Neutrino-driven winds and nucleosynthesis
Abstract
Baryonic outflows from proto-neutron stars formed in core-collapse supernova explosions are one of the possible scenarios for the production of heavy elements via the r-process. If the ejected matter reaches supersonic velocities the outflow is known as neutrino-driven wind. We have studied the long-time evolution of proto-neutron stars with one- and two-dimensional hydrodynamical simulations and performed nucleosynthesis calculations with the resulting wind trajectories. We find that the present wind models are much closer than previous studies to provide suitable conditions for r-process nucleosynthesis. Moreover, we explored the effect of the wind terminations shock, nuclear physics input, and composition of the outer layers of the neutron star on the nucleosynthesis production.
Additional Information
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-ShareAlike. Supported by the Deutsche Forschungsgemeinschaft through contract SFB 634.Attached Files
Published - NIC_X_128.pdf
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Additional details
- Eprint ID
- 89234
- Resolver ID
- CaltechAUTHORS:20180828-122925049
- SFB 634
- Deutsche Forschungsgemeinschaft (DFG)
- Created
-
2018-08-30Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
- Series Name
- Proceedings of Science
- Series Volume or Issue Number
- 53