H2O Maser Outflow from the Red Supergiant Star NML Cygni Observed with Japanese VLBI Network

Details H2O Maser Outflow from the Red Supergiant Star NML Cygni Observed with Japanese VLBI Network H2O Maser Outflow from the Red Supergiant Star NML Cygni Observed with Japanese VLBI Network

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008pasj...60.1069n&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.60, No.5, pp.1069--1075

Astronomy and Astrophysics

Astronomy

1

Masers, Stars: Individual (Nml Cygni), Stars: Kinematics, Stars: Supergiants

Scientific paper

We present the proper motions of H2O masers in NML Cygni, observed with the Japanese VLBI Network at three epochs spanning 455d. We detected about 15 maser features at each epoch. Overall, 13 features that were detected at least twice were tracked by their radial velocities and proper motions. The three-dimensional kinematics of the maser features indicate the presence of an expanding outflow. The major axis of the outflow is estimated to be at a position angle of ˜108°, and an inclination angle of ˜8° with respect to the line of sight. The H2O masers are located between an apparent minimum radius of ˜9.6 × 1012m (64AU) and a maximum radius of ˜3.0 × 1013m (202AU), where the expansion velocity increases from 12 to 27km s-1. A comparison with the distributions of SiO, H2O, and OH masers suggests that the outflow of NML Cygni is expanding outside a radius of ˜1.5 × 1013m (100AU). This radius corresponds to 6 stellar radii, and is consistent with the radius of the inner boundary for the dust shell.

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