Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245..927w&link_type=abstract
Astrophysical Journal, Part 1, vol. 245, May 1, 1981, p. 927-933.
Astronomy and Astrophysics
Astrophysics
13
Gravitational Effects, Interstellar Gas, Perturbation Theory, Shock Waves, Star Formation, Cylindrical Shells, Hydrostatics, Protostars, Radiation Pressure, Taylor Instability, Viscosity
Scientific paper
The possibility of star formation in a curved self-gravitating gas layer formed behind an interstellar shock is considered. Following a brief review of the results obtained by Elmegreen and Elmegreen (1978) for the case of a plane-parallel gas layer of infinite extent, which resulted in conditions for star formation, attention is given to the stability of a pressure-bounded, cylindrical sheath of self-gravitating gas, extending to infinity along the cylinder axis. Analysis of perturbations around the hydrostatic equilibrium of such a gas reveals the presence of self-made Rayleigh-Taylor instabilities which give rise to the growth of perturbations at all wavelengths, with the smallest modes growing fastest. The instabilities would then act to break the layer into fragments too small to collapse further, despite the influences of viscosity within the gas layer or strong radiation pressure from a central object.
Schmid-Burgk Johannes
Welter Gary
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