1,048 research outputs found
The r-Process in Black Hole Winds
All the current r-process scenarios relevant to core-collapse supernovae are
facing severe difficulties. In particular, recent core-collapse simulations
with neutrino transport show no sign of a neutron-rich wind from the
proto-neutron star. In this paper, we discuss nucleosynthesis of the r-process
in an alternative astrophysical site, "black hole winds", which are the
neutrino-driven outflow from the accretion torus around a black hole. This
condition is assumed to be realized in double neutron star mergers, neutron
star - black hole mergers, or hypernovae.Comment: 6 pages, 4 figures, invited talk at OMEG10, March 2010, to be
published in the proceedings of OMEG10 (AIP
Exploring properties of high-density matter through remnants of neutron-star mergers
Remnants of neutron-star mergers are essentially massive, hot, differentially
rotating neutron stars, which are initially strongly oscillating. They
represent a unique probe for high-density matter because the oscillations are
detectable via gravitational-wave measurements and are strongly dependent on
the equation of state. The impact of the equation of state is apparent in the
frequency of the dominant oscillation mode of the remnant. For a fixed total
binary mass a tight relation between the dominant postmerger frequency and the
radii of nonrotating neutron stars exists. Inferring observationally the
dominant postmerger frequency thus determines neutron star radii with high
accuracy of the order of a few hundred meters. By considering symmetric and
asymmetric binaries of the same chirp mass, we show that the knowledge of the
binary mass ratio is not critical for this kind of radius measurements. We
summarize different possibilities to deduce the maximum mass of nonrotating
neutron stars. We clarify the nature of the three most prominent features of
the postmerger gravitational-wave spectrum and argue that the merger remnant
can be considered to be a single, isolated, self-gravitating object that can be
described by concepts of asteroseismology. The understanding of the different
mechanisms shaping the gravitational-wave signal yields a physically motivated
analytic model of the gravitational-wave emission, which may form the basis for
template-based gravitational-wave data analysis. We explore the observational
consequences of a scenario of two families of compact stars including hadronic
and quark stars. We find that this scenario leaves a distinctive imprint on the
postmerger gravitational-wave signal. In particular, a strong discontinuity in
the dominant postmerger frequency as function of the total mass will be a
strong indication for two families of compact stars. (abridged)Comment: 22 pages, 17 figures; accepted for publication in EPJ
Neutrino transport in type II supernovae: Boltzmann solver vs. Monte Carlo method
We have coded a Boltzmann solver based on a finite difference scheme (S_N
method) aiming at calculations of neutrino transport in type II supernovae.
Close comparison between the Boltzmann solver and a Monte Carlo transport code
has been made for realistic atmospheres of post bounce core models under the
assumption of a static background. We have also investigated in detail the
dependence of the results on the numbers of radial, angular, and energy grid
points and the way to discretize the spatial advection term which is used in
the Boltzmann solver. A general relativistic calculation has been done for one
of the models. We find overall good agreement between the two methods. However,
because of a relatively small number of angular grid points (which is
inevitable due to limitations of the computation time) the Boltzmann solver
tends to underestimate the flux factor and the Eddington factor outside the
(mean) ``neutrinosphere'' where the angular distribution of the neutrinos
becomes highly anisotropic. This fact suggests that one has to be cautious in
applying the Boltzmann solver to a calculation of the neutrino heating in the
hot-bubble region because it might tend to overestimate the local energy
deposition rate. A comparison shows that this trend is opposite to the results
obtained with a multi-group flux-limited diffusion approximation of neutrino
transport. The accuracy of the Boltzmann solver can be considerably improved by
using a variable angular mesh to increase the angular resolution in the
semi-transparent regime.Comment: 19 pages, 17 figures, submitted to A&
Electron-capture supernovae as sources of 60Fe
We investigate the nucleosynthesis of the radionuclide 60Fe in
electron-capture supernovae (ECSNe). The nucleosynthetic results are based on a
self-consistent, two-dimensional simulation of an ECSN as well as models in
which the densities are systematically increased by some factors (low-entropy
models). 60Fe is found to be appreciably made in neutron-rich ejecta during the
nuclear quasi-equilibrium phase with greater amounts being produced in the
lower-entropy models. Our results, combining them with the yields of
core-collapse supernovae (CCSNe) in the literature, suggest that ECSNe account
for at least 4-30% of live 60Fe in the Milky Way. ECSNe co-produce neutron-rich
isotopes, 48Ca, 50Ti, 54Cr, some light trans-iron elements, and possibly weak
r-process elements including some radionuclides such as 93Zr, 99Tc, and 107Pd,
whose association with 60Fe might have been imprinted in primitive meteorites
or in the deep ocean crust on the Earth.Comment: 6 pages, 2 figures, accepted for publication in ApJ
Neutrino-driven supernova of a low-mass iron-core progenitor boosted by three-dimensional turbulent convection
We present the first successful simulation of a neutrino-driven supernova
explosion in three dimensions (3D), using the Prometheus-Vertex code with an
axis-free Yin-Yang grid and a sophisticated treatment of three-flavor,
energy-dependent neutrino transport. The progenitor is a nonrotating,
zero-metallicity 9.6 Msun star with an iron core. While in spherical symmetry
outward shock acceleration sets in later than 300 ms after bounce, a successful
explosion starts at ~130 ms postbounce in two dimensions (2D). The 3D model
explodes at about the same time but with faster shock expansion than in 2D and
a more quickly increasing and roughly 10 percent higher explosion energy of
>10^50 erg. The more favorable explosion conditions in 3D are explained by
lower temperatures and thus reduced neutrino emission in the cooling layer
below the gain radius. This moves the gain radius inward and leads to a bigger
mass in the gain layer, whose larger recombination energy boosts the explosion
energy in 3D. These differences are caused by less coherent, less massive, and
less rapid convective downdrafts associated with postshock convection in 3D.
The less violent impact of these accretion downflows in the cooling layer
produces less shock heating and therefore diminishes energy losses by neutrino
emission. We thus have, for the first time, identified a reduced mass accretion
rate, lower infall velocities, and a smaller surface filling factor of
convective downdrafts as consequences of 3D postshock turbulence that
facilitate neutrino-driven explosions and strengthen them compared to the 2D
case.Comment: 7 pages, 5 figures; revised version with more discussion of
resolution dependence and differences to other 3D results; accepted by ApJ
Electron-capture supernovae as origin of 48Ca
We report that electron-capture supernovae (ECSNe), arising from collapsing
oxygen-neon-magnesium cores, are a possible source of 48Ca, whose origin has
remained a long-standing puzzle. Our two-dimensional, self-consistent explosion
model of an ECSN predicts ejection of neutron-rich matter with electron
fractions Ye = 0.40-0.42 and relatively low entropies, s = 13-15 kB per nucleon
(kB is the Boltzmann constant). Post-processing nucleosynthesis calculations
result in appreciable production of 48Ca in such neutron-rich and low-entropy
matter during the quasi-nuclear equilibrium and subsequent freezeout phases.
The amount of ejected 48Ca can account for that in the solar inventory when we
consider possible uncertainties in the entropies or ejecta-mass distribution.
ECSNe could thus be a site of 48Ca production in addition to a hypothetical,
rare class of high-density Type Ia supernovae.Comment: 6 pages, 5 figures, accepted for publication in ApJ
Impact of Nucleon-Nucleon Bremsstrahlung Rates Beyond One-Pion Exchange
Neutrino-pair production and annihilation through nucleon-nucleon
bremsstrahlung is included in current supernova simulations by rates that are
based on the one-pion-exchange approximation. Here we explore the consequences
of bremsstrahlung rates based on a modern nuclear interactions for
proto-neutron star cooling and the corresponding neutrino emission. We find
that despite a reduction of the bremsstrahlung emission by a factor of 2-5 in
the neutrinospheric region, models with the improved treatment exhibit only
5% changes of the neutrino luminosities and an increase of
0.7 MeV of the average energies of the radiated neutrino spectra,
with the largest effects for the antineutrinos of all flavors and at late
times. Overall, the proto-neutron star cooling evolution is slowed down
modestly by 0.5-1 s.Comment: 11 pages, 7 figures, minor changes and additions, to appear in Phys.
Rev.
Supernova deleptonization asymmetry: Impact on self-induced flavor conversion
During the accretion phase of a core-collapse supernova (SN), the
deleptonization flux has recently been found to develop a global dipole pattern
(LESA---Lepton Emission Self-sustained Asymmetry). The minus
flux essentially vanishes in one direction, potentially
facilitating self-induced flavor conversion. On the other hand, below the
stalled shock wave, self-induced flavor conversion is typically suppressed by
multi-angle matter effects, preventing any impact of flavor conversion on SN
explosion dynamics. In a schematic model of SN neutrino fluxes, we study the
impact of modified - flux asymmetries on collective flavor
conversion. In the parameter space consisting of matter density and effective
neutrino density, the region of instability with regard to self-induced flavor
conversion is much larger for a vanishing lepton number flux, yet this
modification does not intersect a realistic SN profile. Therefore, it appears
that, even in the presence of LESA, self-induced flavor conversion remains
suppressed below the shock front.Comment: 14 pages, 6 figures; v2: significant change in presentation, results
and conclusion unchanged, appendix adde
Identifying rotation in SASI-dominated core-collapse supernovae with a neutrino gyroscope
Measuring the rotation of core-collapse supernovae (SN) and of their
progenitor stars is extremely challenging. Here it is demonstrated that
neutrinos may potentially be employed as stellar gyroscopes, if phases of
activity by the standing accretion-shock instability (SASI) affect the neutrino
emission prior to the onset of the SN explosion. This is shown by comparing the
neutrino emission properties of self-consistent, three-dimensional (3D) SN
simulations of a 15 M_sun progenitor without rotation as well as slow and fast
rotation compatible with observational constraints. The explosion of the fast
rotating model gives rise to long-lasting, massive polar accretion downflows
with stochastic time-variability, detectable e.g. by the IceCube Neutrino
Observatory for any observer direction. While spectrograms of the neutrino
event rate of non-rotating SNe feature a well-known sharp peak due to SASI for
observers located in the proximity of the SASI plane, the corresponding
spectrograms of rotating models show activity over a wide range of frequencies,
most notably above 200 Hz for rapid rotation. In addition, the Fourier power
spectra of the event rate for rotating models exhibit a SASI peak with lower
power than in non-rotating models. The spectra for the rotating models also
show secondary peaks at higher frequencies with greater relative heights
compared to the main SASI peak than for non-rotating cases. These rotational
imprints will be detectable for SNe at 10 kpc or closer.Comment: 10 pages, including 6 figures. Minor changes in the text, matches
version accepted for publication in Phys. Rev. D. Animated visualizations
available at: https://wwwmpa.mpa-garching.mpg.de/ccsnarchive/data/Walk2018
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