183 GHz water line variation - An energetic outburst in Orion KL

• Published in: The Astrophysical journal Vol. 283; pp. 106 - 116
• Main Authors: Kuiper, T. B. H., Kuiper, E. N. R., Swanson, P. N., Dickinson, D. F., Klein, M. J., Zimmermann, P.
• Format: Journal Article
• Language: English
• Published: Legacy CDMS 01.08.1984
• Subjects: Astrophysics
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/162279

Observations of the 3(13)-2(20) transition of water vapor in the direction of Ori MC1 in 1980 February show a 50 percent flux increase and an apparent additional red shift of approximately 2 km/s relative to the line observed in 1977 December. From a detailed examination of the amplitude and frequency calibration, it appears unlikely that the effect is due to systematic error. The increase is attributed to the appearance of a new component at a velocity of 12 km/s with respect to the local standard of rest. The new component also has broad wings. Increased emission from a region in the high-velocity core of Ori MC1 can be due either to additional far-IR radiation to pump the 1983 GHz transition or to a change in the physical conditions in the gas. Statistical equilibrium calculations using the large-velocity-gradient formalism were carried out to develop a model for the emission. The calculations support a model in which the gas in the region of enhanced emission is hotter than the dust. The temporal coincidence between the 183 GHz increase and the 22 GH1 water maser outburst suggests a common, impulsive cause, which has heated the gas in a part of the HV source, enhancing the emission in both transitions.