Radiation-hydrodynamical simulations of massive star formation using Monte Carlo radiative transfer II. The formation of a 25 solar-mass star
Harries, TJ; Douglas, T; Ali, A
Date: 16 June 2017
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP) / Royal Astronomical Society
Publisher DOI
Abstract
We present a numerical simulation of the formation of a massive star using Monte-
Carlo-based radiation hydrodynamics (RHD). The star forms via stochastic disc ac-
cretion and produces fast, radiation-driven bipolar cavities. We nd that the evolution
of the infall rate (considered to be the mass
ux across a 1500 au spherical ...
We present a numerical simulation of the formation of a massive star using Monte-
Carlo-based radiation hydrodynamics (RHD). The star forms via stochastic disc ac-
cretion and produces fast, radiation-driven bipolar cavities. We nd that the evolution
of the infall rate (considered to be the mass
ux across a 1500 au spherical boundary),
and the accretion rate onto the protostar, are broadly consistent with observational
constraints. After 35 kyr the star has a mass of 25M and is surrounded by a disc
of mass 7 M and 1500 au radius, and we nd that the velocity eld of the disc is
close to Keplerian. Once again these results are consistent with those from recent
high-resolution studies of discs around forming massive stars. Synthetic imaging of
the RHD model shows good agreement with observations in the near- and far-IR, but
may be in con
ict with observations that suggests that MYSOs are typically circularly
symmetric on the sky at 24.5 m. Molecular line simulations of a CH3CN transition
compare well with observations in terms of surface brightness and line width, and
indicate that it should be possible to reliably extract the protostellar mass from such
observations.
Physics and Astronomy
Faculty of Environment, Science and Economy
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