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3He+ in galactic H II regions: Possible evidence for non-convective mixing in low mass stars

Published online by Cambridge University Press:  04 August 2017

Robert T. Rood ,
Thomas M. Bania  and
Thomas L. Wilson
Robert T. Rood
Affiliation:
University of Virginia
Thomas M. Bania
Affiliation:
Boston University
Thomas L. Wilson
Affiliation:
MPIfR, Bonn

Abstract

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We have detected the 8.7 GHz hyperfine line of 3He+ in the HII regions W43, W51, and W3 and obtained significant upper limits for M17, W49, and Orion A. Even though the abundances derived from measured line parameters can have large uncertainty due to the detailed structure of the sources, it seems almost certain that the 3He+ abundance in W3, 12 kpc from the galactic center is significantly higher than in sources closer to the galactic center. If this is the result of general chemical evolution of the galaxy, it is exactly the opposite of what is expected.

Type
IV. RELATION WITH CHEMICAL EVOLUTION OF GALAXIES AND COSMOLOGY
Information
Symposium - International Astronomical Union , Volume 105: Observational Tests of the Stellar Evolution Theory , 1984 , pp. 567 - 570
Copyright
Copyright © Reidel 1984 

References

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Rood, R. T. Steigman, G., and Tinsley, B. M. 1976, Ap. J. Letters, 207, L57.Google Scholar
Schatzmann, E. 1984, this volume, p. 491.Google Scholar