1998ApJ...509..256B

We monitored the 22 GHz H₂O maser emission toward W49N from December 1989 through May 1990. During this period we observed an outburst in a component at -66.25 km.s^–1. The flux density of the flaring component increased by a factor of ≳10 to a maximum of 4020 Jy over a period of 24 days and decreased over the following 34 days to 1400 Jy on the last day of monitoring. During the flux increase the line narrowed from about 1.1 to 0.8 km.s^–1; it subsequently rebroadened to 1.0 km.s^–1. Most interestingly, during the flaring behavior the line center shifted by approximately 0.5 km.s^–1 over the 58 day period. To explain the flare, particularly its shifting line center, we present a model of two interacting maser clouds. In the model, saturated maser radiation produced in a background cloud is amplified by an unsaturated, masing foreground cloud. Motion of the foreground cloud across the line of sight produces a flaring line, accompanied by line narrowing. We demonstrate that the observed flare in W49N may be explained by such a model where a rotating foreground cloud passes in front of a nonrotating background cloud. The differential amplification of the background cloud's radiation produces the observed increase in flux density, line narrowing, and systematic shift in center velocity.