Rayleigh-Taylor instability of a self-similar spherical expansion

Details Rayleigh-Taylor instability of a self-similar spherical expansion Rayleigh-Taylor instability of a self-similar spherical expansion

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...225..633b&link_type=abstract

Astrophysical Journal, Part 1, vol. 225, Oct. 15, 1978, p. 633-640. Research supported by the U.S. Department of Energy and U.S

Astronomy and Astrophysics

Astrophysics

35

Gas Expansion, Isentropic Processes, Pulsars, Radiation Pressure, Stellar Models, Symmetrical Bodies, Taylor Instability, Gas Dynamics, Spheres, Stellar Envelopes

Scientific paper

The self-similar motion of a spherically symmetric isentropic cloud of ideal gas driven outward by an expanding low-density medium (e.g., radiation pressure from a pulsar) is shown to be unstable to Rayleigh-Taylor modes which develop in the neighborhood of the interface. A complete solution of the linearized equations of motion is obtained. The implications for astrophysical phenomena are discussed.

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