Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pasj...54..781b&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.54, No.5, pp.781-785
Astronomy and Astrophysics
Astronomy
4
Accretion, Accretion Disks, Methods: Numerical, Shock Waves, Stars: Binary: Close, Stars: Cataclysmic Variables
Scientific paper
Spiral structures and shocks often appear in astrophysical gas dynamics and particular in accretion-disc simulations; however, they are difficult to follow numerically. In this paper we consider a black hole of 8 Msolar as a primary and a small secondary of 0.5 Msolar , following the idea that a low M2/M1 would favour spiral structure and possibly spiral shock onset through gas compression induced by strong gravitational attraction. In the framework of Smooth Particle Hydrodynamics (SPH), we performed two 2D models and two 3D models. Simulations in either pair are distinguished by the adopted γ value (low and high compressibility cases). Indeed, both 2D models reveal the existence of spiral structures in the disc bulk. Furthermore, spiral shocks at the outer disc edge are evident for the high compressibility 2D model. Spiral structures appear to develop also for the 3D high compressibility model. Instead, for the 3D low compressibility model, no clear conclusion can be drawn as the number of particles (and thus the SPH resolution) is low.
Belvedere Gaetano
Lanzafame Giuseppe
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