Speaker
Dr
sarmistha banik
(BITS Pilani, Hyderabad)
Description
The equation of state (EoS) of hot and dense matter plays a fundamental role in the understanding of core-collapse supernova.
A phase transition from hadronic to exotic phases might occur
in the early post-bounce phase of a core collapse supernova.
We generate a full tabular equation of state of dense matter with $\Lambda$
hyperons. The $\beta$-equilibrated
EoS involving hyperon-hyperon interaction results in a $2.1 M_{\odot}$ neutron
star, that is compatible with the latest observations. We adopt
a density-dependent relativistic mean field model(DD2) for a broad
range of density
($\sim 10^4-10^{15}$ g/cm$^3$), temperature($T=0.01\quad \mathrm{to}\quad 10^{2.4}$ MeV ) and charge-to-baryon number ratio
($Y_p= 0 \quad \mathrm{to} \quad0.65$ ).
The DD model is exploited to describe uniform and non-uniform
matter in a consistent manner. Further, light and heavy nuclei along with interacting
nucleons are treated in the nuclear statistical equilibrium (NSE) model
of Hempel and Schaffner-Bielich (HS) which includes excluded volume effects
and DD relativistic interactions.
We investigate
the role of strange hyperons in the dynamical collapse of a non-rotating
massive star to a black hole using 1D General relativistic simulation $GR1D$.
We follow the dynamical formation and collapse
of a protoneutron star (PNS) from the gravitational collapse of a massive
progenitor of Wooseley, adopting our DD2 hyperonic EoS. We
also study the neutrino signals that may be used as a probe to core collapse
supernova. We compare our results with those of Shen EoS.
Primary author
Dr
sarmistha banik
(BITS Pilani, Hyderabad)
