Investigating Possible Existence of Hyper-Heavy Nuclei in Neutron Star Environment
arXiv:2205.00478 · doi:10.1103/PhysRevC.106.L012802
Abstract
The synthesis of hyper-heavy elements is investigated under conditions simulating neutron star environment. The Constrained Molecular Dynamics (CoMD) approach is used to simulate low energy collisions of extremely n-rich nuclei. A new type of the fusion barrier due to a "neutron wind" is observed when the effect of neutron star environment (screening of Coulomb interaction) is introduced implicitly. When introducing also a background of surrounding nuclei, the nuclear fusion becomes possible down to temperatures of 10 K and synthesis of extremely heavy and n-rich nuclei appears feasible. A possible existence of hyper-heavy nuclei in a neutron star environment could provide a mechanism of extra coherent neutrino scattering or an additional mechanism, resulting in X-ray burst or a gravitational wave signal and, thus, becoming another crucial process adding new information to the suggested models on neutron star evolution.
arXiv comment10 pages, 5 figures
References in corpus (19)
- R-Process Nucleosynthesis in Dynamically Ejected Matter of Neutron Star Mergers
- Constraint Molecular Dynamics approach to Fermionic systems
- Inner crust of neutron stars with mass-fitted Skyrme functionals
- A New Equation of State for Astrophysical Simulations
- Nuclear Physics of the Outer Layers of Accreting Neutron Stars
- Nuclear Reactions in the Crusts of Accreting Neutron Stars
- The Neutron Star Crust: Nuclear Physics Input
- Hyperheavy nuclei: existence and stability
- Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants
- A realistic model of superfluidity in the neutron star inner crust
- Equation of state for -stable hot nuclear matter
- Heavy Nuclei as Thermal Insulation for Proto-Neutron Stars
- Microscopic dynamical description of proton-induced fission with the Constrained Molecular Dynamics (CoMD) Model
- Properties of the neutron star crust: Quantifying and correlating uncertainties with improved nuclear physics
- Hot neutron stars and their equation of state
- Constraining the equation of state of nuclear matter from competition of fusion and quasi-fission in the reactions leading to production of the superheavy elements
- Simulation of fusion and quasi-fission in nuclear reactions leading to production of superheavy elements using the Constrained Molecular Dynamics model
- Microscopic description of proton-induced spallation reactions with the Constrained Molecular Dynamics (CoMD) Model
- Thermal impacts on the properties of nuclear matter and young neutron star