Physics and chemistry of hot molecular cores

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.

6 pages, 3 figures, proceedings to the IAU Syposium 237 "Triggered star formation in a turbulent ISM"

References in corpus (1)

• CB17: Inferring the dynamical history of a prestellar core with chemo-dynamical models

Cited by in corpus (4)

• ATOMS:ALMA Three-millimeter Observations of Massive Star-forming regions -- III :Catalogues of candidate hot molecular cores and Hyper/Ultra compact HII regions
• Multi-line (sub)millimetre observations of the high-mass proto cluster IRAS 05358+3543
• Ultracompact HII regions with extended emission: The case of G43.89-0.78 and its molecular environment
• (Sub)mm Interferometry Applications in Star Formation Research