Hostname: page-component-745bb68f8f-grxwn Total loading time: 0 Render date: 2025-01-11T15:45:27.446Z Has data issue: false hasContentIssue false
  • English
  • Français

Investigation of the chemical structure of our Galaxy using radial pulsating stars as tracers

Published online by Cambridge University Press:  09 March 2010

Marian Doru Suran
Marian Doru Suran*
Affiliation:
Astronomical Institute of the Romanian Academy, str. Cutitul de Argint 5, RO-040557, Bucharest, Romania email: suran@aira.astro.ro
Rights & Permissions [Opens in a new window]

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.

In this paper we try to determine the properties of different galactic components (2 < r < 12kpc) using radial pulsating stars (RPS stars) as tracers. For RPS stars in Galaxy we use a quasi-seismological inversion method (Post Theoretical Mass Method, PTM) which allows us to determine the mass M and the abundance Z for each star. Based on PTM method and using RPS stars as tracers we could determine the chemical structure and evolution of the Galaxy: abundance gradients and segregation between different evolutionary populations. This method is planned to be extended further using the RPS star observed by the KEPLER space mission.

Keywords

ISM: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 378 - 379
Copyright
Copyright © International Astronomical Union 2010

References

Cox, A. 1980, ARA&A, 18, 15Google Scholar
Suran, M. D. 1985, Top. Astrophys. Astron. Space Sci., 1, 1Google Scholar
Suran, M. D. 1986, Top. Astrophys. Astron. Space Sci., 2, 28Google Scholar
Suran, M. D. 1990, Contrib. Astron. Obs. Skalnat Pleso, 20, 77Google Scholar