Radio interferometric observations of an H2O maser flare in the Orion Nebula at epoch 1982.9 have been used to determine the flare’s spatial structure. Antennas in the Crimea, Effelsberg, and Onsala were used. The emission region consists of three groups of components. The angular sizes of the components are 0.2 0.9 mas, and the widths of the emitted lines are 0.2 0.7 km/s. The velocities of the components are correlated with their relative positions, which correspond to expanding concentric rings. Assuming a 1 M ⊙ protostar in a Keplerian approximation, the radius of the inner ring R is 15 AU, the velocity of its rotation V rot is 8.98 km/s, and the radial component of the velocity V rad is 1.79 km/s. For the outer ring, R=15.7 AU, V rot=8.79 km/s, and V rad=2.61 km/s. |