Speaker
Description
Strong first-order QCD phase transitions from hadronic to quark matter can produce disconnected hybrid-star branches, and the evolution and fate of stellar configurations close to the onset of the unstable branch triggered by the phase transition may depend on finite-temperature and composition effects in the equation of state (EOS). To investigate these aspects, we perform three-dimensional (3D) general relativistic hydrodynamic (GRHD) simulations using the WhiskyTHC code, and adopt representative hybrid-star EOSs with a Maxwell construction. We compare four thermodynamic treatments of the hybrid EOS: (i) a cold barotropic EOS implemented with constant thermal gamma-law pressures, (ii) a specific table imposed with fixed temperature, (iii) a specific table enforced with beta equilibrium conditions, and (iv) a full 3D table $P(\rho,T,Y_e)$. Under all four EOS treatments, configurations initialized on the stable hybrid branch remain on this branch throughout the evolution and retain their quark cores. For typical hybrid configurations on the unstable branch, our results indicate that only the full 3D table preserves a hot, low-Ye quark core over our simulation timescale, highlighting the significance of incorporating realistic microphysics in evaluating the dynamics and stability of hybrid stars.
| Academic Status | I am a Ph.D. student |
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