Abstract
We monitored the 22-GHz water vapor emission from W49N using a single VLBA antenna on intervals of a few days to about a week from December 1989 through May 1990. During this period, a strong flare occurred in one of the spectral features. This feature increased in flux density by a factor of ≳20 over a period of approximately 30 days. Line narrowing accompanied the rise in flux density; the decrease in linewidth with flux density follows the power law ΔV ∝ F −0.22
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© 1993 Springer-Verlag
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Boboltz, D.A., Simonetti, J.H., Diamond, P.J., Uphoff, J.A., Dennison, B. (1993). An H2O flare in W49N. In: Clegg, A.W., Nedoluha, G.E. (eds) Astrophysical Masers. Lecture Notes in Physics, vol 412. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-56343-1_260
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DOI: https://doi.org/10.1007/3-540-56343-1_260
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