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  1. ; ; ; ; ; ( , Astronomy & Astrophysics)
    Context. Pulsational pair-instability supernovae (PPISNe) and pair instability supernovae (PISNe) are the result of a thermonuclear runaway in the presence of a background electron-positron pair plasma. As such, their evolution and resultant black hole masses could possibly be affected by screening corrections due to the electron pair plasma. Aims. The sensitivity of PISNe and PPISNe to relativistic weak screening has been explored. Methods. In this paper a weak screening model that includes effects from relativistic pair production has been developed and applied at temperatures approaching and exceeding the threshold for pair production. This screening model replaces “classical” screening commonly usedmore »in astrophysics. Modifications to the weak screening electron Debye length were incorporated in a computationally tractable analytic form. Results. In PPISNe the BH masses were found to increase somewhat at high temperatures, though this increase is small. The BH collapse is also found to occur at earlier times, and the pulsational morphology also changes. In addition to the resultant BH mass, the sensitivity to the screening model of the pulsational period, the pulse structure, the PPISN-to-PISN transition, and the shift in the BH mass gap has been analyzed. The dependence of the composition of the ejected mass was also examined.« less
    Free, publicly-accessible full text available March 1, 2023
  2. ( , Journal of Physics: Conference Series)
    Abstract Entanglement of constituents of a many-body system is a recurrent feature of quantum behaviour. Quantum information science provides tools, such as the entanglement entropy, to help assess the amount of entanglement in such systems. Many-neutrino systems are present in core-collapse supernovae, neutron star mergers, and the Early Universe. Recent work in applying the tools of quantum information science to the description of the entanglement in astrophysical many-neutrino systems is reviewed.
    Free, publicly-accessible full text available February 1, 2023
  3. ; ; ; ; ( , EPJ Web of Conferences)
    Liu, W. ; Wang, Y. ; Guo, B. ; Tang, X. ; Zeng, S. (Ed.)
    We study the v\bar v\-pair emission from electrons and protons in a relativistic quantum approach. In this work we calculate the luminosity of the v\bar v\-pairs emitted from neutron-star-matter with a strong magnetic field, and find that this luminosity is much larger than that in the modified Urca process. The v\bar v\-pair emission processes in strong magnetic fields significantly contribute to the cooling of the magnetars.
    Free, publicly-accessible full text available January 1, 2023
  4. ; ; ; ( , Astroparticle Physics)
    Free, publicly-accessible full text available July 1, 2022
  5. ; ; ; ; ; ; ; ; ; ; et al ( , Journal of Physics G: Nuclear and Particle Physics)
    Free, publicly-accessible full text available June 14, 2022
  6. ; ; ; ; ; ; ( , Monthly Notices of the Royal Astronomical Society)
    ABSTRACT The joint detection of the gravitational wave GW170817, of the short γ-ray burst GRB170817A and of the kilonova AT2017gfo, generated by the the binary neutron star (NS) merger observed on 2017 August 17, is a milestone in multimessenger astronomy and provides new constraints on the NS equation of state. We perform Bayesian inference and model selection on AT2017gfo using semi-analytical, multicomponents models that also account for non-spherical ejecta. Observational data favour anisotropic geometries to spherically symmetric profiles, with a log-Bayes’ factor of ∼104, and favour multicomponent models against single-component ones. The best-fitting model is an anisotropic three-component composed ofmore »dynamical ejecta plus neutrino and viscous winds. Using the dynamical ejecta parameters inferred from the best-fitting model and numerical–relativity relations connecting the ejecta properties to the binary properties, we constrain the binary mass ratio to q < 1.54 and the reduced tidal parameter to $120\lt \tilde{\Lambda }\lt 1110$. Finally, we combine the predictions from AT2017gfo with those from GW170817, constraining the radius of a NS of 1.4 M⊙ to 12.2 ± 0.5 km (1σ level). This prediction could be further strengthened by improving kilonova models with numerical-relativity information.« less
    Free, publicly-accessible full text available June 4, 2022
  7. ; ; ; ( , Physical Review D)
    Free, publicly-accessible full text available June 1, 2022
  8. ; ; ; ; ( , Physical Review D)
    Free, publicly-accessible full text available June 1, 2022
  9. ; ; ( , Physics Reports)
    Free, publicly-accessible full text available June 1, 2022
  10. ; ; ; ; ; ; ( , Progress in Particle and Nuclear Physics)
    Free, publicly-accessible full text available June 1, 2022