Conveners
Explosive Stellar Objects and Nuclear Physics
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Explosive Stellar Objects and Nuclear Physics
- Jordi Jose
Explosive Stellar Objects and Nuclear Physics
- There are no conveners in this block
Explosive Stellar Objects and Nuclear Physics
- There are no conveners in this block
Classical novae are a class of thermonuclear explosions that involve mass-accreting white dwarfs. The low-mass, main sequence companion (or a red giant, particularly for recurrent novae) overfills its Roche lobe and matter flows through the inner Lagrangian point of the system. While most nova simulations have focused on the early stages of the explosion and ejection, it is clear that a...
With the detection of multiple neutron-star merger events in the last few years, the need for a more comprehensive understanding of nuclear and atomic properties as well as radiative transfer has become increasingly important. Despite our current understanding, there are still large discrepancies in the opacities obtained from different codes and methods. These discrepancies lead to variations...
The progenitors of many supernovae are expected to be in binary systems. After the supernova explosion in a binary system, the companion star may suffer from mass stripping and be shock heated and polluted with heavy elements as a result of the impact of the supernova ejecta. If the binary system is disrupted by the supernova explosion, the companion star is ejected as a runaway star, and in...
The merger of two neutron stars and the collapses of rotating massive stars can form a system composed of a central object (either a neutron star or black hole) and a centrifugally supported disk. Inside the disk, a turbulent state is generated by magnetorotational instability and then induces an effective viscosity. The viscous angular momentum transport and heating can evolve the system and...
Neutrinos can play an important role in the synthesis of nuclides in high energy astrophysical processes involving compact objects, such as core-collapse supernovae or binary neutron star mergers, where neutrinos can experience collective flavor oscillations driven by neutrino-neutrino interactions. Here, we seek to explore the possible influences of neutrino interactions on the heavy-element...
Core-collapse supernovae can be a copious source of sterile neutrinos, hypothetical particles that mix with active neutrinos. We develop two-dimensional stellar core-collapse models that incorporate the mixing between tau neutrinos and heavy sterile neutrinos---those with the mass of 150--200 MeV---to investigate signatures of sterile neutrinos in supernova observables. We find that the decay...
Pair-instability supernovae (PISNe) are the final fates of massive stars with an initial mass ranging from 140-260 $M_{\odot}$. Unlike other supernovae, PISNe do not leave behind compact objects. Stellar evolution theory predicts a gap in the distribution of black hole masses due to PISNe. Recent works suggested that the uncertainty may influence the location of this gap in the...
Strong magnetic fields could exist in the inner regions of a supernova. Inside these magnetic fields, the phase space of the electrons becomes quantized. As a result, the rates of weak interaction processes can deviate from the field-free case.
This talk focuses on the absorption and emission process of (anti)neutrinos in such strong fields. This process is crucial, as it determines the...
Massive stars ($>10M_{\odot}$) undergo core-collapse supernova explosions at the end of their evolution. These explosions release elements ranging from helium to the iron peak, which are (produced during the stellar evolution) to iron peak elements (synthesized in explosive nucleosynthesis near the supernova core region). Although the explosion mechanism of core-collapse supernovae is not...
