EPoS Contribution
EPoS Contribution
Physical conditions, kinematics and magnetic field in the accretion disk of a massive star

Alberto Sanna
INAF, Bologna, IT
I will present a comprehensive analysis of the properties of an accretion disk around a young massive star. We have recently made use of ALMA at band 6 to image a sub-Keplerian disk around an O-type young star, where gas is falling in at high rate, and which drives a molecular jet with a radio counterpart. With ALMA at band 7, we now further resolve the disk structure and sample the disk mid-plane with twelve distinct beams, where we measure the gas (and dust) physical conditions separately. Extraordinarily, we also reveal that the accretion disk extends above the mid-plane showing a spiral morphology which we sample with ten additional beams. I will present these results and discuss the dependence of line opacity, temperature, and column density on the radius from the star, as well as addressing the disk stability. I will finally combine this information with the magnetic field morphology inferred from ALMA dust polarization observations, which underline a number of accretion streams conveying mass from the envelope to the disk.
Collaborators:
L. Moscadelli, INAF, IT
R. Cesaroni, INAF, IT
R. Kuiper, Tuebingen U, DE
K. Menten, MPIfR, DE
Key publication

Suggested Session: High-Mass Star Formation