Spiral Structure in IP Peg: Confronting Theory and Observations
Astrophysics
2016-01-27 v2
Abstract
The first convincing piece of evidence of spiral structure in the accretion disc in IP Pegasi was found by Steeghs et al. (1997). We performed two kinds of 2D hydrodynamic simulations, a SFS finite volume scheme and a SPH scheme, with a mass ratio of 0.5. Both results agreed well with each other. We constructed Doppler maps and line flux-binary phase relations based on density distributions, the results agreeing well with those obtained by observation.
Cite
@article{arxiv.astro-ph/9807239,
title = {Spiral Structure in IP Peg: Confronting Theory and Observations},
author = {Takuya Matsuda and Makoto Makita and Hiroshi Yukawa and Henri M. J. Boffin},
journal= {arXiv preprint arXiv:astro-ph/9807239},
year = {2016}
}
Comments
4 pages, LaTeX with 2 ps figures using crckapb.sty. To appear in the Proceedings of Numerical Astrophysics 1998, Tokyo, Japan, 10-13 March, 1998, eds. S. M. Miyama, K. Tomisaka and T. Hanawa (Kluwer Academic Publishers)