2008/12/02 by S. Li, Shengtai Li, M. J. Buoni +3 · 2 citations
Engineering · Physics and Astronomy · #Adhesion, Friction, and Surface Interactions #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1088/0067-0049/181/1/244
8 figures, accepted to ApJS
arxiv created 2008/12/02 · openalex publication_date 2009/03/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Disk self-gravity could play an important role in the dynamic evolution of interaction between disks and embedded protoplanets. We have developed a fast and accurate solver to calculate the disk potential and disk self-gravity forces for disk systems on a uniform polar grid. Our method closely follows the method given by Chan et al., in which a fast Fourier transform in the azimuthal direction is performed and a direct integral approach in the frequency domain in the radial direction is implemented on a uniform polar grid. This method can be very effective for disks with vertical structures that depend only on the disk radius, achieving the same computational efficiency as for zero-thickness disks. We describe how to parallelize the solver efficiently on distributed parallel computers. We propose a mode-cutoff procedure to reduce the parallel communication cost and achieve nearly linear scalability for a large number of processors. For comparison, we have also developed a particle-based fast tree code to calculate the self-gravity of the disk system with a vertical structure. The numerical results show that our direct integral method is at least two orders of magnitude faster than our optimized tree-code approach.