2008A&A...483..633P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST13:44:27

2008A&A...483..633P - Astronomy and Astrophysics, volume 483, 633-642 (2008/5-4)

On the formation and migration of giant planets in circumbinary discs.

PIERENS A. and NELSON R.P.

Abstract (from CDS):

We present the results of hydrodynamic simulations of the formation and subsequent orbital evolution of giant planets embedded in a circumbinary disc. The aim is to examine whether or not giant planets can be found to orbit stably in close binary systems. We performed numerical simulations using a grid-based hydrodynamics code. We assume that a 20M core has migrated to the edge of the inner cavity formed by the binary where it remains trapped by corotation torques. This core is then allowed to accrete gas from the disc, and we study its orbital evolution as it grows in mass. For each of the two accretion time scales we considered, we performed three simulations. In two of the three simulations, we stopped the accretion onto the planet once its mass became characteristic of that of Saturn or Jupiter. In the remaining case, the planet accreted disc material freely in such a way that its mass became higher than Jupiter's. The simulations show different outcomes depending on the final mass mp of the giant. For mp=1MS (where MS is Saturn's mass), we find that the planet migrates inward through its interaction with the disc until its eccentricity becomes high enough to induce a torque reversal. The planet then migrates outward, and the system remains stable on long time scales. For mp≥1MJ (where MJ is Jupiter's mass) we observed two different outcomes. In each case the planet enters the 4:1 resonance with the binary, and resonant interaction drives up the eccentricity of the planet until it undergoes a close encounter with the secondary star, leading to scattering. The result can either be ejection from the system or scattering out into the disc followed by a prolonged period of outward migration. These results suggest that circumbinary planets are more likely to be quite common in the Saturn-mass range. Jupiter-mass circumbinary planets are likely to be less common because of their less stable evolution, but if present are likely to orbit at large distances from the central binary.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - planets and satellites: formation - stars: binaries: close - hydrodynamics - methods: numerical

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 13445 PM* 02 10 25.9190575041 -50 49 25.467227759   6.94 6.17     K1.5V 414 2
2 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 647 1
3 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 286 0
4 V* GW Ori Or* 05 29 08.3925564419 +11 52 12.653756566   10.83 10.10 9.52   G5/8Ve 299 0
5 HD 41004 ** 05 59 49.6473573887 -48 14 22.805780232   9.49 8.65     K1IV 151 1
6 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 269 2
7 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 235 1
8 HD 202206 PM* 21 14 57.7684954746 -20 47 21.162361638   8.79 8.07     G6V 192 1
9 * gam Cep SB* 23 39 20.9015326708 +77 37 56.505477975 5.190 4.250   2.6   K1III-IVCN1 547 1

    Equat.    Gal    SGal    Ecl

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2020.07.03-13:44:27

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