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We analyze the physical parameters of interstellar filaments that we describe by an idealized model of isothermal self-gravitating infinite cylinder in pressure equilibrium with the ambient medium. Their gravitational state is characterized by the ratio fcyl of their mass line density to the maximum possible value for a cylinder in a vacuum. Equilibrium solutions exist only for fcyl 0.5 the instabilities should promote core formation through compression, with a separation of about five times the FWHM. We discuss the nature of filaments with high mass line densities and their relevance to gravitational fragmentation and star formation.
Fischera et al. (Sat,) studied this question.