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The Structure of OH Maser Clouds Associated with Late-Type Stars

Published online by Cambridge University Press:  04 August 2017

P. F. Bowers ,
K. J. Johnston  and
J. H. Spencer
P. F. Bowers
Affiliation:
1E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, D. C. 20375 2Sachs/Freeman Associates, Bowie, Maryland 20715
K. J. Johnston
Affiliation:
1E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, D. C. 20375
J. H. Spencer
Affiliation:
1E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, D. C. 20375

Extract

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The absolute positions and the arcsec structure of OH maser clouds surrounding 20 Mira variables and late-type supergiant stars have been measured using the Very Large Array in a spectral line mode at 1612 MHz. The stars observed are listed in Table 1 which indicates that the angular radii θ of the maser clouds range up to 4″. The linear radii R range from < 100 AU for the Mira variable U Ori to 104 AU for the supergiant IRC+10420 and are correlated with the stellar mass loss rates.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 110: VLBI and Compact Radio Sources , 1984 , pp. 327 - 328
Copyright
Copyright © Reidel 1984 

References

Bowers, P. F., Johnston, K. J., and Spencer, J. H. 1983, Ap. J., in press.Google Scholar