Volume 390, Number 1, July IV 2002
|Page(s)||281 - 287|
|Published online||05 July 2002|
A water maser flare in W49N
The superposition of the spectra of two component masers
Department of Astronomy, Nanjing University, Nanjing 210093, PR China
2 Urumqi Astronomical Station, Chinese Academy of Science, Xinjiang, 830011, PR China
Corresponding author: J. J. Zhou, firstname.lastname@example.org
Accepted: 7 May 2002
We report the results of our short time scale monitoring observations of W49N. Three water maser features were found to show obvious variations in flux density, line width and center velocity. Over a period of about 22 days, the -88.3, -56.9 and -12.8 km features declined linearly in flux density at rates of 57, 113, 98.8 Jy per day, respectively. The line widths of the -56.9 and -12.8 km features increased at rates of ~0.022 and ~0.046 km per day, respectively, while the line width of the -88.3 km feature increased at a rate of 0.01 km per day during the first 17 days and decreased at a rate of 0.017 km per day during the remainder of the days. All three features show a systematic shift of ~1 km in center velocity. We propose a model based on the superposition of the spectra of two maser clouds to explain the variations of these maser features: two rigidly rotating, unsaturated spherical maser clouds during the declining phase reach the same line-of-sight velocity, then they depart from each other because of their relative acceleration.
Key words: masers-stars: formation-ISM: individual objects: W49N
© ESO, 2002
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