Hostname: page-component-7c8c6479df-ws8qp Total loading time: 0 Render date: 2024-03-29T12:39:44.541Z Has data issue: false hasContentIssue false

Galactic Chemical Evolution in the Context of the Recently Revealed SNe Ia Delay Time Distribution

Published online by Cambridge University Press:  17 January 2013

Takuji Tsujimoto*
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan email: taku.tsujimoto@nao.ac.jp
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.

The Galaxy is composed of four distinct structures, i.e., halo, bulge, and thick and thin disks, that are formed and evolved on different timescales; thus accordingly the speeds of chemical enrichment are different from one another, which is imprinted in individual stellar abundances. To decipher them, precise knowledge of the timing of the release of nucleosynthesis materials from various production sites is critical. The delay time distribution (DTD) of Type Ia supernovae (SNe Ia), recently revealed by the SNe Ia surveys of external galaxies, is incorporated into the models of chemical evolution for each structure. Here we report that the observed chemical properties for the thin and thick disks are compatible with a new SNe Ia DTD, and suggests a close chemical connection between the two in the way that the thin disk is formed from gas left after thick disk formation. This nicely explains the lack of thin disk stars with [Fe/H] ≲ −0.8. In this new context, a top-heavy IMF for the bulge is firmly confirmed. Finally we discuss the possibility of some modification of the DTD that might be considered for the halo case.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Bensby, T., et al. 2010, A&A, 512, A41Google Scholar
Bensby, T., Feltzing, S., Lundström, I., & Ilyiin, I. 2005, A&A, 433, 185Google Scholar
Gilroy, K. K., Sneden, C., Pilachowski, C. A., & Cowan, J. J. 1988, ApJ, 327, 298CrossRefGoogle Scholar
Gonzalez, O., A., et al. 2011, A&A, 530, A54Google Scholar
Mannucci, F., Della Valle, M., & Panagia, N. 2006, MNRAS, 370, 773Google Scholar
Maoz, D., Sharon, K., & Gal-Yam, A. 2010, ApJ, 722, 1879Google Scholar
Roederer, I. U., Cowan, J. I., Karakas, A. I., Kratz, K.-L., et al. 2010, ApJ, 724, 975CrossRefGoogle Scholar
Sullivan, M., et al. 2006, ApJ, 648, 868Google Scholar
Totani, T., Morokuma, T., Oda, T., Doi, M., & Yasuda, N. 2008, PASJ, 60, 1327Google Scholar
Tsujimoto, T., Bland-Hawthorn, J., & Freeman, K. C. 2010, PASJ, 62, 447CrossRefGoogle Scholar
Venn, K. A., Irwin, M., Shetrone, M. D., Tout, C. A., Hill, V., & Tolstoy, E. 2004, AJ, 128, 1177Google Scholar