Hostname: page-component-65f69f4695-vv84r Total loading time: 0 Render date: 2025-06-30T19:11:13.906Z Has data issue: false hasContentIssue false
  • English
  • Français

SiO Isotope Emissions from Late-Type Stars

Published online by Cambridge University Press:  12 April 2016

N. Ukita  and
N. Kaifu
N. Ukita
Affiliation:
Nobeyama Radio Observatory, Tokyo Astron. Obsevatory Minamisaku, Nagano 384-13, Japan
N. Kaifu
Affiliation:
Nobeyama Radio Observatory, Tokyo Astron. Obsevatory Minamisaku, Nagano 384-13, Japan

Abstract

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 J=2-1, v=0 emissions of 28SiO, 29SiO, and 30SiO from three late-type stars were simultaneously observed with the Nobeyama 45-m telescope in Jaunuary 1987. The relative intensities of [29SiO] / [30SiO] were measured to be 2.4 for χ Cyg, 1.5 for NML Tau, and 2.9 for V1111 0ph. These values are lower limits for the relative isotope abundance of [29Si] / [30Si], and are larger than the terrestrial value of 1.51. Recext theoretical studies suggest that hydrostatic nucleosysnthesis and supernova explosions result in smaller values of [29Si / [30 Si] than solar. These models cannot explain the observed excess of 29Si.

Information

Type
Part I. Chemical Peculiarities as Probe of Stellar Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 51 - 52
Copyright
Copyright © Springer-Verlag 1988

References

Nomoto, K., Thielemann, F.-K., and Yokoi, K., 1984, Astrophys. J., 286, 644.CrossRefGoogle Scholar
Thielemann, F.-K., and Arnett, W.D., 1985, Astrophys. J., 295, 604.CrossRefGoogle Scholar
Woosley, S.E. and Weaver, T.A., 1986, Ann. Rev. Astron. Astrophys, 24, 205 CrossRefGoogle Scholar