The merging of two neutron stars is a true multimessenger event that includes gravitational waves, an electromagnetic signal, and the emission of enormous numbers of neutrinos. In order to understand these signals we need a careful accounting of the microphysics that occurs during and after the merger. I will focus on the elements produced in these objects and the effect of two aspects of this...
The properties of nuclear matter at extremely high densities and temperatures remain a mystery. This talk discusses two environments for which the nuclear matter can be found at the highest densities. These are: during the collapse of the core of a massive star to form a supernova or black hole; and during the merger of two neutron stars to form a black hole. Here, we highlight recent...
We study the sensitivity of the r-process nucleosynthesis to the nuclear reactions of light nuclei.
We first update nuclear reaction data in Libnucnet code if available in experiments. We then calculate the r-process nucleosynthesis in the core-collapse supernovae and collapsar. For core-collapse supernovae we consider two different scenarios: the magnetohydrodynamic (MHD) jet model and a...
Metal-poor stars are thought to have the result of nucleosynthesis in the early stages of galaxy formation in their atmospheres. A variety of surveys and follow-up observations have been performed to determine detailed abundance patterns for many metal-poor stars. The r-process, which provides about a half of the elements heavier than iron, is thought to be caused by neutron star mergers....
Magnetorotational-driven supernovae (MRNSe) are a peculiar type of core-collapse SNe. Their progenitors are fast-rotating massive stars with strong magnetic fields and they are candidates for the central engine of hypernovae and gamma-ray bursts. They are also expected to be astronomical sites for the r-process, as they have a different explosion mechanism from regular SNe. MRSNe may have very...
Half of the elements heavier than iron are produced by a sequence of neutron captures, beta-decays and fission known as r-process. It requires an astrophysical site that ejects material with extreme neutron rich conditions. Once the r-process ends, the radioactive decay of the freshly synthesized material is able to power an electromagnetic transient with a typical intrinsic luminosity. Such...
More than 30 years after the discovery of SN 1987A, it entered a phase of a young supernova remnant. It is considered that molecules and dust are formed in the ejecta. Actually, recent ALMA observations (Abellán et al. 2017) have revealed that the 3D distribution of carbon monoxide (CO) and silicon monoxide (SiO) is rather non-spherical and lumpy. However, how molecules are formed in...
The light heavy elements between strontium and silver, can be synthesized in a primary process in either neutron- (weak r-process) or proton-rich (νp-process) neutrino-driven outflows of explosive environments [1]. Constraining the nuclear physics uncertainties, for example the (α,xn) reaction rates in the weak r-process [2,3], allows us to investigate the conditions that create the light ...
Neutron-capture processes made most of the abundances of heavy elements in the Solar System, however they cannot produce a number of rare proton-rich stable isotopes lying on the left side of the valley of stability. The p-process, or $\gamma$-process, is recognised and generally accepted as a feasible process for the synthesis of proton-rich nuclei in core collapse supernovae. However this...
A huge number of neutrinos emitted in a supernova explosion interact with a dense plasma. The interaction between neutrinos and electrons remarkably changes the neutrino oscillation probability at the specific electron density, known as the Mikheyev–Smirnov–Wolfenstein (MSW) resonance effect. Previous studies for the neutrino-process in core-collapsing supernova have well-established the...
