Abstract
This poster illustrates the results of ongoing simulations – within our previously developed modeling framework – allowing for stochastic accretion within closed and open systems. All models include three “zones” (halo, thick disk, and thin disk) and are initialized with only the halo, the abundances for which are assumed to be primordial. The time history of star formation is computed directly from the model equations rather than being assumed a priori without instantaneous recycling [1]. The yields and deterministic rates are the same as used in our previous work [2]. f stoc
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References
1. Ferrini, F., Matteucci, F., Pardi, M. C., & Penco, U., 1992, ApJ, 387, 138
2. Valle, G., Ferrini, F., Galli, D., & Shore, S. N., 2002, ApJ, 566, 252
3. Comins, N.F. & Shore, S.N. 1990, A&A 237, 345
4. Quilis, V., Moore, B., & Bower, R., 2000, Science, 288, 1617
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Valle, G., Shore, S., Galli, D. (2006). Multipopulation Models for Galactic Star Formation and Chemical Evolution. Effects of Stochastic Accretion and Collisional Stripping (Especially for Deuterium). In: Randich, S., Pasquini, L. (eds) Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites. ESO ASTROPHYSICS SYMPOSIA. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-34136-9_118
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DOI: https://doi.org/10.1007/978-3-540-34136-9_118
Publisher Name: Springer, Berlin, Heidelberg
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