Cloud virial parameters rise by about a factor of 2 from 4 to 15 kpc, fitting a pressure-bounded equilibrium model dominated by nearby stars, with star formation proceeding in small cores (mass fraction ~1e-3) rather than global collapse.
# is often used to quantify the ability of a cloud to form stars. This section relates the observed and modeled values of 饾浖!
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Gravitational Binding and Star Formation in Molecular Clouds of the Milky Way
Cloud virial parameters rise by about a factor of 2 from 4 to 15 kpc, fitting a pressure-bounded equilibrium model dominated by nearby stars, with star formation proceeding in small cores (mass fraction ~1e-3) rather than global collapse.