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Equation of State of Stellar Matter in Wide Thermodynamic Domain: A Study on Core-Collapse Supernovae

This study explores the equation of state of stellar matter in diverse thermodynamic settings, crucial for understanding core-collapse supernovae. It delves into topics such as Nuclear Statistical Equilibrium (NSE) and shock wave formation in collapsing stellar cores. The research highlights the Nuclear Physics perspectives, neutron stars, and neutrino-matter interactions in supernovae.

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Equation of State of Stellar Matter in Wide Thermodynamic Domain: A Study on Core-Collapse Supernovae

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  1. Equation of state of stellar matter in a wide domain of thermodynamic  parameters, characteristic for CCSN

  2. From: T. Fischer, M. Hempel, I. Sagert, Y. Suwa, and J. Schaffner-Bielich, Eur. Phys. J. A (2014) 50: 46

  3. Nuclear Statistical Equilibrium (NSE) T9  3–4 (T9=T/109) i=(A,Z)

  4. EoS under the conditions ofNSE 1,

  5. Electron-positron gas phase diagram

  6. The shock wave formation into a collapsing stellar core t = -0.9 ms t = 0.0 ms t = 10 ms t = 1.0 ms

  7. Brookhaven national laboratory

  8. Single nucleus approximation G. BAYM, H.A. BETHE, C.J. PETHICK Nuclear Physics A175 (1971) 225-27 1

  9. Oyamatsu, Nuclear Physics A561 (1993) 431-452 S.B. R.uster, M. Hempel, and J. Schaffner-Bielich “The outer crust of non-accreting cold neutron stars”

  10. S. Kreima, M. Hempel, D. Lunneyd, J. Schaffner-Bieliche “Nuclear Masses and Neutron Stars”

  11. R. Kaiser

  12. K. Oyamatsu, Nuclear Physics A 561 (1993) 431-452 C. J. Horowitz: Links Between Heavy Ion and Astrophysics

  13. Pure uniform nuclear matter F.D. Swesty, J.M. Lattimer, E.S. Myra, Astroph. J. 425, 195-204 (1993) “Thermal properties of supernova matter: The bulk homogeneous phase” C. Constantinou, B. Muccioli,M. Prakash,J. M. Lattimer

  14. From: T. Fischer, M. Hempel, I. Sagert, Y. Suwa, and J. Schaffner-Bielich, Eur. Phys. J. A (2014) 50: 46

  15. Equation of state of dense matter The ravine of instability Sly EOS; Douchin & Haensel (2001)

  16. Neutrino-matter interaction rates and neutrino transport

  17. Kνи Sν– the energy and impulse fluxes, Uν– energy density of neutrinos, andμ–cosine of the angle between radius-vector and the neutrino direction.

  18. Neutrino heat conduction

  19. G. Rafelt, Astrophys. J. 561 (2001) 890.

  20. A. Burrows, T.A. Thompson NEUTRINO-MATTER INTERACTION RATESIN SUPERNOVAE

  21. S.W. Bruenn Astroph. J. Suppl. S., 58:771-841 (1985)

  22. Oscillations C. Lunardinia, I. Tamborra “Difuse supernova neutrinos:oscillation eects, stellar cooling and progenitor mass dependence Kotake et al 2006

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