A Detailed Comparison of the Modes of Star Formation in G305.35+0.7 and NGC 2174/5

Mathematics – Logic

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Scientific paper

Some low-mass stars form in regions of isolated star formation, such as the nearby Taurus-Auriga molecular cloud. Others form instead in regions surrounding massive stars. There are a number of indications that the process of star formation itself may different in important ways depending on the details of the larger environment. In particular, while much star formation seems to be the result of hierarchical collapse and fragmentation in isolated cloud cores, both low- and high-mass star formation in other regions appears to be triggered by compression of gas in advance of expanding ionization fronts around massive stars. There are many implications of these differences, ranging from the origin of the IMF to our understanding of the environment in which the Sun and Solar System formed and evolved. In this proposal we request time to conduct a detailed MIPS/IRAC/IRS investigation of G305.35+0.07 and NGC 2174/5, comparing and contrasting star formation between the two regions. The morphology of one of these regions (G305.35+0.07) is strongly suggestive of triggered star formation in a shell around massive stars, while the other region (NGC2174/5) consists of several apparently detached clusters that might have formed instead through heirarchical collapse. Studies of the distribution of low-mass protostars in these regions, and especially the extent to which they are concentrated in compressed gas around the periphery of each region, will allow us to discriminate between triggered and untriggered star formation. Among our goals is determining whether overt morphological characteristics of H II regions are reliable indicators of the nature of low-mass star formation in these regions.

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