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• W1966247736 endingPage "35" @default.
• W1966247736 startingPage "35" @default.
• W1966247736 abstract "Using three-dimensional magnetohydrodynamic simulations, including the effects of radiative cooling/heating, chemical reactions, and thermal conduction, we investigate the formation of molecular clouds in the multi-phase interstellar medium. As suggested by recent observations, we consider the formation of molecular clouds due to accretion of H i clouds. Our simulations show that the initial H i medium is piled up behind the shock waves induced by accretion flows. Since the initial medium is highly inhomogeneous as a consequence of thermal instability, a newly formed molecular cloud becomes very turbulent owing to the development of the Richtmyer–Meshkov instability. The kinetic energy of the turbulence dominates the thermal, magnetic, and gravitational energies throughout the entire 10 Myr evolution. However, the kinetic energy measured using CO-fraction-weighted densities is comparable to the other energies, once the CO molecules are sufficiently formed as a result of UV shielding. This suggests that the true kinetic energy of turbulence in molecular clouds as a whole can be much larger than the kinetic energy of turbulence estimated using line widths of molecular emission. We find that clumps in a molecular cloud show the following statistically homogeneous evolution: the typical plasma β of the clumps is roughly constant 〈β〉 ≃ 0.4; the size–velocity dispersion relation is Δv ≃ 1.5 km s−1 (l/1 pc)0.5, irrespective of the density; the clumps evolve toward magnetically supercritical, gravitationally unstable cores; and the clumps seem to evolve into cores that satisfy the condition for fragmentation into binaries. These statistical properties may represent the initial conditions of star formation." @default.
• W1966247736 created "2016-06-24" @default.
• W1966247736 creator A5062038963 @default.
• W1966247736 creator A5085873695 @default.
• W1966247736 date "2012-10-15" @default.
• W1966247736 modified "2023-10-12" @default.
• W1966247736 title "FORMATION OF TURBULENT AND MAGNETIZED MOLECULAR CLOUDS VIA ACCRETION FLOWS OF H I CLOUDS" @default.
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• W1966247736 doi "https://doi.org/10.1088/0004-637x/759/1/35" @default.
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