Variation of the Core Lifetime and Fragmentation Scale in Molecular Clouds as an Indication of Ambipolar Diffusion

Abstract

Ambipolar diffusion likely plays a pivotal role in the formation and evolution of dense cores in weakly-ionized molecular clouds. Linear analyses show that the evolutionary times and fragmentation scales are significantly greater than the hydrodynamic (Jeans) values even for clouds with mildly supercritical mass-to-flux ratio. We utilize values of fragmentation scales and growth times that correspond to typical ionization fractions within a molecular cloud, and apply to the context of the observed estimated lifetime of prestellar cores as well as the observed number of such embedded cores forming in a parent clump. By varying a single parameter, the mass-to-flux ratio, over the range of observationally measured densities, we fit the range of estimated prestellar core lifetimes ($\sim 0.1$ to a few Myr) identified with Herschel as well as the number of embedded cores formed in a parent clump measured in Perseus with the Submillimeter Array (SMA). Our model suggests that the prestellar cores are formed with a transcritical mass-to-flux ratio and higher densities correspond to somewhat higher mass-to-flux ratio but the normalized mass-to-flux ratio $\mu$ remains in the range $1\lesssim \mu \lesssim 2$. Our best-fit model exhibits $B\propto n^{0.43}$ for prestellar cores, due to partial flux-freezing as a consequence of ambipolar diffusion.

Accepted For Publication in Astronomy & Astrophysics Letters, 9 pages, 5 figures

References in corpus (7)

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Cited by in corpus (5)

• Non-ideal MHD simulations of subcritical prestellar cores with non-equilibrium chemistry
• CARMA-NRO Orion Survey: unbiased survey of dense cores and core mass functions in Orion A
• Magnetic field measurement in TMC-1C using 22.3 GHz CCS Zeeman splitting
• An ALMA search for substructure and fragmentation in starless cores in Orion B North
• The Magnetic Field versus Density relation in Star-Forming Molecular Clouds