Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano
Observations on the UBV and DDO photometric systems have been obtained for 182 red evolved stars in 53 open clusters belonging to the disc and the galactic plane. Cluster membership was confirmed for 77 % of the stars by using two independent criteria. Interstellar reddening, ultraviolet excess, and...
Guardado en:
| Autor principal: | |
|---|---|
| Formato: | Articulo Comunicacion |
| Lenguaje: | Español |
| Publicado: |
1980
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/146719 |
| Aporte de: |
| id |
I19-R120-10915-146719 |
|---|---|
| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Español |
| topic |
Astronomía Galaxia |
| spellingShingle |
Astronomía Galaxia Clariá, J.J. Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| topic_facet |
Astronomía Galaxia |
| description |
Observations on the UBV and DDO photometric systems have been obtained for 182 red evolved stars in 53 open clusters belonging to the disc and the galactic plane. Cluster membership was confirmed for 77 % of the stars by using two independent criteria. Interstellar reddening, ultraviolet excess, and cyanogen anomalies have been determined for the stars. The clusters were ordered by their relative ages in a self-consistent sequence. The variation of [Fe/H] with age and position in the galaxy was analysed. Although the abundance determinations for the youngest clusters are very uncertain, their [Fe/H] values appear to be higher in the mean than the average for solar neighborhood K giants. No evidence for a variation of [Fe/H] with age in the last ∼10⁹ years was found. On the other hand, a trend of decreasing metal content with increasing age seems to exist for the disc clusters. An examination of the location of the clusters in the galaxy supports the conclusion that position rather than age could be the dominant factor determining the metal abundance of stars in our galaxy. |
| format |
Articulo Comunicacion |
| author |
Clariá, J.J. |
| author_facet |
Clariá, J.J. |
| author_sort |
Clariá, J.J. |
| title |
Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| title_short |
Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| title_full |
Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| title_fullStr |
Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| title_full_unstemmed |
Composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| title_sort |
composición química en la galaxia: distribución de elementos pesados en el disco y en el plano |
| publishDate |
1980 |
| url |
http://sedici.unlp.edu.ar/handle/10915/146719 |
| work_keys_str_mv |
AT clariajj composicionquimicaenlagalaxiadistribuciondeelementospesadoseneldiscoyenelplano |
| bdutipo_str |
Repositorios |
| _version_ |
1764820461572587520 |