Kinematics of a hot massive accretion disk candidate
Beuther, H., and Walsh, A.J. (2008) Kinematics of a hot massive accretion disk candidate. The Astrophysical Journal: an international review of astronomy and astronomical physics, 673 (1). pp. 55-58.
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View at Publisher Website: http://dx.doi.org/10.1086/527434
Characterizing rotation, infall, and accretion disks around high-mass protostars is an important topic in massive star formation research. With the Australia Telescope Compact Array and the Very Large Array, we studied a massive disk candidate at high angular resolution in ammonia [NH3(4, 4) and (5, 5)] tracing the warm disk but not the envelope. The observations resolved at ~0.4'' resolution (corresponding to ~1400 AU) a velocity gradient indicative of rotation perpendicular to the molecular outflow. Assuming a Keplerian accretion disk, the estimated protostar-disk mass would be high, similar to the protostellar mass. Furthermore, the position-velocity diagram exhibits additional deviation from a Keplerian rotation profile that may be caused by infalling gas and/or a self-gravitating disk. Moreover, a large fraction of the rotating gas is at temperatures >100 K, markedly different from typical low-mass accretion disks. In addition, we resolve a central double-lobe centimeter continuum structure perpendicular to the rotation. We identify this with an ionized, optically thick jet.
|Item Type:||Article (Refereed Research - C1)|
|Keywords:||stars: early-type; stars: formation; stars: individual; IRAS 18089-1732|
|FoR Codes:||02 PHYSICAL SCIENCES > 0299 Other Physical Sciences > 029999 Physical Sciences not elsewhere classified @ 100%|
|SEO Codes:||97 EXPANDING KNOWLEDGE > 970102 Expanding Knowledge in the Physical Sciences @ 100%|
|Deposited On:||04 Jan 2010 15:11|
|Last Modified:||23 May 2013 00:50|
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|Citation Counts with External Providers:||Web of Science: 18|
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