1,312 research outputs found
Natal Kicks of Stellar-Mass Black Holes by Asymmetric Mass Ejection in Fallback Supernovae
Integrating trajectories of low-mass X-ray binaries containing black holes
within the Galactic potential, Repetto, Davies & Sigurdsson recently showed
that the large distances of some systems above the Galactic plane can only be
explained if black holes receive appreciable natal kicks. Surprisingly, they
found that the distribution of black hole kick velocities (rather than that of
the momenta) should be similar to that of neutron stars. Here I argue that this
result can be understood if neutron star and black hole kicks are a consequence
of large-scale asymmetries created in the supernova ejecta by the explosion
mechanism. The corresponding anisotropic gravitational attraction of the
asymmetrically expelled matter does not only accelerate new-born neutron stars
by the "gravitational tug-boat mechanism". It can also lead to delayed
black-hole formation by asymmetric fallback of the slowest parts of the initial
ejecta onto the transiently existing neutron star, in course of which the
momentum of the black hole can grow with the fallback mass. Black hole kick
velocities will therefore not be reduced by the ratio of neutron star to black
hole mass as would be expected for kicks caused by anisotropic neutrino
emission of the nascent neutron star.Comment: 7 pages, 1 figure (3 eps files); submitted to MNRA
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
Spatial distribution of radionuclides in 3D models of SN 1987A and Cas A
Fostered by the possibilities of multi-dimensional computational modeling, in
particular the advent of three-dimensional (3D) simulations, our understanding
of the neutrino-driven explosion mechanism of core-collapse supernovae (SNe)
has experienced remarkable progress over the past decade. First
self-consistent, first-principle models have shown successful explosions in 3D,
and even failed cases may be cured by moderate changes of the microphysics
inside the neutron star (NS), better grid resolution, or more detailed
progenitor conditions at the onset of core collapse, in particular large-scale
perturbations in the convective Si and O burning shells. 3D simulations have
also achieved to follow neutrino-driven explosions continuously from the
initiation of the blast wave, through the shock breakout from the progenitor
surface, into the radioactively powered evolution of the SN, and towards the
free expansion phase of the emerging remnant. Here we present results from such
simulations, which form the basis for direct comparisons with observations of
SNe and SN remnants in order to derive constraints on the still disputed
explosion mechanism. It is shown that predictions based on hydrodynamic
instabilities and mixing processes associated with neutrino-driven explosions
yield good agreement with measured NS kicks, light-curve properties of SN
1987A, and asymmetries of iron and 44Ti distributions observed in SN 1987A and
Cassiopeia A.Comment: 9 pages, 6 figures; submitted to: "SN 1987A, 30 years later",
Proceedings IAU Symposium No. 331, 2017; eds. M. Renaud et a
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
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
Three-Dimensional Simulations of Core-Collapse Supernovae: From Shock Revival to Shock Breakout
We present 3D simulations of core-collapse supernovae from blast-wave
initiation by the neutrino-driven mechanism to shock breakout from the stellar
surface, considering two 15 Msun red supergiants (RSG) and two blue supergiants
(BSG) of 15 Msun and 20 Msun. We demonstrate that the metal-rich ejecta in
homologous expansion still carry fingerprints of asymmetries at the beginning
of the explosion, but the final metal distribution is massively affected by the
detailed progenitor structure. The most extended and fastest metal fingers and
clumps are correlated with the biggest and fastest-rising plumes of
neutrino-heated matter, because these plumes most effectively seed the growth
of Rayleigh-Taylor (RT) instabilities at the C+O/He and He/H composition-shell
interfaces after the passage of the SN shock. The extent of radial mixing,
global asymmetry of the metal-rich ejecta, RT-induced fragmentation of initial
plumes to smaller-scale fingers, and maximal Ni and minimal H velocities do not
only depend on the initial asphericity and explosion energy (which determine
the shock and initial Ni velocities) but also on the density profiles and
widths of C+O core and He shell and on the density gradient at the He/H
transition, which lead to unsteady shock propagation and the formation of
reverse shocks. Both RSG explosions retain a great global metal asymmetry with
pronounced clumpiness and substructure, deep penetration of Ni fingers into the
H-envelope (with maximum velocities of 4000-5000 km/s for an explosion energy
around 1.5 bethe) and efficient inward H-mixing. While the 15 Msun BSG shares
these properties (maximum Ni speeds up to ~3500 km/s), the 20 Msun BSG develops
a much more roundish geometry without pronounced metal fingers (maximum Ni
velocities only ~2200 km/s) because of reverse-shock deceleration and
insufficient time for strong RT growth and fragmentation at the He/H interface.Comment: 21 pages, 15 figures; revised version with minor changes in Sect.1;
accepted by Astron. Astrophy
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&
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
Resolution Study for Three-dimensional Supernova Simulations with the Prometheus-Vertex Code
We present a carefully designed, systematic study of the angular resolution
dependence of simulations with the Prometheus-Vertex neutrino-hydrodynamics
code. Employing a simplified neutrino heating-cooling scheme in the Prometheus
hydrodynamics module allows us to sample the angular resolution between 4
degrees and 0.5 degrees. With a newly-implemented static mesh refinement (SMR)
technique on the Yin-Yang grid, the angular coordinates can be refined in
concentric shells, compensating for the diverging structure of the spherical
grid. In contrast to previous studies with Prometheus and other codes, we find
that higher angular resolution and therefore lower numerical viscosity provides
more favorable explosion conditions and faster shock expansion. We discuss the
possible reasons for the discrepant results. The overall dynamics seem to
converge at a resolution of about 1 degree. Applying the SMR setup to
marginally exploding progenitors is disadvantageous for the shock expansion,
however, because kinetic energy of downflows is dissipated to internal energy
at resolution interfaces, leading to a loss of turbulent pressure support and a
steeper temperature gradient. We also present a way to estimate the numerical
viscosity on grounds of the measured turbulent kinetic-energy spectrum, leading
to smaller values that are better compatible with the flow behavior witnessed
in our simulations than results following calculations in previous literature.
Interestingly, the numerical Reynolds numbers in the turbulent, neutrino-heated
postshock layer (some 10 to several 100) are in the ballpark of expected
neutrino-drag effects on the relevant length scales in the turbulent postshock
layer. We provide a formal derivation and quantitative assessment of the
neutrino drag terms in an appendix.Comment: 37 pages, 14 figures, 4 tables; revised version with neutrino drag
discussion extended for numerical evaluation; accepted by Ap
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
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