Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-06T07:46:29.874Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopic Analysis of HR 1099

Published online by Cambridge University Press:  12 April 2016

I.S. Savanov  and
I. Tuominen
I.S. Savanov
Affiliation:
Crimean Astrophysical Observatory, Nauchny, 334413, Crimea, USSR
I. Tuominen
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, Tähtitorninmäki, 00130 Helsinki, Finland

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 calculated synthetic spectra for HR 1099 for the wavelength region λ6425-6445 Å, which includes the Cal λ6439 Å and FeI λ6430 Å lines, often used for the surface imaging of rapidly rotating late-type stars. The best agreement between the theoretical and observed spectra can be achieved with solar abundances in the both components of the system, except for Ca in the primary. Theoretical calculations give the possibility of estimating the influence of microturbulence, damping and blending on Ca I and Fe I line profiles.

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 449 - 451
Copyright
Copyright © Springer-Verlag 1991

References

Bell, R.A., Eriksson, K., Gustafsson, B., Nordlund, Å.: 1976, Astron. Astrophys. Suppl. 23, 37 Google Scholar
Fekel, F.C.: 1983, Astrophys. J. 268, 274 Google Scholar
Gray, D.F.: 1976, in The observations and analysis of stellar photospheres, Wiley, New York Google Scholar
Lyubimkov, L.S., Samedov, Z.A.: 1987, Bull. Crimean Astrophys. Obs. 77, 109 Google Scholar
Vogt, S.S., Penrod, G.D.: 1983, Publ. A. S. P. 95, 565 Google Scholar