Non-axisymmetric instability in three-dimensional accretion toroids

Details Non-axisymmetric instability in three-dimensional accretion toroids Non-axisymmetric instability in three-dimensional accretion toroids

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231..739b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, April 1, 1988, p. 739-764.

Statistics

Computation

7

Accretion Disks, Black Holes (Astronomy), Finite Difference Theory, Molecular Clouds, Solar Corona, Toroids, Angular Momentum, Computational Astrophysics, Interstellar Magnetic Fields, Perturbation Theory, Time Dependence

Scientific paper

A finite-difference numerical code is used to study the non-linear evolution of low m, non-axisymmetric density perturbations [exp(imφ)] in the Papaloizou-Pringle accretion toroid. The calculations are both time-dependent and fully three-dimensional in space. The toroids studied include thin and narrow as well as thick and wide toroids with constant specific angular momentum [q = 2, where the angular velocity Ω(R) = Ω0(R/R0)-q and R is the cylindrical radius], and a toroid with Keplerian specific angular momentum (q = 3/2). The results are most applicable to hot accretion discs surrounding massive objects, and are not applicable to models of the solar nebula because of fundamental differences in the thermodynamics.

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