Hostname: page-component-cb9f654ff-pvkqz Total loading time: 0 Render date: 2025-08-04T04:31:53.296Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Information

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