Nonlinear instability of the accretion line

Journal Article · Thu Aug 01 04:00:00 EDT 1991 · Astrophysical Journal; (United States)

DOI:https://doi.org/10.1086/170322· OSTI ID:5184770

Soker, N ^[1]

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1. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)

The instability of the flow along the accretion line in the two-dimensional Bondi-Hoyle-Lyttleton type accretion flow is studied. By means of numerical simulations, the nonlinear regime of the instability is explored, thus extending a previous work that dealt with the linear regime using the WKB approximation. In contrast to the behavior in the linear regime, in the nonlinear regime the radial and tangential modes are coupled. The radial instability, which manifests itself as large density and velocity variations on short distances, grows far beyond the linear regime. The tangential instability, on the other hand, stays in the linear regime and is dominant by long-wavelength perturbations. This results from both the influence of the radial instability and the incoming material (the material accreted onto the accretion line). 17 refs.

• OSTI ID: 5184770
• Journal Information: Astrophysical Journal; (United States), Journal Name: Astrophysical Journal; (United States) Vol. 376; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ACCRETION DISKS
FLUID MECHANICS
HYDRODYNAMICS
INSTABILITY
MAGNETOHYDRODYNAMICS
MATHEMATICAL MODELS
MATHEMATICS
MECHANICS
NONLINEAR PROBLEMS
NUMERICAL ANALYSIS
STABILITY
WKB APPROXIMATION