Physics
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..239i&link_type=abstract
Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam
Physics
Scientific paper
We developed the SPH method to calculate long-term evolution of a rotating gaseous disk, with two-dimensional thin-disk approximation, without self-gravity of the disk. For example, in a calculation of gas capturing process by Jupiter in the protoplanetary disk, we need to follow the dynamical evolution for many tens of Keplerian time scale. To obtain a quantitatively meaningful result in such calculations, we should minimize the numerical shear viscosity. However, the standard SPH produces false evolution, even in the simplest test calculation where fluid elements are rotating on a circular orbit in steady stable state under axisymmetric gravitational potential. Large numerical shear viscosity causes unphysical angular momentum transfer and the density distribution changes largely within a few dynamical time scale. This problem always arises in a system with strong shear motion. To handle this problem, Taylor-series expansion of physical variables is applied around each particles and the interpolated values of physical variables are summed up around them with certain weighting function. Through these procedures, we can obtain the distribution of physical variables and their derivatives precisely at any point in space. This enable us to calculate accurately the angular momentum transfer due to waves with small amplitudes.
Imaeda Yusuke
Inutsuka Shu-ichiro
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