Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.381w&link_type=abstract
The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole
Astronomy and Astrophysics
Astronomy
Scientific paper
Recent detections of disks around young high-mass stars indicate their formation through accretion rather than coalescence, but the physical properties of these disks are poorly known. In this study, we used Plateau de Bure interferometric images to probe the environment of the nearby (˜1 kpc) and luminous (˜20000 L_&sun;) high-mass (10-16 M_&sun;) young star AFGL 2591 in continuum and in lines of HDO, H_218O and SO_2 in the 115 and 230 GHz bands. At ˜ 0.5 '' (500 AU) resolution, the images clearly resolve the velocity field of central compact source (diameter of ˜800-1000 AU) and show linear velocity gradients (˜10-30 km s-1 per 1000 AU) roughly in NE-SW direction which is basically perpendicular to the large scale E-W bipolar outflow as an indication of a circumstellar disk around the central massive star. In addition, the HDO line shows a clear triple-peak profile. We suggest that the blue- and red-shifted components come from the rotating disk and the systemic component comes from the surrounding dense envelope. Modeling the kinematics with a 2D radiative transfer code suggests that the velocity field in the proposed disk is consistent with rigid-body rotation plus expansion. Magnetic braking may occur in the disk resulting a linear velocity gradient. The expansion motion may be a signature of the outward angular momentum transportation of an accretion disk or due to the influences of outflows and winds from the star. Our results support the idea that early B-type stars can be formed through disk accretion.
Hogerheijde Michiel
van der Tak Floris
Wang Kun-Shan
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