Spiral Structure in IP Peg: Confronting Theory and Observations

Takuya Matsuda; Makoto Makita; Hiroshi Yukawa; Henri M. J. Boffin

doi:10.1007/978-94-011-4780-4_64

paper

Spiral Structure in IP Peg: Confronting Theory and Observations

arXiv:astro-ph/9807239 · doi:10.1007/978-94-011-4780-4_64

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.

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)