The solar neighborhood age-metallicity relation - Does it exist?
(2002) Workshop on Modes of Star Formation and the Origin of Field Populations 285. p.243-247- Abstract
- We test the hypothesis that the spread in the age-metallicity plot of the solar neighborhood is due to a mixture of stars belonging to kinematically different sub-populations of the Galactic disk, i.e., the thin and the thick disk. We use a kinematic subsample of similar to 600 stars from a sample of similar to 6000 dwarf and subgiant stars from the Hipparcos catalog. All of these stars have a full set of stellar parameters determined, including good ages. We find that a significant spread in [Me/H] is present in both kinematic populations, especially at large stellar ages. This implies that a simple one-to-one relation between ages and metallicities is not possible. In fact, there are stars that are-truly old and at the same time have... (More)
- We test the hypothesis that the spread in the age-metallicity plot of the solar neighborhood is due to a mixture of stars belonging to kinematically different sub-populations of the Galactic disk, i.e., the thin and the thick disk. We use a kinematic subsample of similar to 600 stars from a sample of similar to 6000 dwarf and subgiant stars from the Hipparcos catalog. All of these stars have a full set of stellar parameters determined, including good ages. We find that a significant spread in [Me/H] is present in both kinematic populations, especially at large stellar ages. This implies that a simple one-to-one relation between ages and metallicities is not possible. In fact, there are stars that are-truly old and at the same time have [Me/H] > 0.2 dex. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/1406935
- author
- Feltzing, Sofia LU ; Holmberg, Johan LU and Hurley, J
- organization
- publishing date
- 2002
- type
- Chapter in Book/Report/Conference proceeding
- publication status
- published
- subject
- host publication
- Modes of Star Formation and the Origin of Field Populations, Proceedings
- volume
- 285
- pages
- 243 - 247
- publisher
- Astronomical Society of the Pacific (ASP)
- conference name
- Workshop on Modes of Star Formation and the Origin of Field Populations
- conference location
- Heidelberg, Germany
- conference dates
- 2000-10-09 - 2000-10-13
- external identifiers
-
- wos:000180752500035
- ISBN
- 1-58381-128-1
- language
- English
- LU publication?
- yes
- id
- d79e0e57-1253-46e5-8565-bd8e878ea68a (old id 1406935)
- date added to LUP
- 2016-04-04 10:43:21
- date last changed
- 2020-06-16 15:05:00
@inproceedings{d79e0e57-1253-46e5-8565-bd8e878ea68a, abstract = {{We test the hypothesis that the spread in the age-metallicity plot of the solar neighborhood is due to a mixture of stars belonging to kinematically different sub-populations of the Galactic disk, i.e., the thin and the thick disk. We use a kinematic subsample of similar to 600 stars from a sample of similar to 6000 dwarf and subgiant stars from the Hipparcos catalog. All of these stars have a full set of stellar parameters determined, including good ages. We find that a significant spread in [Me/H] is present in both kinematic populations, especially at large stellar ages. This implies that a simple one-to-one relation between ages and metallicities is not possible. In fact, there are stars that are-truly old and at the same time have [Me/H] > 0.2 dex.}}, author = {{Feltzing, Sofia and Holmberg, Johan and Hurley, J}}, booktitle = {{Modes of Star Formation and the Origin of Field Populations, Proceedings}}, isbn = {{1-58381-128-1}}, language = {{eng}}, pages = {{243--247}}, publisher = {{Astronomical Society of the Pacific (ASP)}}, title = {{The solar neighborhood age-metallicity relation - Does it exist?}}, volume = {{285}}, year = {{2002}}, }