Diversity of planetary systems from evolution of solids in protoplanetary disks

Kornet, K.; Stepinski, T. F.; Rozyczka, M.

doi:10.1051/0004-6361:20011183

Cited by 56 publications

(71 citation statements)

References 20 publications

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“…In the present communication we demonstrate the difference between R sl and R evap for a broad sample of disk models analyzed by Kornet et al (2001Kornet et al ( , 2002. We identify the radial drift as the major factor responsible for the final location of the snowline, and we show how redistribution of solids can enhance the abundance of solid material leading naturally to an emergence of a giant planet formation zone.…”

Section: Introductionmentioning

confidence: 68%

An alternative look at the snowline in protoplanetary disks

Kornet

Rozyczka

Stepinski

2004

A&A

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Abstract.We have calculated an evolution of protoplanetary disk from an extensive set of initial conditions using a timedependent model capable of simultaneously keeping track of the global evolution of gas and water-ice. A number of simplifications and idealizations allows for an embodiment of gas-particle coupling, coagulation, sedimentation, and evaporation/condensation processes. We have shown that, when the evolution of ice is explicitly included, the location of the snowline has to be calculated directly as the inner edge of the region where ice is present and not as the radius where disk's temperature equals the evaporation temperature of water-ice. The final location of the snowline is set by an interplay between all involved processes and is farther from the star than implied by the location of the evaporation temperature radius. The evolution process naturally leads to an order of magnitude enhancement in surface density of icy material.

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Section: Introductionmentioning

confidence: 68%

An alternative look at the snowline in protoplanetary disks

Kornet

Rozyczka

Stepinski

2004

A&A

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“…As has been shown by Kornet et al (2001), the transition from the very early dust phase to the later planetesimal phase involves a number of coupled mechanisms of dust-dust and dustgas interactions like dust settling to the midplane, dust growth by coagulation and radial drift. This leads to a redistribution of the solids within the disk, which can in turn have important effects on planetary formation (Kornet et al 2005).…”

Section: Dust To Gas Ratio F D/g -[Fe/h]mentioning

confidence: 86%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

533

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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“…The second contribution to the radial velocity is produced by the accretion of the gas. This part of the radial velocity is calculated as follows (Kornet et al 2001)…”

Section: Relative Velocitiesmentioning

confidence: 99%

The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals?

Zsom¹,

Ormel²,

Güttler³

et al. 2010

A&A

511

522

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Context. The sticking of micron-sized dust particles caused by surface forces within circumstellar disks is the first stage in the production of asteroids and planets. The key components describing this process are the relative velocity between the dust particles in this environment and the complex physics of dust aggregate collisions. Aims. We present the results of a collision model based on laboratory experiments of these aggregates. We investigate the maximum aggregate size and mass that can be reached by coagulation in protoplanetary disks. Methods. We use the results of laboratory experiments to establish the collision model previously published by Güttler et al. The collision model is based on the assumptions that we model the aggregates as spheres with compact and porous "phases" and that there is a continuous transition between these two. We apply this collision model to the Monte Carlo method developed previously by Zsom & Dullemond and include Brownian motion, radial drift, and turbulence as contributors of relative velocity between dust particles. Results. We model the growth of dust aggregates at 1 AU in the midplane for three different gas densities. We find that the evolution of the dust does not follow the previously assumed growth-fragmentation cycles. Catastrophic fragmentation hardly occurs in the three disk models. Furthermore, we see long-lived, quasi-steady states in the distribution function of the aggregates caused by bouncing. We explore how the mass and the porosity depend on both the turbulence parameter and the critical mass ratio of dust particles. Upon varying the turbulence parameter, the system behaves in a non-linear way, and we find that the critical mass ratio has a strong effect on the particle sizes and masses. Particles reach Stokes numbers of roughly 10 −4 during the simulations. Conclusions. The particle growth is stopped by bouncing rather than fragmentation in these models. The final Stokes number of the aggregates is rather insensitive to the variations in the gas density and the strength of turbulence. The maximum mass of the particles is limited to ≈1 g (chondrule-sized particles). Planetesimal formation can proceed by the means of the turbulent concentration of these aerodynamically size-sorted, chondrule-sized particles.

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Diversity of planetary systems from evolution of solids in protoplanetary disks

Cited by 56 publications

References 20 publications

An alternative look at the snowline in protoplanetary disks

An alternative look at the snowline in protoplanetary disks

Extrasolar planet population synthesis

The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals?

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