Modeling of Protostellar Clouds and their Observational Properties

Abstract

A physical model and two-dimensional numerical method for computing the evolution and spectra of protostellar clouds are described. The physical model is based on a system of magneto-gasdynamical equations, including ohmic and ambipolar diffusion, and a scheme for calculating the thermal and ionization structure of a cloud. The dust and gas temperatures are determined during the calculations of the thermal structure of the cloud. The results of computing the dynamical and thermal structure of the cloud are used to model the radiative transfer in continuum and in molecular lines. We presented the results for clouds in hydrostatic and thermal equilibrium. The evolution of a rotating magnetic protostellar cloud starting from a quasi-static state is also considered. Spectral maps for optically thick lines of linear molecules are analyzed. We have shown that the influence of the magnetic field and rotation can lead to a redistribution of angular momentum in the cloud and the formation of a characteristic rotational velocity structure. As a result, the distribution of the velocity centroid of the molecular lines can acquire an hourglass shape. We plan to use the developed program package together with a model for the chemical evolution to interpret and model observed starless and protostellar cores.

Accepted to Astronomy Reports

References in corpus (5)

• Cold Dark Clouds: The Initial Conditions for Star Formation
• Molecular line radiative transfer in protoplanetary disks: Monte Carlo simulations versus approximate methods
• Chemical and thermal structure of protoplanetary disks as observed with ALMA
• Molecular Emission Line Formation in Prestellar Cores
• CB17: Inferring the dynamical history of a prestellar core with chemo-dynamical models

Cited by in corpus (6)

• The Earliest Phases of Star formation observed with Herschel (EPoS): The dust temperature and density distributions of B68
• Variation in dust properties in a dense filament of the Taurus molecular complex (L1506)
• Three intermediate-mass YSOs with different properties emerging from the same natal cloud in IRAS 00117+6412
• Thermal structure of a protostellar envelope
• Simulations of the isothermal collapse of magnetic rotating protostellar clouds
• Primary disks and their observational appearance in collapsing magnetic rotating protostellar clouds