Modeling the accretion disk around the high-mass protostar GGD 27-MM1
  Recent high-angular resolution (40 mas) ALMA observations at 1.14 mm resolve
a compact (R~200 au) flattened dust structure perpendicular to the HH 80-81 jet
emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate
for a true accretion disk. The jet/disk system (HH 80-81 / GGD 27-MM1) resemble
those found in association with low- and intermediate-mass protostars. We
present radiative transfer models that fit the 1.14 mm ALMA dust image of this
disk which allow us to obtain its physical parameters and predict its density
and temperature structure. Our results indicate that this accretion disk is
compact (Rdisk~170 au) and massive (5Msun), about 20% of the stellar mass of 20
Msun. We estimate the total dynamical mass of the star-disk system from the
molecular line emission finding a range between 21 and 30 Msun, which is
consistent with our model. We fit the density and temperature structures found
by our model with power law functions. These results suggest that accretion
disks around massive stars are more massive and hotter than their low-mass
siblings, but they still are quite stable. We also compare the temperature
distribution in the GGD 27-MM1 disk with that found in low- and
intermediate-mass stars and discuss possible implications on the water snow
line. We have also carried about a study of the distance based on Gaia DR2 data
and the population of young stellar objects (YSOs) in this region, and from the
extinction maps. We conclude that the source distance is in within 1.2 and 1.4
kpc, closer than what was derived in previous studies (1.7 kpc).
