2002/06/18 by M. Terasawa, K. Sumiyoshi, S. Yamada +2 · 48 citations
Physics and Astronomy · #Boundary (topology) #Boundary layer #Boundary value problem #Neutrino Physics Research #Neutron #Neutron star #Nuclear physics research studies #Nucleosynthesis #Pulsars and Gravitational Waves Research #Shock wave #Smoothed-particle hydrodynamics #Thermal #astro-ph #nucl-th
paper · pdf · doi:10.1086/344698
published in The Astrophysical Journal 578(2), L137-L140 (IOP Publishing) · 14 pages, 2 figures
arxiv created 2002/06/18 · openalex publication_date 2002/10/08 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We study the effects of the outer boundary conditions in neutrino-driven winds on r -process nucleosynthesis. We perform numerical simulations of hydrodynamics of neutrino-driven winds and nuclear reaction network calculations. As an outer boundary condition of hydrodynamic calculations, we set a pressure upon the outermost layer of the wind, which is approaching toward the shock wall. Varying the boundary pressure, we obtain various asymptotic thermal temperatures of expanding material in the neutrino-driven winds for resulting nucleosynthesis. We find that a slightly lower asymptotic temperature reduces the charged particle reaction rates and the resulting amount of seed elements and leads to a high neutron-to-seed ratio for a successful r -process abundance pattern, which is in reasonable agreement with the solar system r -process abundance pattern. As a result, the asymptotic temperature, slightly lower than those in previous studies of neutrino-driven winds, can lead to a successful r -process even for the typical proto-neutron star mass M NS ~ 1.4 M ☉ . We also explore the relation between the boundary condition and the neutron star mass, which is related to the progenitor mass, for a successful r -process.