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Paper: Chemo-Dynamical and Radiation Transfer Models to Understand the Early Stages of Star Formation
Volume: 510, Stars: From Collapse to Collapse
Page: 3
Authors: Shustov, B.; Pavlyuchenkov, Y.
Abstract: It is observation of emission (absorption) lines in molecular spectra (supplemented by infrared observations of dust) that shapes a phenomenological picture of star formation. In spite of great amount of observation data of numerous molecular species (at the moment there are known about 200 molecular species) the revealing nature of objects on the very early stages of star formation turned out to be not an easy task, since solving a typical astronomical inverse problem of determining the properties of an astronomical object from observations (spectrum) requires some additional information. We use evolutionary chemo-dynamical models of star formation (from starless cores to protoplanetary disks) as such an additional information. This allows us to understand the nature of object under study, i.e. estimate distributions of gas density, temperature, velocity, the abundances of individual chemical components, and the evolutionary status of the object. The brief review examines the progress in understanding evolution of young objects that is derived from observations of molecular spectra and our chemo-dynamical models. Also disclosed is a method for determining the validity of interpretation of the observed spectra of prestellar objects, protostars and protostellar disks. This method was used for number of such objects.
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