Maser Mapping and Dust Properties of Red Supergiant Winds

Details Maser Mapping and Dust Properties of Red Supergiant Winds Maser Mapping and Dust Properties of Red Supergiant Winds

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ap%26ss.251...55r&link_type=abstract

Astrophysics and Space Science, Volume 251, Issue 1-2, pp. 55-62

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Maser emission from the circumstellar envelopes of four late-type red supergiants has been mapped with milli-arcsecond resolution using MERLIN1. The wind is driven by radiation pressure on dust and the structure and kinematics of the masing regions reflect the dust properties. The unbeamed radius of water maser blobs, ˜ 1012 m, has been measured for the first time. The velocity gradient is used to derive the dust absorption coefficient which increases with radius from ≤ 0.1 to ≤ 1.0 m2 kg-1. Comparison with laboratory studies suggests that small crystalline grains are formed near the star and are annealed into astronomical silicates at larger distances.

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