Nested-grid calculations of disk-planet interaction

D’Angelo, Gennaro; Henning, Thomas; Kley, W.

doi:10.1051/0004-6361:20020173

Cited by 180 publications

(207 citation statements)

References 24 publications

(48 reference statements)

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“…Indeed, hydrodynamical simulations (Lubow et al 1999;D'Angelo et al 2002) have shown that, when the planet opens a gap in the disk, the accretion rate of gas is highly reduced. However, it has also been shown (see Kley & Dirksen 2006) that when the mass of the planet becomes of the order of 3−5 M (M is the mass of Jupiter ≈318 M ⊕ ), the disk-planet system can undergo a dynamic instability, leading to a substantial increase of the accretion rate of gas.…”

Section: Migration Ratementioning

confidence: 99%

“…For example, the eccentric instability that justifies the assumption that the planetary gas accretion rate is the same as the disk accretion rate occurs only for planets larger than a certain mass (Kley & Dirksen 2006). At smaller masses, the accretion rate could be smaller (D'Angelo et al 2002). Also planet-planet interactions of several giant planets forming concurrently can have important consequences for the migration and accretion rate.…”

Section: Type II Migrationmentioning

confidence: 99%

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Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

526

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: Migration Ratementioning

confidence: 99%

Section: Type II Migrationmentioning

confidence: 99%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

2009

A&A

526

551

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show abstract

“…This migration is generally described by two different regimes that depend on the mass of the protoplanet. The first is type I migration for low-mass planets, which are too small to form a gap in the disk, and the second is type II migration for planets that open a gap (D'Angelo et al 2002). A&A 567, A121 (2014) In our previous work (e.g., Mordasini et al 2009a;Alibert et al 2011), we used the results obtained for isothermal disks reported in Tanaka et al (2002) to calculate type I migration rates.…”

Section: Introductionmentioning

confidence: 99%

Impacts of planet migration models on planetary populations

Dittkrist

Mordasini

Klahr

et al. 2014

A&A

Self Cite

120

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Context. Several recent studies have found that planet migration in adiabatic disks differs significantly from migration in isothermal disks. Depending on the thermodynamic conditions, that is, the effectiveness of radiative cooling, and on the radial surface density profile, planets migrate inward or outward. Clearly, this will influence the semimajor-axis-to-mass distribution of planets predicted by population-synthesis simulations. Aims. Our goal is to study the global effects of radiative cooling, viscous torque desaturation, gap opening, and stellar irradiation on the tidal migration of a synthetic planet population. Methods. We combined results from several analytical studies and 3D hydrodynamic simulations in a new semi-analytical migration model for the application in our planet population synthesis calculations. Results. We find a good agreement of our model with torques obtained in 3D radiative hydrodynamic simulations. A typical disk has three convergence zones to which migrating planets move from the in-and outside. This strongly affects the migration behavior of low-mass planets. Interestingly, this leads to a slow type II like migration behavior for low-mass planets captured in these zones even without an ad hoc migration rate reduction factor or a yet-to-be-defined halting mechanism. This means that the new prescription of migration that includes nonisothermal effects makes the previously widely used artificial migration rate reduction factor obsolete. Conclusions. Outward migration in parts of a disk helps some planets to survive long enough to become massive. The convergence zones lead to potentially observable accumulations of low-mass planets at certain semimajor axes. Our results indicate that more studies of the mass at which the corotation torque saturates are needed since its value has a main impact on the properties of planet populations.

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“…Grid-based hydrodynamical or smoothed particle hydrodynamical (SPH) simulations (D'Angelo et al 2002;Fouchet et al 2010), combined with follow-up radiative transfer simulations (Wolf et al 2002;Jang-Condell & Sasselov 2003;Wolf & D'Angelo 2005;Jang-Condell & Boss 2007;Jang-Condell 2009;Gonzalez et al 2010Gonzalez et al , 2012, have shown that largescale disk structures are visible through the continuum reemission and scattered light of the disk. The case of the observability of simulated line emission has been investigated A&A 549, A97 (2013) by Semenov et al (2008), Regály et al (2010), and Cleeves et al (2011).…”

Section: Introductionmentioning

confidence: 99%

Tracing large-scale structures in circumstellar disks with ALMA

Ruge

Wolf

Uribe

et al. 2013

A&A

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Context. Planets are supposed to form in circumstellar disks. The additional gravitational potential of a planet perturbs the disk and leads to characteristic structures, i.e. spiral waves and gaps, in the disk's density profile. Aims. We perform a large-scale parameter study of the observability of these planet-induced structures in circumstellar disks in the (sub)mm wavelength range for the Atacama Large (Sub)Millimeter Array (ALMA). Methods. On the basis of hydrodynamical and magneto-hydrodynamical simulations of star-disk-planet models, we calculated the disk temperature structure and (sub)mm images of these systems. These were used to derive simulated ALMA images. Because appropriate objects are frequent in the Taurus-Auriga region, we focused on a distance of 140 pc and a declination of ≈20 • . The explored range of star-disk-planet configurations consists of six hydrodynamical simulations (including magnetic fields and different planet masses), nine disk sizes with outer radii ranging from 9 AU to 225 AU, 15 total disk masses in the range between 2.67 × 10 −7 M and 4.10 × 10 −2 M , six different central stars, and two different grain size distributions, resulting in 10 000 disk models.Results. On almost all scales and in particular down to a scale of a few AU, ALMA is able to trace disk structures induced by planet-disk interaction or by the influence of magnetic fields on the wavelength range between 0.4 and 2.0 mm. In most cases, the optimum angular resolution is limited by the sensitivity of ALMA. However, within the range of typical masses of protoplanetary disks (0.1-0.001 M ) the disk mass has a minor impact on the observability. It is possible to resolve disks down to 2.67 × 10 −6 M and trace gaps induced by a planet with Mp M = 0.001 in disks with 2.67 × 10 −4 M with a signal-to-noise ratio greater than three. The central star has a major impact on the observability of gaps, as well as the considered maximum grainsize of the dust in the disk. In general, it is more likely to trace planet-induced gaps in our magnetohydrodynamical disk models, because gaps are wider in the presence of magnetic fields. We also find that zonal flows resulting from magneto-rotational instability (MRI) create gap-like structures in the disk's re-emission radiation, which are observable with ALMA. Conclusions. Through the unprecedented resolution and sensitivity of ALMA in the (sub)mm wavelength range, the expected detailed observations of planet-disk interaction and global disk structures will deepen our understanding of the planet formation and disk evolution process.

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Nested-grid calculations of disk-planet interaction

Cited by 180 publications

References 24 publications

Extrasolar planet population synthesis

Extrasolar planet population synthesis

Impacts of planet migration models on planetary populations

Tracing large-scale structures in circumstellar disks with ALMA

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