THREE-DIMENSIONAL HYDRODYNAMIC BONDI-HOYLE ACCRETION. IV. SPECIFIC HEAT RATIO 4/3.

Details THREE-DIMENSIONAL HYDRODYNAMIC BONDI-HOYLE ACCRETION. IV. SPECIFIC HEAT RATIO 4/3. THREE-DIMENSIONAL HYDRODYNAMIC BONDI-HOYLE ACCRETION. IV. SPECIFIC HEAT RATIO 4/3.

1995-03-06

arxiv.org/abs/astro-ph/9503026v1

Astron.Astrophys.Suppl.Ser.113:133,1995

Astronomy and Astrophysics

Astrophysics

uuencoded compressed postscript. 12 pages. includes some figures.

Scientific paper

We investigate the hydrodynamics of three-dimensional classical Bondi-Hoyle accretion. A totally absorbing sphere of different sizes (1, 0.1 and 0.02 accretion radii) exerts gravity on and moves at different Mach numbers (0.6, 1.4, 3.0 and 10) relative to a homogeneous and slightly perturbed medium, which is taken to be an ideal gas ($\gamma=4/3$). We examine the influence of Mach number of the flow and size of the accretor upon the physical behaviour of the flow and the accretion rates. The hydrodynamics is modeled by the ``Piecewise Parabolic Method'' (PPM). The resolution in the vicinity of the accretor is increased by multiply nesting several $32^3$-zone grids around the sphere, each finer grid being a factor of two smaller in zone dimension than the next coarser grid. This allows us to include a coarse model for the surface of the accretor (vacuum sphere) on the finest grid while at the same time evolving the gas on the coarser grids. For small Mach numbers (0.6 and~1.4) the flow patterns tend towards a steady state, while in the case of supersonic flow (Mach~3 and~10) and small enough accretors, (radius of~0.1 and~0.02 accretion radii) an unstable Mach cone develops, destroying axisymmetry. Our 3D models do not show the highly dynamic flip-flop flow so prominent in 2D calculations performed by other authors. In the gamma=4/3 models, the shock front remains closer to the accretor and the mass accretion rates are higher than in the gamma=5/3 models, whereas the rms of the specific angular momentum accreted does not change.

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