Highly dense and isospin asymmetric matter is partly out of the reach of nuclear laboratories on Earth. Our theoretical understanding of strong and nuclear forces at high density and relatively low temperatures is also limited such that the equation of state and properties of dense matter remains a mystery. However, this particular type of matter comprises the deepest shells of the highly...
In previous work [1] we demonstrated that a crossover transition from hadronic to quark matter during the merger of binary neutron stars can lead to interesting observational consequences in the emergent gravitational waves. In particular, quark matter may cause increased pressure in the crossover density region (2-5 times the nuclear saturation density). This could lead to an extended...
Observations of GW170817 strongly suggest that binary neutron star mergers produce rapid neutron-capture nucleosynthesis (r-process) elements. However, it remains an open question whether these mergers can account for al the r-process element enrichment in the Milky Way's history. In particular, the neutron star merger-only enrichment scenario has been shown to be inconsistent with the...
Understanding gravitational-wave observations of binary neutron star mergers requires a knowledge of high-density matter. In turn, the electromagnetic signal is by-and-large determined by r-process elements and hence it requires accurate knowledge of the underlying nucleosynthesis processes. In this talk, I will present first nuclear physics results that aim at elucidating the thermal...
Neutron star equations of state based on Skyrme-interaction are one of the most widely used models to describe ultra-dense nuclear matter at the interior of these degenerate stars. In this presentation, I will discuss the effect of various Skyrme parameters on the stellar structural properties of a neutron star and its observables. I will also briefly present the potential source of biases in...
We perform three-dimensional supernova simulations with a phenomenological treatment of neutrino flavor conversions. We show that the explosion energy can increase to as high as $\sim10^{51}$ erg depending on the critical density for the onset of flavor conversions, due to a significant enhancement of the mean energy of electron antineutrinos. Our results confirm previous studies showing such...
