2007A&A...472..993P


Query : 2007A&A...472..993P

2007A&A...472..993P - Astronomy and Astrophysics, volume 472, 993-1001 (2007/9-4)

On the migration of protoplanets embedded in circumbinary disks.

PIERENS A. and NELSON R.P.

Abstract (from CDS):

We present the results of hydrodynamical simulations of low mass protoplanets embedded in circumbinary accretion disks. The aim is to examine the migration and long term orbital evolution of the protoplanets, in order to establish the stability properties of planets that form in circumbinary disks. Simulations were performed using a grid-based hydrodynamics code. First we present a set of calculations that study how a binary interacts with a circumbinary disk. We evolve the system for ∼105 binary orbits, which is the time needed for the system to reach a quasi-equilibrium state. From this time onward the apsidal lines of the disk and the binary are aligned, and the binary eccentricity remains essentially unchanged with a value of eb∼0.08. Once this stationary state is obtained, we embed a low mass protoplanet in the disk and let it evolve under the action of the binary and disk forces. We consider protoplanets with masses of mp=5, 10 and 20M. In each case, we find that inward migration of the protoplanet is stopped at the edge of the tidally truncated cavity formed by the binary. This effect is due to positive corotation torques, which can counterbalance the net negative Lindblad torques in disk regions where the surface density profile has a sufficiently large positive gradient. Halting of migration occurs in a region of long-term stability, suggesting that low mass circumbinary planets may be common, and that gas giant circumbinary planets should be able to form in circumbinary disks.

Abstract Copyright:

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

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 13445 PM* 02 10 25.9181700303 -50 49 25.465181208   6.945 6.117     K1.5V 438 1
2 V* GG Tau Or* 04 32 30.3506925552 +17 31 40.494063144 14.84 14.78 13.40 11.54   M0e+M2.0e 708 1
3 V* DQ Tau Or* 04 46 53.0575226016 +17 00 00.136127304 14.56 13.67 12.00 13.21   M1Ve 319 0
4 V* GW Ori Or* 05 29 08.3928710640 +11 52 12.666457092   10.83 10.10 9.52   G5/8Ve 339 0
5 HD 41004 ** 05 59 49.6501762752 -48 14 22.888358520   9.49 8.65     K1IV 171 1
6 V* SU UMa CV* 08 12 28.2695986944 +62 36 22.427676396           B2 490 0
7 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 287 2
8 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 259 1
9 HD 202206 PM* 21 14 57.7686051936 -20 47 21.161521320   8.79 8.07     G6V 219 1
10 * gam Cep SB* 23 39 20.9104133784 +77 37 56.510781384 5.190 4.250   2.6   K1III-IVCN1 579 1

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2023.02.02-18:27:27

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