yr.

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“…strongly nonlinear. This is the case in the so-called runaway growth regime, where massive bodies grow quicker than small ones, so that these runaway bodies detach from the remaining population of small planetesimals (Weidenschilling et al, 1997). However, with increasing mass, these big bodies start to increase the random velocities of the small ones, so that the growth becomes slower, and the mode changes to the so-called oligarchic mode, where the big bodies grow in lockstep (Ida and Makino, 1993).…”

Section: From Planetesimals To Protoplanetsmentioning

confidence: 99%

Circumstellar disks and planets

Wolf

Malbet

Alexander

et al. 2012

Astron Astrophys Rev

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We present a review of the interplay between the evolution of circumstellar disks and the formation of planets, both from the perspective of theoretical models and dedicated observations. Based on this, we identify and discuss fundamental questions concerning the formation and evolution of circumstellar disks and planets which can be addressed in the near future with optical and infrared long-baseline interferometers. Furthermore, the importance of complementary observations with long-baseline (sub)millimeter interferometers and high-sensitivity infrared observatories is outlined.

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Accretional Evolution of a Planetesimal Swarm

Cited by 311 publications

References 40 publications

Extrasolar planet population synthesis

Extrasolar planet population synthesis

Damping of Terrestrial‐Planet Eccentricities by Density‐Wave Interactions with a Remnant Gas Disk

Circumstellar disks and planets

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