Proto-Neutron Star Convection and the Neutrino-Driven Wind: Implications for the r-Process
arXiv:2302.01249 · doi:10.1093/mnras/stad372
Abstract
The neutrino-driven wind from proto-neutron stars is a proposed site for r-process nucleosynthesis, although most previous work has found that a wind heated only by neutrinos cannot produce the third r-process peak. However, several groups have noted that introducing a secondary heating source within the wind can change the hydrodynamic conditions sufficiently for a strong r-process to proceed. One possible secondary heating source is gravito-acoustic waves, generated by convection inside the proto-neutron star. As these waves propagate into the wind, they can both accelerate the wind and shock and deposit energy into the wind. Additionally, the acceleration of the wind by these waves can reduce the total number of neutrino captures and thereby reduce the final electron fraction of the wind. In neutron rich conditions, all of these effects can make conditions more favorable for r-process nucleosynthesis. Here, we present a systematic investigation of the impact of these convection-generated gravito-acoustic waves within the wind on potential nucleosynthesis. We find that wave effects in the wind can generate conditions favorable for a strong r-process, even when the energy flux in the waves is a factor of smaller than the total neutrino energy flux and the wind is marginally neutron-rich. Nevertheless, this depends strongly on the radius at which the wave become non-linear and form shocks. We also find that both entropy production after shock formation and the acceleration of the wind due to stresses produced by the waves prior to shock formation impact the structure and nucleosynthesis of these waves.
arXiv comment14 pages, 14 figures, accepted for publication in MNRAS
References in corpus (24)
- Nucleosynthesis in neutrino-driven winds: I. The physical conditions
- Evolution of Protoneutron Stars
- Protoneutron star evolution and the neutrino driven wind in general relativistic neutrino radiation hydrodynamics simulations
- The Physics of Protoneutron Star Winds: Implications for r-Process Nucleosynthesis
- Nucleosynthesis in neutrino-driven winds: II. Implications for heavy element synthesis
- Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric hydrodynamic simulations
- General relativistic effects on neutrino-driven wind from young, hot neutron star and the r-process nucleosynthesis
- Charged-current weak interaction processes in hot and dense matter and its impact on the spectra of neutrinos emitted from proto-neutron star cooling
- Medium modification of the charged current neutrino opacity and its implications
- The r-process in proto-neutron-star wind revisited
- Neutrino-driven wind simulations and nucleosynthesis of heavy elements
- Proto-Neutron Star Winds with Magnetic Fields and Rotation
- SkyNet: A modular nuclear reaction network library
- Multi-Dimensional Radiation/Hydrodynamic Simulations of Protoneutron Star Convection
- General relativistic effects in the neutrino-driven wind and r-process nucleosynthesis
- A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations
- Impact of neutrino flavor oscillations on the neutrino-driven wind nucleosynthesis of an electron-capture supernova
- Supernova neutrino signals based on long-term axisymmetric simulations
- Alfven Wave-Driven Proto-Neutron Star Winds And R-Process Nucleosynthesis
- High-entropy ejections from magnetized proto-neutron star winds: implications for heavy element nucleosynthesis
- Neutrino-heated winds from rotating proto-magnetars
- Neutrino Signatures From Young Neutron Stars
- Active-sterile Neutrino Oscillations in Neutrino-driven Winds: Implications for Nucleosynthesis
- Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism