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arXiv · 1701.03781

Evolutionary Description of Giant Molecular Cloud Mass Functions on Galactic Disks

Masato I. N. Kobayashi·Shu-ichiro Inutsuka·Hiroshi Kobayashi·Kenji Hasegawa
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Abstract

Recent radio observations show that the giant molecular cloud (GMC) mass functions noticeably vary across galactic disks. High-resolution magnetohydrodynamics simulations show that multiple episodes of compression are required for creating a molecular cloud in the magnetized interstellar medium. In this article, we formulate the evolution equation for the GMC mass function to reproduce the observed profiles, for which multiple compression are driven by the network of expanding shells due to HII regions and supernova remnants. We introduce the cloud-cloud collision (CCC) terms in the evolution equation in contrast to the previous work (Inutsuka et al. 2015). The computed time evolution suggests that the GMC mass function slope is governed by the ratio of GMC formation timescale to its dispersal timescale, and that the CCC effect is limited only in the massive-end of the mass function. In addition, we identify a gas resurrection channel that allows the gas dispersed by massive stars to regenerate GMC populations or to accrete onto the pre-existing GMCs. Our results show that almost all of the dispersed gas contribute to the mass growth of pre-existing GMCs in arm regions whereas less than 60 per cent in inter-arm regions. Our results also predict that GMC mass functions have a single power-law exponent in the mass range < 10^5.5 Msun (where Msun represents the solar mass), which is well characterized by GMC self-growth and dispersal timescales. Measurement of the GMC mass function slope provides a powerful method to constrain those GMC timescales and the gas resurrecting factor in various environment across galactic disks.

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Masato I. N. Kobayashi, Shu-ichiro Inutsuka, Hiroshi Kobayashi, Kenji Hasegawa. 2017-01-16. Evolutionary Description of Giant Molecular Cloud Mass Functions on Galactic Disks. https://doi.org/10.3847/1538-4357%2F836%2F2%2F175

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