Physics and chemistry of hot molecular cores
arXiv:astro-ph/0610411 · doi:10.1017/S1743921307001378
Abstract
Young massive star-forming regions are known to produce hot molecular gas cores (HMCs) with a rich chemistry. While this chemistry is interesting in itself, it also allows to investigate important physical parameters. I will present recent results obtained with high-angular-resolution interferometers disentangling the small-scale structure and complexity of various molecular gas components. Early attempts to develop a chemical evolutionary sequence are discussed. Furthermore, I will outline the difficulty to isolate the right molecular lines capable to unambiguously trace potential massive accretion disks.
arXiv comment6 pages, 3 figures, proceedings to the IAU Syposium 237 "Triggered star formation in a turbulent ISM"
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Cited by in corpus (5)
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- Multi-line (sub)millimetre observations of the high-mass proto cluster IRAS 05358+3543
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- (Sub)mm Interferometry Applications in Star Formation Research