Numerical study of the non-linear stage of thermal instability in cooling flows. II - The non-linear perturbation in the case of a spherically symmetric background flow

Details Numerical study of the non-linear stage of thermal instability in cooling flows. II - The non-linear perturbation in the case of a spherically symmetric background flow Numerical study of the non-linear stage of thermal instability in cooling flows. II - The non-linear perturbation in the case of a spherically symmetric background flow

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.248..630y&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 248, Feb. 15, 1991, p. 630-641.

Statistics

Computation

14

Computational Astrophysics, Cooling Flows (Astrophysics), Perturbation Theory, Thermal Instability, Flow Stability, Interstellar Magnetic Fields, Mathematical Models, Nonlinear Equations, Vortices

Scientific paper

Two-dimensional numerical hydrodynamical calculations of thermal instability in cooling flows in a spherical coordinate system are performed in order to investigate the evolution of the nonlinear axisymmetric perturbation. If the relative density contrast is smaller than the critical value the perturbation decays, due to the formation of the vortex ring before the perturbation cools. One-dimensional spherically symmetric calculations are carried out and show that even if the density contrast is smaller than the critical value, in the case of the spherically symmetric perturbation it can cool. Numerical results show that the nonradial motion is very important for the evolution of the nonlinear perturbation. The criterion for the amplitude and size of perturbations which are thermally unstable are given. It is shown that only if the density contrast of the perturbation is very large, can the thermal instability develop in the spherically symmetric background cooling flow. These results indicate that the apparently pervasive and extensive mass desposition occurring in real cooling flows remains unexplained and what makes thermal instability occur, for example a magnetic field, may be needed.

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