Hostname: page-component-5c6d5d7d68-vt8vv Total loading time: 0.001 Render date: 2024-08-07T09:30:37.387Z Has data issue: false hasContentIssue false
  • English
  • Français

IR Boron Lines in Stellar Spectra

Published online by Cambridge University Press:  25 May 2016

J Meléndez ,
B. V. Castilho  and
B Barbuy
J Meléndez
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, Departamento de Astronomia, Caixa Postal 3386, 01060-970, Brazil
B. V. Castilho
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, Departamento de Astronomia, Caixa Postal 3386, 01060-970, Brazil
B Barbuy
Affiliation:
Instituto Astronômico e Geofísico, Universidade de São Paulo, Departamento de Astronomia, Caixa Postal 3386, 01060-970, Brazil

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.

We have computed synthetic spectra of the infrared B I transitions at 1.166 and 1.624 μm in order to examine the possibility of abundance determination by using these lines. We found that the IR boron lines are better observed in cool giants and supergiants. S/N > 150 and R ≈ 60000 are required in order to determine the boron abundances.

Type
6. Stellar Knowledge to and from Light Elements
Information
Symposium - International Astronomical Union , Volume 198: The Light Elements and their Evolution , 2000 , pp. 487 - 488
Copyright
Copyright © Astronomical Society of the Pacific 2000 

References

Castilho, B. V., Spite, F., Barbuy, B., Spite, M., De Medeiros, J.R., & Gregorio-Hetem, J. 1999, A&A, 345, 249 Google Scholar
Cunha, K., & Smith, V. 1999, ApJ, 512, 1006 CrossRefGoogle Scholar
Duncan, D. K., Peterson, R. C., Thorburn, J. A. & Pinsonneault, M. H. 1998, ApJ, 499, 871 CrossRefGoogle Scholar
Meléndez, J., & Barbuy, B. 1999, ApJS, 124, 527 CrossRefGoogle Scholar