Open AccessMERLIN observations of water maser proper motions in VY Canis Majoris
Author(s) -
Richards A. M. S.,
Yates J. A.,
Cohen R. J.
Publication year - 1998
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1998.01386.x
Subject(s) - physics , maser , astrophysics , circumstellar envelope , supergiant , astronomy , outflow , proper motion , nebula , merlin (protein) , stars , meteorology , medicine , cancer , suppressor
MERLIN observations of the 22‐GHz water masers in the circumstellar envelope of the supergiant VY CMa show an ellipsoidal distribution with a maximum extent of 700 mas east–west and 400 mas north–south. Comparison with observations made nine years earlier shows that the majority of maser features have survived and show proper motions throughout the region. The mean change in position is 28 mas and the proper motions are generally directed away from the assumed stellar position, and tend to be larger for features at greater projected distances. If the H 2 O maser region is modelled as a partially filled thick spherical shell, and VY CMa is at a distance of 1.5 kpc, then the proper motion velocities in the direction of expansion are between 8 km s −1 at a distance of 75 mas from the assumed stellar position and 32 km s −1 at 360 mas. These velocities are consistent with the H 2 O maser spectral line velocities which correspond to a maximum expansion velocity of 36 km s −1 at 400 mas from the assumed stellar position. These observations are consistent with radiation pressure on dust providing the force to accelerate the stellar wind as it passes through the H 2 O maser shell. The H 2 O maser region is elongated in the same direction as the dusty nebula around VY CMa. The water masers illuminate the small‐scale dynamics and clumpiness which show the role of dust in driving the outflow. The overall ellipsoidal shape may be due to properties of the dust, such as its behaviour in the stellar magnetic field, or to interaction between the wind and circumstellar material. Maser monitoring also shows the difference between changes on the time‐scale of stellar variability (a few years) and possible stages in the evolution of VY CMa to its likely fate as a supernova.