225 research outputs found
Long-term evolution of massive star explosions
We examine simulations of core-collapse supernovae in spherical symmetry. Our
model is based on general relativistic radiation hydrodynamics with
three-flavor Boltzmann neutrino transport. We discuss the different supernova
phases, including the long-term evolution up to 20 seconds after the onset of
explosion during which the neutrino fluxes and mean energies decrease
continuously. In addition, the spectra of all flavors become increasingly
similar, indicating the change from charged- to neutral-current dominance.
Furthermore, it has been shown recently by several groups independently, based
on sophisticated supernova models, that collective neutrino flavor oscillations
are suppressed during the early mass-accretion dominated post-bounce evolution.
Here we focus on the possibility of collective flavor flips between electron
and non-electron flavors during the later, on the order of seconds, evolution
after the onset of an explosion with possible application for the
nucleosynthesis of heavy elements.Comment: 12 pages, 7 figures, conference proceeding, HANSE 2011 worksho
WKB approximation for multi-channel barrier penetrability
Using a method of local transmission matrix, we generalize the well-known WKB
formula for a barrier penetrability to multi-channel systems. We compare the
WKB penetrability with a solution of the coupled-channels equations, and show
that the WKB formula works well at energies well below the lowest adiabatic
barrier. We also discuss the eigen-channel approach to a multi-channel
tunneling, which may improve the performance of the WKB formula near and above
the barrier.Comment: 15 pages, 4 eps figure
Presupernova collapse models with improved weak-interaction rates
Improved values for stellar weak interaction rates have been recently
calculated based upon a large shell model diagonalization. Using these new
rates (for both beta decay and electron capture), we have examined the
presupernova evolution of massive stars in the range 15-40 Msun. Comparing our
new models with a standard set of presupernova models by Woosley and Weaver, we
find significantly larger values for the electron-to-baryon ratio Ye at the
onset of collapse and iron core masses reduced by approximately 0.1 Msun. The
inclusion of beta-decay accounts for roughly half of the revisions, while the
other half is a consequence of the improved nuclear physics. These changes will
have important consequences for nucleosynthesis and the supernova explosion
mechanism.Comment: 4 pages, 2 figure
Effects of Inelastic Neutrino-Nucleus Scattering on Supernova Dynamics and Radiated Neutrino Spectra
Based on the shell model for Gamow-Teller and the Random Phase Approximation
for forbidden transitions, we have calculated reaction rates for inelastic
neutrino-nucleus scattering (INNS) under supernova (SN) conditions, assuming a
matter composition given by Nuclear Statistical Equilibrium. The rates have
been incorporated into state-of-the-art stellar core-collapse simulations with
detailed energy-dependent neutrino transport. While no significant effect on
the SN dynamics is observed, INNS increases the neutrino opacities noticeably
and strongly reduces the high-energy tail of the neutrino spectrum emitted in
the neutrino burst at shock breakout. Relatedly the expected event rates for
the observation of such neutrinos by earthbound detectors are reduced by up to
about 60%.Comment: 4 pages, 2 figures, 1 tabl
Theory of Core-Collapse Supernovae
Advances in our understanding and the modeling of stellar core-collapse and
supernova explosions over the past 15 years are reviewed, concentrating on the
evolution of hydrodynamical simulations, the description of weak interactions
and nuclear equation of state effects, and new insights into the
nucleosynthesis occurring in the early phases of the explosion, in particular
the neutrino-p process. The latter is enabled by the proton-richness of the
early ejecta, which was discovered because of significant progress has been
made in the treatment of neutrino transport and weak interactions. This
progress has led to a new generation of sophisticated Newtonian and
relativistic hydrodynamics simulations in spherical symmetry. Based on these,
it is now clear that the prompt bounce-shock mechanism is not the driver of
supernova explosions, and that the delayed neutrino-heating mechanism can
produce explosions without the aid of multi-dimensional processes only if the
progenitor star has an ONeMg core inside a very dilute He-core, i.e., has a
mass in the 8--10 solar mass range. Hydrodynamic instabilities of various kinds
have indeed been recognized to occur in the supernova core and to be of
potential importance for the explosion. Neutrino-driven explosions, however,
have been seen in two-dimensional simulations with sophisticated neutrino
transport so far only when the star has a small iron core and low density in
the surrounding shells as being found in stars near 10--11 solar masses. The
explosion mechanism of more massive progenitors is still a puzzle. It might
involve effects of three-dimensional hydrodynamics or might point to the
relevance of rapid rotation and magnetohydrodynamics, or to still incompletely
explored properties of neutrinos and the high-density equation of state.Comment: 49 pages, 20 figures; submitted to the Bethe Centennial Volume of
Physics Report
Clarification of the relationship between bound and scattering states in quantum mechanics: Application to 12C + alpha
Using phase-equivalent supersymmetric partner potentials, a general result
from the inverse problem in quantum scattering theory is illustrated, i.e.,
that bound-state properties cannot be extracted from the phase shifts of a
single partial wave, as a matter of principle. In particular, recent R-matrix
analyses of the 12C + alpha system, extracting the asymptotic normalization
constant of the 2+ subthreshold state, C12, from the l=2 elastic-scattering
phase shifts and bound-state energy, are shown to be unreliable. In contrast,
this important constant in nuclear astrophysics can be deduced from the
simultaneous analysis of the l=0, 2, 4, 6 partial waves in a simplified
potential model. A new supersymmetric inversion potential and existing models
give C12=144500+-8500 fm-1/2.Comment: Expanded version (50% larger); three errors corrected (conversion of
published reduced widths to ANCs); nine references added, one remove
Role of virtual break-up of projectile in astrophysical fusion reactions
We study the effect of virtual Coulomb break-up, commonly known as the dipole
polarizability, of the deuteron projectile on the astrophysical fusion reaction
3He(d,p)4He. We use the adiabatic approximation to estimate the potential shift
due to the E1 transition to the continuum states in the deuteron, and compute
the barrier penetrability in the WKB approximation. We find that the
enhancement of the penetrability due to the deuteron break-up is too small to
resolve the longstanding puzzle observed in laboratory measurements that the
electron screening effect is surprisingly larger than theoretical prediction
based on an atomic physics model. The effect of the 3He break-up in the
3He(d,p)4He reaction, as well as the 7Li break-up in the 7Li(p,alpha)4He
reaction is also discussed.Comment: 9 pages, 2 eps figure
SMMC method for two-neutrino double beta decay
Shell Model Monte Carlo (SMMC) techniques are used to calculate two-neutrino
double beta decay matrix elements. We validate the approach against direct
diagonalization for Ca in the complete -shell using the KB3
interaction. The method is then applied to the decay of Ge in the
model space using a newly calculated realistic
interaction. Our result for the matrix element is MeV, in
agreement with the experimental value.Comment: 10 pages, 3 figures available at
http://www.krl.caltech.edu/preprints/MAP.htm
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