269 research outputs found
Type Ia Supernova: Burning and Detonation in the Distributed Regime
A simple, semi-analytic representation is developed for nuclear burning in
Type Ia supernovae in the special case where turbulent eddies completely
disrupt the flame. The speed and width of the ``distributed'' flame front are
derived. For the conditions considered, the burning front can be considered as
a turbulent flame brush composed of corrugated sheets of well-mixed flames.
These flames are assumed to have a quasi-steady-state structure similar to the
laminar flame structure, but controlled by turbulent diffusion. Detonations
cannot appear in the system as long as distributed flames are still
quasi-steady-state, but this condition is violated when the distributed flame
width becomes comparable to the size of largest turbulent eddies. When this
happens, a transition to detonation may occur. For current best estimates of
the turbulent energy, the most likely density for the transition to detonation
is in the range 0.5 - 1.5 x 10^7 g cm^{-3}.Comment: 12 pages, 4 figure
Cluster virial expansion for nuclear matter within a quasiparticle statistical approach
Correlations in interacting many-particle systems can lead to the formation
of clusters, in particular bound states and resonances. Systematic quantum
statistical approaches allow to combine the nuclear statistical equilibrium
description (law of mass action) with mean-field concepts. A chemical picture,
which treats the clusters as distinct entities, serves as an intuitive concept
to treat the low-density limit. Within a generalized Beth-Uhlenbeck approach,
the quasiparticle virial expansion is extended to include arbitrary clusters,
where special attention must be paid to avoid inconsistencies such as double
counting. Correlations are suppressed with increasing density due to Pauli
blocking. The contribution of the continuum to the virial coefficients can be
reduced by considering clusters explicitly and introducing quasiparticle
energies. The cluster-virial expansion for nuclear matter joins known
benchmarks at low densities with those near saturation density.Comment: 18 pages, 6 figures, 2 table
Symmetry energy of dilute warm nuclear matter
The symmetry energy of nuclear matter is a fundamental ingredient in the
investigation of exotic nuclei, heavy-ion collisions and astrophysical
phenomena. New data from heavy-ion collisions can be used to extract the free
symmetry energy and the internal symmetry energy at subsaturation densities and
temperatures below 10 MeV. Conventional theoretical calculations of the
symmetry energy based on mean-field approaches fail to give the correct
low-temperature, low-density limit that is governed by correlations, in
particular by the appearance of bound states. A recently developed quantum
statistical (QS) approach that takes the formation of clusters into account
predicts symmetry energies that are in very good agreement with the
experimental data. A consistent description of the symmetry energy is given
that joins the correct low-density limit with quasiparticle approaches valid
near the saturation density.Comment: 4 pages, 2 figures, 1 tabl
Neutron and proton drip lines using the modified Bethe-Weizsacker mass formula
Proton and neutron separation energies have been calculated using the
extended Bethe-Weizsacker mass formula. This modified Bethe-Weizsacker mass
formula describes minutely the positions of all the old and the new magic
numbers. It accounts for the disappearance of some traditional magic numbers
for neutrons and provides extra stability for some new neutron numbers. The
neutron and proton drip lines have been predicted using this extended
Bethe-Weizsacker mass formula. The implications of the proton drip line on the
astrophysical rp-process and of the neutron drip line on the astrophysical
r-process have been discussed.Comment: 5 pages, 2 figure
Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
A new scheme for testing nuclear matter equations of state (EsoS) at high
densities using constraints from neutron star phenomenology and a flow data
analysis of heavy-ion collisions is suggested. An acceptable EoS shall not
allow the direct Urca process to occur in neutron stars with masses below
, and also shall not contradict flow and kaon production data of
heavy-ion collisions. Compact star constraints include the mass measurements of
2.1 +/- 0.2 M_sun (1 sigma level) for PSR J0751+1807, of 2.0 +/- 0.1 M_sun from
the innermost stable circular orbit for 4U 1636-536, the baryon mass -
gravitational mass relationships from Pulsar B in J0737-3039 and the
mass-radius relationships from quasiperiodic brightness oscillations in 4U
0614+09 and from the thermal emission of RX J1856-3754. This scheme is applied
to a set of relativistic EsoS constrained otherwise from nuclear matter
saturation properties with the result that no EoS can satisfy all constraints
simultaneously, but those with density-dependent masses and coupling constants
appear most promising.Comment: 15 pages, 8 figures, 5 table
From femtonova to supernova: Heavy-ion collisions and the supernova equation of state
AB Calculations using astrophysical equations of state at low densities comparable to that of the neutrino emission surface in supernovae and accretion disks are confronted with experimental results from heavy ion collisions. An extension of previous work shows that it is important to include all of the measured experimental data to draw conclusions about the astrophysical equation of state. Armed with this information, the calculations of the astrophysical equation of state are significantly constrained. Predictions of temperatures and densities sampled in black hole accretion disks are compared to those sampled in the experimental data
Relativistic quantum kinetic equation of the Vlasov type for systems with internal degrees of freedom
We present an approach to derive a relativistic kinetic equation of the
Vlasov type. Our approach is especially reliable for the description of quantum
field systems with many internal degrees of freedom. The method is based on the
Heisenberg picture and leads to a kinetic equation which fulfills the
conservation laws. We apply the approach to the standard Walecka Lagrangian and
an effective chiral Lagrangian.Comment: 11 pages, LaTeX, uses ijmpel.st
Staggering behavior of the low lying excited states of even-even nuclei in a Sp(4,R) classification scheme
We implement a high order discrete derivative analysis of the low lying
collective energies of even-even nuclei with respect to the total number of
valence nucleon pairs N in the framework of F- spin multiplets appearing in a
symplectic sp(4,R) classification scheme. We find that for the nuclei of any
given F- multiplet the respective experimental energies exhibit a Delta N=2
staggering behavior and for the nuclei of two united neighboring F- multiplets
well pronounced Delta N=1 staggering patterns are observed. Those effects have
been reproduced successfully through a generalized sp(4,R) model energy
expression and explained in terms of the step-like changes in collective modes
within the F- multiplets and the alternation of the F-spin projection in the
united neighboring multiplets. On this basis we suggest that the observed Delta
N=2 and Delta N=1 staggering effects carry detailed information about the
respective systematic manifestation of both high order alpha - particle like
quartetting of nucleons and proton (neutron) pairing interaction in nuclei.PACS
number(s):21.10.Re, 21.60.FwComment: 22 pages and 6 figures changes in the figure caption
Electrical conductivity of plasmas of DB white dwarf atmospheres
The static electrical conductivity of non-ideal, dense, partially ionized
helium plasma was calculated over a wide range of plasma parameters:
temperatures and mass density . Calculations of
electrical conductivity of plasma for the considered range of plasma parameters
are of interest for DB white dwarf atmospheres with effective temperatures
.
Electrical conductivity of plasma was calculated by using the modified random
phase approximation and semiclassical method, adapted for the case of dense,
partially ionized plasma. The results were compared with the unique existing
experimental data, including the results related to the region of dense
plasmas. In spite of low accuracy of the experimental data, the existing
agreement with them indicates that results obtained in this paper are correct
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