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Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r‐process nuclei
The most promising astrophysical sources of kHz gravitational waves (GWs) are the inspiral and merger of binary neutron star(NS)/black hole systems. Maximizing the scientific return of a GW detection…
Neutrino-induced nucleosynthesis of A>64 nuclei: the nu p process.
In this process, antineutrino absorptions in the proton-rich environment produce neutrons that are immediately captured by neutron-deficient nuclei, allowing for the nucleosynthesis of nuclei with mass numbers A>64, , making this process a possible candidate to explain the origin of the solar abundances of (92,94)Mo and (96,98)Ru.
Theory of core-collapse supernovae
Muon Creation in Supernova Matter Facilitates Neutrino-Driven Explosions.
- R. Bollig, H. Janka, A. Lohs, G. Martínez-Pinedo, C. Horowitz, T. Melson
- PhysicsPhysical review letters
- 14 June 2017
The appearance of muons softens the NS equation of state, triggers faster NS contraction, and thus leads to higher luminosities and mean energies of the emitted neutrinos, which strengthens the postshock heating by neutrines and can facilitate explosions by the neutrino-driven mechanism.
Composition of the Innermost Core-Collapse Supernova Ejecta
With currently known input physics and computer simulations in one dimension, a self-consistent treatment of core-collapse supernovae does not yet lead to successful explosions, while two-dimensional…
Energy density functional study of nuclear matrix elements for neutrinoless ββ decay.
We present an extensive study of nuclear matrix elements (NME) for the neutrinoless double-beta decay of the nuclei 48Ca, 76Ge, 82Se, 96Zr, 100Mo, 116Cd, 124Sn, 128Te, 130Te, 136Xe, and 150Nd based…
ADVANCED BURNING STAGES AND FATE OF 8–10 M☉ STARS
The stellar mass range 8 ≲ M/M☉ ≲ 12 corresponds to the most massive asymptotic giant branch (AGB) stars and the most numerous massive stars. It is host to a variety of supernova (SN) progenitors and…
The Role of Electron Captures in Chandrasekhar-Mass Models for Type Ia Supernovae
The Chandrasekhar-mass model for Type Ia supernovae (SNe Ia) has received increasing support from recent comparisons of observations with light-curve predictions and modeling of synthetic spectra. It…
Electron capture rates on nuclei and implications for stellar core collapse.
This work has calculated rates for electron capture on nuclei with mass numbers A=65-112 for the temperatures and densities appropriate for core collapse to find that these rates are large enough so that, in contrast to previous assumptions, electron capture in nuclei dominates over capture on free protons.
Consequences of nuclear electron capture in core collapse supernovae.
With realistic treatment of electron capture on heavy nuclei come significant changes in the hydrodynamics of core collapse and bounce, as well as the ramifications for the postbounce evolution in core collapse supernovae.