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Astron. Astrophys. 364, 232-236 (2000)

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4. Conclusion

Daily monitoring for a period of about a month has allowed accurate measurements of rapid variations of the water masers in W3(OH) and NGC 6334C and the results can be summarized as follows:

The flux density of the -52.8 km[FORMULA] component in W3(OH) decayed linearly with the timescale of 19 days, and the -84.4 km[FORMULA] component in NGC 6334C flared rapidly, rising from 1090 to 2200 Jy with a timescale of about 4 days.

The rapid time variations could be explained by interstellar propagation effects, but even if the true size of the water source in NGC 6334C has an order of magnitude less than the typical estimate in diameter, the refractive time scale was still hard to fit to the fluctuation time scale seen in NGC 6334C.

The collision rapidly heats the gas to the temperature of the dust and thus quenches the pump in the following few days or longer period. The collsion may cause the rapid time variabilities of the observed water maser features.

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© European Southern Observatory (ESO) 2000

Online publication: December 15, 2000
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