Issue |
A&A
Volume 387, Number 2, May IV 2002
|
|
---|---|---|
Page(s) | 605 - 623 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20020240 | |
Published online | 13 May 2002 |
The co-orbital corotation torque in a viscous disk: Numerical simulations
Service d'Astrophysique, L'Orme des Merisiers, CE-Saclay, 91191 Gif-sur-Yvette Cedex, France
Corresponding author: fmasset@cea.fr
Received:
26
September
2001
Accepted:
5
February
2002
The torque felt by a non-accreting protoplanet on a
circular orbit embedded in a uniform surface density protoplanetary disk is analyzed by
means of time-dependent numerical
simulations. Varying the viscosity enables one to disentangle the Lindblad
torque (which is independent of viscosity) from the corotation torque,
which saturates at low viscosity and is unsaturated at high viscosity.
The dependence of the corotation torque upon the viscosity and upon the
width of the librating zone is compared with
previous analytical expressions, and shown to be in agreement with
those. The effect of the potential smoothing respectively on the Lindblad
torque and on the corotation torque is investigated, and the question of whether
3D effects and their impact on the total torque sign and magnitude can be
modeled by an adequate smoothing prescription in a 2D simulation is addressed.
As a side result, this study shows that the total torque acting on a Neptune-sized protoplanet
is positive in a
sufficiently thin,
viscous disk (%,
), but the inward migration time of smaller
bodies is still very short, making it unlikely that they reach the torque reversal mass before
having migrated all the way to the central object.
Key words: stars: planetary systems: formation / stars: planetary systems: protoplanetary disks / stars: planetary systems / hydrodynamics / methods: numerical
© ESO, 2002
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