.png){kind=icon}
.png){kind=icon}
Return
The Santa Barbara Binary-disk Code Comparison
.png){kind=icon}
OA
AI
DOI：10.3847/1538-4357/ad5a7e.png)
.png){kind=icon}
Original request for help.png){kind=icon}
Share.png){kind=icon}
Save
Abstract
En 中文
We have performed numerical calculations of a binary interacting with a gas disk, using 11 different numerical methods and a standard binary-disk setup. The goal of this study is to determine whether all codes agree on a numerically converged solution and to determine the necessary resolution for convergence and the number of binary orbits that must be computed to reach an agreed-upon relaxed state of the binary-disk system. We find that all codes can agree on a converged solution (depending on the diagnostic being measured). The zone spacing required for most codes to reach a converged measurement of the torques applied to the binary by the disk is roughly 1% of the binary separation in the vicinity of the binary components. For our disk model to reach a relaxed state, codes must be run for at least 200 binary orbits, corresponding to about a viscous time for our parameters, 0.2(a 2 Omega B /nu) binary orbits, where nu is the kinematic viscosity. The largest discrepancies between codes resulted from the dimensionality of the setup (3D vs. 2D disks). We find good agreement in the total torque on the binary between codes, although the partition of this torque between the gravitational torque, orbital accretion torque, and spin accretion torque depends sensitively on the sink prescriptions employed. In agreement with previous studies, we find a modest difference in torques and accretion variability between 2D and 3D disk models. We find cavity precession rates to be appreciably faster in 3D than in 2D.
Keywords:
BLACK-HOLE ACCRETION
CIRCUMBINARY DISCS
MASS-RATIO
ORBITAL EVOLUTION
MAGNETOHYDRODYNAMICS CODE
ECCENTRIC BINARIES
SIMULATIONS
DYNAMICS
VARIABILITY
DRIVEN
Journal
IF:
5.4
Papers:
8.3W
Citations:
32.0W
Organization
View more organizations