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Bodo G, Mignone A, Rosner R. Kelvin-Helmholtz instability for relativistic fluids. Phys Rev E Stat Nonlin Soft Matter Phys. 2004;70(3):036304doi: 10.1103/PhysRevE.70.036304.
Bodo, G., Mignone, A., & Rosner, R. (2004). Kelvin-Helmholtz instability for relativistic fluids. Physical review. E, Statistical, nonlinear, and soft matter physics, 70(3), 036304. https://doi.org/10.1103/PhysRevE.70.036304
Bodo, G, et al. "Kelvin-Helmholtz instability for relativistic fluids." Physical review. E, Statistical, nonlinear, and soft matter physics vol. 70,3 (2004): 036304. doi: https://doi.org/10.1103/PhysRevE.70.036304
Bodo G, Mignone A, Rosner R. Kelvin-Helmholtz instability for relativistic fluids. Phys Rev E Stat Nonlin Soft Matter Phys. 2004 Sep;70(3):036304. doi: 10.1103/PhysRevE.70.036304. Epub 2004 Sep 13. PMID: 15524630.
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Phys Rev E Stat Nonlin Soft Matter Phys. 2004 Sep;70(3):036304. doi: 10.1103/PhysRevE.70.036304. Epub 2004 Sep 13.

Kelvin-Helmholtz instability for relativistic fluids.

Physical review. E, Statistical, nonlinear, and soft matter physics

G Bodo, A Mignone, R Rosner

Affiliations

  1. INAF Osservatorio Astronomico di Torino, Strada Osservatorio 20, I-10025 Pino Torinese, Italy.

PMID: 15524630 DOI: 10.1103/PhysRevE.70.036304

Abstract

We reexamine the stability of an interface separating two nonmagnetized relativistic fluids in relative motion, showing that, in an appropriate reference frame, it is possible to find analytic solutions to the dispersion relation. Moreover, we show that the critical value of the Mach number, introduced by compressibility, is unchanged from the nonrelativistic case if we redefine the Mach number as M= [beta/ (1- beta(2) )(1/2) ] [ beta(s) / (1- beta(2)(s) )(1/2) ](-1) , where beta and beta(s) are, respectively, the speed of the fluid and the speed of sound (in units of the speed of light).

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