Evolution of the H2O Maser Emission Zone in ON2 N

Details Evolution of the H2O Maser Emission Zone in ON2 N Evolution of the H2O Maser Emission Zone in ON2 N

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010arep...54..509l&link_type=abstract

Astronomy Reports, Volume 54, Issue 6, pp.509-513

Astronomy and Astrophysics

Astronomy

Scientific paper

Results of a multi-faceted study of the H2O maser emission in the region ON2 N carried out on the Very Large Array (VLA, NRAO) and 22-m radio telescope of the Pushchino Radio Astronomy Observatory are reported. The envelope around the ultracompact HII region is fairly extended and has a composite, strongly fragmented structure. The maser emission zone consists of single spots and spot clusters arranged along an arc, which is associated with a ram shock front. This shock front is nonsta-tionary, and its position changes with time. The front position probably depends on the state of activity of the central star. There can be turbulent motions of material in clusters as well as individual maser spots (such as turbulent vortices). In the turbulent-vortex model, the size of an H2O maser spot is estimated to be 0.07-0.1 AU. Flux-correlated radial-velocity drifts of emission features have been detected, which can be accompanied by spatial displacement (proper motion) of maser spots.

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