Search

Stars ending with core collapse supernovae (SNe) emit a tremendous number of neutrinos during their explosions. While these neutrinos pass through each layer of the stars, they react with the nuclides in the progenitor. Although the neutrino cross sections are very small, its huge flux is high enough to react with nuclides to change their abundances. We consider this ν-process, by which abundances of some elements may be explained exclusively by this neutrino process. One of the candidates is 98Tc. In this study, we check the ν-process contributions due to the neutrino reactions. In this calculation we also include the neutrino oscillation effect in the matter with varying density, so called MSW effect, not only for 98Tc production but also 4He and 12C destruction, which occurs at first in the He/C layer in the present model.Stars ending with core collapse supernovae (SNe) emit a tremendous number of neutrinos during their explosions. While these neutrinos pass through each layer of the stars, they react with the nuclides in the progenitor. Although the neutrino cross sections are very small, its huge flux is high enough to react with nuclides to change their abundances. We consider this ν-process, by which abundances of some elements may be explained exclusively by this neutrino process. One of the candidates is 98Tc. In this study, we check the ν-process contributions due to the neutrino reactions. In this calculation we also include the neutrino oscillation effect in the matter with varying density, so called MSW effect, not only for 98Tc production but also 4He and 12C destruction, which occurs at first in the He/C layer in the present model.

Previous simulations of X-ray bursts (XRBs), for example, those performed by MESA (Modules for Experiments in Stellar Astrophysics) could not address the dynamical effects of strong radiation, which are important to explain the photospheric radius expansion (PRE) phenomena seen in many XRBs. In order to study the effects of strong radiation, we propose to use SNEC (the SuperNova Explosion Code), a 1D Lagrangian open source code that is designed to solve hydrodynamics and equilibrium-diffusion radiation transport together. Because SNEC is able to control modules of radiation-hydrodynamics for properly mapped inputs, radiation-dominant pressure occurring in PRE XRBs can be handled. Here we present simulation models for PRE XRBs by applying SNEC together with MESA.

It has been known that there is a linearly proportional relationship between the column densities of CH and OH measured toward bright UV-emitting stars, although there are four outliers in this relationship among the total 24 measured targets. By using the Simbad database, we investigate reasonable configurations of diffuse interstellar medium (ISM) which could explain the observed relationship. We first identify the locations of 24 targets on the celestial sphere getting the distances to them and then count the number of molecular clouds, nebulae, and peculiar stars toward the targets which could contribute to the production of OH and CH. We present the results of our search by testing three hypothetical configurations of diffuse ISM which may explain the observed relationship.

Core-collapsed Supernova (CCSN) is one of violent phenomena in the universe. CCSN generates heavy elements and leaves a neutron star behind. It has been known that the physical properties of CCSN depend on those of pre-supernova such as mass, metallicities including distribution of elements, and the density and temperature profile which are obtained from the stellar evolution calculation. In particular, the production of heavy elements in CCSN is sensitive to the abundance profiles in the pre-supernova models. In this study, we evolve a massive main sequence star with 15Msun and solar metallicity to the pre-supernova stage by using two different networks, small and large. The large nuclear reaction network includes more than four times isotopes than the small network. Our calculations were done by MESA (Modules for Experiments in Stellar Astrophysics) which allowed us to use the large network containing about a hundred isotopes. We compare the results obtained with two networks.