Molecular Line Emission from Massive Protostellar Disks: Predictions for ALMA and the EVLA

Details Molecular Line Emission from Massive Protostellar Disks: Predictions for ALMA and the EVLA Molecular Line Emission from Massive Protostellar Disks: Predictions for ALMA and the EVLA

2007-05-03

arxiv.org/abs/0705.0536v1

Astrophys.J.665:478-491,2007

Astronomy and Astrophysics

Astrophysics

15 pages, 9 figures, emulateapj format, accepted for publication in ApJ. Resolution of figures severely degraded to fit within

Scientific paper

10.1086/519305

We compute the molecular line emission of massive protostellar disks by solving the equation of radiative transfer through the cores and disks produced by the recent radiation-hydrodynamic simulations of Krumholz, Klein, & McKee. We find that in several representative lines the disks show brightness temperatures of hundreds of Kelvin over velocity channels ~10 km s^-1 wide, extending over regions hundreds of AU in size. We process the computed intensities to model the performance of next-generation radio and submillimeter telescopes. Our calculations show that observations using facilities such as the EVLA and ALMA should be able to detect massive protostellar disks and measure their rotation curves, at least in the nearest massive star-forming regions. They should also detect significant sub-structure and non-axisymmetry in the disks, and in some cases may be able to detect star-disk velocity offsets of a few km s^-1, both of which are the result of strong gravitational instability in massive disks. We use our simulations to explore the strengths and weaknesses of different observational techniques, and we also discuss how observations of massive protostellar disks may be used to distinguish between alternative models of massive star formation.

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