The Chemical Evolution of the Galactic Bulge
Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemic...
Ausführliche Beschreibung
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| Autor*in: |
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| Format: |
E-Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1999 |
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| Umfang: |
8 |
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| Reproduktion: |
Springer Online Journal Archives 1860-2002 |
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| Übergeordnetes Werk: |
in: Astrophysics and space science - 1968, 265(1999) vom: Jan./Apr., Seite 311-318 |
| Übergeordnetes Werk: |
volume:265 ; year:1999 ; month:01/04 ; pages:311-318 ; extent:8 |
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| 245 | 1 | 0 | |a The Chemical Evolution of the Galactic Bulge |
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| 520 | |a Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. | ||
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(DE-627)NLEJ193082748 DE-627 ger DE-627 rakwb eng The Chemical Evolution of the Galactic Bulge 1999 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. Springer Online Journal Archives 1860-2002 Matteucci, F. oth Romano, D. oth in Astrophysics and space science 1968 265(1999) vom: Jan./Apr., Seite 311-318 (DE-627)NLEJ188985301 (DE-600)1472548-4 1572-946X nnns volume:265 year:1999 month:01/04 pages:311-318 extent:8 http://dx.doi.org/10.1023/A:1002172113229 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 265 1999 1/4 311-318 8 |
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(DE-627)NLEJ193082748 DE-627 ger DE-627 rakwb eng The Chemical Evolution of the Galactic Bulge 1999 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. Springer Online Journal Archives 1860-2002 Matteucci, F. oth Romano, D. oth in Astrophysics and space science 1968 265(1999) vom: Jan./Apr., Seite 311-318 (DE-627)NLEJ188985301 (DE-600)1472548-4 1572-946X nnns volume:265 year:1999 month:01/04 pages:311-318 extent:8 http://dx.doi.org/10.1023/A:1002172113229 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 265 1999 1/4 311-318 8 |
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(DE-627)NLEJ193082748 DE-627 ger DE-627 rakwb eng The Chemical Evolution of the Galactic Bulge 1999 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. Springer Online Journal Archives 1860-2002 Matteucci, F. oth Romano, D. oth in Astrophysics and space science 1968 265(1999) vom: Jan./Apr., Seite 311-318 (DE-627)NLEJ188985301 (DE-600)1472548-4 1572-946X nnns volume:265 year:1999 month:01/04 pages:311-318 extent:8 http://dx.doi.org/10.1023/A:1002172113229 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 265 1999 1/4 311-318 8 |
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(DE-627)NLEJ193082748 DE-627 ger DE-627 rakwb eng The Chemical Evolution of the Galactic Bulge 1999 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. Springer Online Journal Archives 1860-2002 Matteucci, F. oth Romano, D. oth in Astrophysics and space science 1968 265(1999) vom: Jan./Apr., Seite 311-318 (DE-627)NLEJ188985301 (DE-600)1472548-4 1572-946X nnns volume:265 year:1999 month:01/04 pages:311-318 extent:8 http://dx.doi.org/10.1023/A:1002172113229 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 265 1999 1/4 311-318 8 |
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(DE-627)NLEJ193082748 DE-627 ger DE-627 rakwb eng The Chemical Evolution of the Galactic Bulge 1999 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. Springer Online Journal Archives 1860-2002 Matteucci, F. oth Romano, D. oth in Astrophysics and space science 1968 265(1999) vom: Jan./Apr., Seite 311-318 (DE-627)NLEJ188985301 (DE-600)1472548-4 1572-946X nnns volume:265 year:1999 month:01/04 pages:311-318 extent:8 http://dx.doi.org/10.1023/A:1002172113229 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 265 1999 1/4 311-318 8 |
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Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. |
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Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. |
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Abstract In this paper we review the chemical evolution models for the Galactic bulge: in particular, we discuss the predictions of models as compared with the available abundance data and infer the mechanism as well as the time scale for the formation of the Galactic bulge. We show that good chemical evolution models reproducing the observed metallicity distribution of stars in the bulge predict that the [α/Fe] >0 over most of the metallicity range. This is a very important constraint indicating that the bulge of our Galaxy formed at the same time and even faster than the inner Galactic halo. We also discuss predictions for the evolution of light elements such as D and 7Li and conclude that the D astration should be maximum due to the high star formation rate required for the bulge whereas the evolution of the abundance of Li should be similar to that observed in the solar neighbourhood, but with an higher Li abundance in the interstellar medium at the present time. |
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