We present the results of line and continuum observations towards the source IRAS 20126+4104, performed at 1.3 mm and 3.5 mm with the Plateau de Bure interferometer, from 350 mu m to 2 mm with the James Clerk Maxwell telescope, and at 10 and 20 mu m with the United Kingdom infrared telescope. The results fully confirm the findings of Cesaroni et al. (\cite{cftwo}), namely that IRAS 20126+4104 is a very young stellar object embedded in a dense, hot core and lying at the centre of a rotating disk. The bipolar jet imaged by Cesaroni et al. (\cite{cftwo}) in the 2.122 mu m H_2 line is seen also in the SiO(2-1) transition, which allows to study the velocity field in the jet. A simple model is developed to obtain the inclination angle of the jet (and hence of the disk axis), which turns out to be almost perpendicular to the line of sight. By studying the diameter of the disk in different transitions and the corresponding line widths and peak velocities, one can demonstrate that the disk is Keplerian and collapsing, and thus compute the mass of the central object and the accretion luminosity. We show that if all the mass inducing the Keplerian rotation is concentrated in a single star, then this cannot be a ZAMS star, but more likely a massive protostar which derives its luminosity from accretion.
Cesaroni R, Felli M, Jenness T, Neri R, Olmi L, Robberto M, et al. (1999). Unveiling the disk-jet system in the massive (proto)star IRAS 20126+4104. ASTRONOMY & ASTROPHYSICS, 345, 949-964.
Unveiling the disk-jet system in the massive (proto)star IRAS 20126+4104
Testi L;
1999
Abstract
We present the results of line and continuum observations towards the source IRAS 20126+4104, performed at 1.3 mm and 3.5 mm with the Plateau de Bure interferometer, from 350 mu m to 2 mm with the James Clerk Maxwell telescope, and at 10 and 20 mu m with the United Kingdom infrared telescope. The results fully confirm the findings of Cesaroni et al. (\cite{cftwo}), namely that IRAS 20126+4104 is a very young stellar object embedded in a dense, hot core and lying at the centre of a rotating disk. The bipolar jet imaged by Cesaroni et al. (\cite{cftwo}) in the 2.122 mu m H_2 line is seen also in the SiO(2-1) transition, which allows to study the velocity field in the jet. A simple model is developed to obtain the inclination angle of the jet (and hence of the disk axis), which turns out to be almost perpendicular to the line of sight. By studying the diameter of the disk in different transitions and the corresponding line widths and peak velocities, one can demonstrate that the disk is Keplerian and collapsing, and thus compute the mass of the central object and the accretion luminosity. We show that if all the mass inducing the Keplerian rotation is concentrated in a single star, then this cannot be a ZAMS star, but more likely a massive protostar which derives its luminosity from accretion.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
