Abstract
The strongly magnetized degenerate astrophysical plasma is investigated.Arelativistic Hartree self-consistent field method is applied to calculate the screening potential. A profile froma15M⊙ core collapsing supernova (SN) progenitor is applied to evaluate the electron-capture rates of 54Fe. It is found that the screening potential at high field is enhanced compared with the previous study. If the field is high enough and only the lowest Landau level is allowed, two orders of magnitude reduction of the capture rates are found in the high-density region. Such deviations of the electron capture rates are essential since the rates determine the neutron richness of the progenitor model as well as the iron core mass, which are crucial for MHD-Jet SNe explosion calculation.
Highlights
The weak interactions determine the nucleosynthetic path in the supernovae (SNe) and its explosion models [1,2,3,4]
For an extremely strong magnetic field, EF decreases monotonically as a function of B, only the Lowest Landau Level (LLL) is occupied, and the value of fi j shows the same trend since the Fermi energy determines the maximum energy of electrons
All the rates are converged to the same value for electron chemical potentials μe larger than about 25 MeV, while at lower μe values, the capture rates are more sensitive to the magnetic field strengths
Summary
The weak interactions determine the nucleosynthetic path in the supernovae (SNe) and its explosion models [1,2,3,4]. For the MHD-Jet SNe, it is believed that the collapsing and bouncing phases have relativistic degenerate electron gas in a strong magnetic field of the order of 1014−16 G [5] in the inner region. The thermodynamics of the electrons (positrons) in such an environment is different from the field-free case and could further deviate the nuclear weak interactions significantly. Prompted by this fact, this work focuses on the microscopic effects of the relativistic, magnetized degenerate plasmas on the weak interactions. The results are essential to determine the iron core mass before the explosion and the electron fraction Ye during SN’s collapsing phase
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