61 research outputs found
Thermonuclear explosion of rotating massive stars could explain core-collapse supernovae
It is widely thought that core-collapse supernovae (CCSNe), the explosions of
massive stars following the collapse of the stars' iron cores, is obtained due
to energy deposition by neutrinos. So far, this scenario was not demonstrated
from first principles. Kushnir and Katz (2014) have recently shown, by using
one-dimensional simulations, that if the neutrinos failed to explode the star,
a thermonuclear explosion of the outer shells is possible for some (tuned)
initial profiles. However, the energy released was small and negligible amounts
of ejected Ni were obtained, implying that these one-dimensional
collapse induced thermonuclear explosions (CITE) are unlikely to represent
typical CCSNe. Here I provide evidence supporting a scenario in which the
majority of CCSNe are the result of CITE. I use two-dimensional simulations to
show that collapse of stars that include slowly (few percent of breakup)
rotating shells of mixed helium-oxygen, leads to an
ignition of a thermonuclear detonation wave that unbinds the stars' outer
layers. Simulations of massive stars with different properties show that CITE
is a robust process, and results in explosions with kinetic energies in the
range of , and Ni yields of up to
, which are correlated, in agreement with observations for the
majority of CCSNe. Stronger explosions are predicted from higher mass
progenitors that leave more massive remnants, in contrast to the neutrino
mechanism. Neutron stars are produced in weak ()
explosions, while strong () explosions leave black
hole remnants.Comment: 4 pages, 5 figures, 3 table
The progenitors of core-collapse supernovae suggest thermonuclear origin for the explosions
Core-collapse supernovae (CCSNe) are the explosions of massive stars
following the collapse of the stars' iron cores. Poznanski (2013) has recently
suggested an observational correlation between the ejecta velocities and the
inferred masses of the red supergiant progenitors of type II-P explosions,
which implies that the kinetic energy of the ejecta ()
increases with the mass of the progenitor. I point out that the same conclusion
can be reached from the model-free observed correlation between the ejected
Ni masses () and the luminosities of the progenitors
for type II supernovae, which was reported by Fraser et al. (2011). This
correlation is in an agreement with the predictions of the collapse-induced
thermonuclear explosions (CITE) for CCSNe and in a possible contradiction with
the predictions of the neutrino mechanism. I show that a correlation between
and holds for all types of CCSNe
(including type Ibc). This correlation suggests a common mechanism for all
CCSNe, which is predicted for CITE, but is not produced by current simulations
of the neutrino mechanism. Furthermore, the typical values of
and for type Ibc explosions are larger by
an order of a magnitude than the typical values for II-P explosions, a fact
which disfavors progenitors with the same initial mass range for these
explosions. Instead, the progenitors of type Ibc explosions could be massive
Wolf-Rayet stars, which are predicted to yield strong explosions with low
ejecta masses (as observed) according to CITE. In this case, there is no
deficit of high mass progenitors for CCSNe, which was suggested under the
assumption of a similar mass range for the progenitors of types II-P and Ibc
supernovae.Comment: 4 pages, 3 figures, 2 table
Comments on "Numerical Stability of Detonations in White Dwarf Simulations"
Katz & Zingale (2019, KZ19) recently studied a one-dimensional test problem,
intended to mimic the process of detonation ignition in head-on collisions of
two carbon--oxygen (CO) white dwarfs. They do not obtain ignition of a
detonation in pure CO compositions unless the temperature is artificially
increased or 5% He is included. In both of these cases they obtain converged
ignition only for spatial resolutions better than 0.1 km, which are beyond the
capability of multidimensional simulations. This is in a contradiction with the
claims of Kushnir et al. (2013, K13), that a convergence to is
achieved for a resolution of a few km. Using Eulerian and Lagrangian codes we
show that a converged and resolved ignition is obtained for pure CO in this
test problem without the need for He or increasing the temperature. The two
codes agree to within 1% and convergence is obtained at resolutions of several
km. We calculate the case that includes He and obtain a similar slow
convergence, but find that it is due to a boundary numerical artifact that can
(and should) be avoided. Correcting the boundary conditions allows convergence
with resolution of in an agreement with the claims of
K13. It is likely that the slow convergence obtained by KZ19 in this case is
because of a similar boundary numerical artifact, but we are unable to verify
this. KZ19 further recommended to avoid the use of the burning limiter
introduced by K13. We show that their recommendation is not justified.Comment: 7 pages, 6 figures. Modified following referee repor
Hard X-ray emission from accretion shocks around galaxy clusters
We show that the hard X-ray (HXR) emission observed from several galaxy
clusters is naturally explained by a simple model, in which the nonthermal
emission is produced by inverse Compton scattering of cosmic microwave
background photons by electrons accelerated in cluster accretion shocks: The
dependence of HXR surface brightness on cluster temperature is consistent with
that predicted by the model, and the observed HXR luminosity is consistent with
the fraction of shock thermal energy deposited in relativistic electrons being
\lesssim 0.1. Alternative models, where the HXR emission is predicted to be
correlated with the cluster thermal emission, are disfavored by the data. The
implications of our predictions to future HXR observations (e.g. by NuStar,
Simbol-X) and to (space/ground based) gamma-ray observations (e.g. by Fermi,
HESS, MAGIC, VERITAS) are discussed.Comment: 7 pages, 3 figures, somewhat revised, published in JCA
Neutrino Signal of Collapse-Induced Thermonuclear Supernovae: The Case for Prompt Black Hole Formation in SN1987A
Collapse-induced thermonuclear explosion (CITE) may explain core-collapse
supernovae (CCSNe). We present a preliminary analysis of the neutrino signal
predicted by CITE and compare it to the neutrino burst of SN1987A. For strong
CCSNe, as SN1987A, CITE predicts a proto-neutron star (PNS) accretion phase,
accompanied by the corresponding neutrino luminosity, that can last a few
seconds and that is cut-off abruptly by black hole (BH) formation. The neutrino
luminosity can later be revived by accretion disc emission after a dead time of
few to a few ten seconds. In contrast, the neutrino mechanism for CCSNe
predicts a shorter PNS accretion phase, followed by a slowly declining PNS
cooling luminosity. We repeat statistical analyses used in the literature to
interpret the neutrino mechanism, and apply them to CITE. The first 1-2 sec of
the neutrino burst are equally compatible with CITE and with the neutrino
mechanism. However, the data hints to a luminosity drop at t=2-3 sec, in some
tension with the neutrino mechanism while being naturally attributed to BH
formation in CITE. The occurrence of neutrino events at 5 sec in SN1987A
suggests that the accretion disc formed by that time. We perform 2D numerical
simulations, showing that CITE may be able to accommodate this disc formation
time while reproducing the ejected Ni mass and ejecta kinetic energy
within factors 2-3 of observations. We estimate the disc neutrino luminosity
and show that it can roughly match the data. This suggests that direct BH
formation is compatible with the neutrino burst of SN1987A. With current
neutrino detectors, the neutrino burst of the next Galactic CCSN may give us
front-row seats to the formation of an event horizon in real time. Access to
phenomena near the event horizon motivates the construction of a few Megaton
neutrino detector that should observe extragalactic CCSNe on a yearly basis.Comment: 11 pages, 6 figure
Towards an accurate description of an accretion induced collapse and the associated ejected mass
We revisit the accretion-induced collapse (AIC) process, in which a white
dwarf collapses into a neutron star. We are motivated by the persistent radio
source associated with the fast radio burst FRB 121102, which was explained by
Waxman as a weak stellar explosion with a small ()
mildly relativistic mass ejection that may be consistent with AIC.
Additionally, the interaction of the relatively low ejected mass with a
pre-collapse wind might be related to fast optical transients. The AIC is
simulated with a one-dimensional, Lagrangian, Newtonian hydrodynamic code. We
put an emphasis on accurately treating the equation of state and the nuclear
burning, which is required for any study that attempts to accurately simulate
AIC. We leave subjects such as neutrino physics and general relativity
corrections for future work. Using an existing initial profile and our own
initial profiles, we find that the ejected mass is to
over a wide range of parameters, and we construct a simple
model to explain our results.Comment: Accepted for publication in ApJ, 15 pages, 9 figure
Nonthermal emission from clusters of galaxies
We show that the spectral and radial distribution of the nonthermal emission
of massive, M>10^{14.5}M_sun, galaxy clusters (GCs) may be approximately
described by simple analytic expressions, which depend on the GC thermal X-ray
properties and on two model parameter, beta_{core} and eta_e. beta_{core} is
the ratio of CR energy density (within a logarithmic CR energy interval) and
the thermal energy density at the GC core, and eta_{e(p)} is the fraction of
the thermal energy generated in strong collisionless shocks, which is deposited
in CR electrons (protons). Using a simple analytic model for the evolution of
ICM CRs, which are produced by accretion shocks (primary CRs), we find that
beta_{core} ~ eta_{p}/200, nearly independent of GC mass and with a scatter
Delta ln(beta_{core}) ~ 1 between GCs of given mass. We show that the HXR and
gamma-ray luminosities produced by IC scattering of CMB photons by primary
electrons exceed the luminosities produced by secondary particles (generated in
hadronic interactions within the GC) by factors ~500(eta_e/eta_p)(T/10
keV)^{-1/2} and ~150(eta_e/eta_p)(T/10 keV)^{-1/2} respectively, where T is the
GC temperature. Secondary particle emission may dominate at the radio and VHE
(> 1 TeV) gamma-ray bands. Our model predicts, in contrast with some earlier
work, that the HXR and gamma-ray emission from GCs are extended, since the
emission is dominated at these energies by primary electrons. Our predictions
are consistent with the observed nonthermal emission of the Coma cluster for
eta_peta_e ~ 0.1. The implications of our predictions to future HXR
observations (e.g. by NuStar, Simbol-X) and to (space/ground based) gamma-ray
observations (e.g. by Fermi, HESS, MAGIC, VERITAS) are discussed. Finally, we
show that our model's results agree with results of detailed numerical
calculations.Comment: 22 pages, 16 figures, somewhat revised, published in JCA
Can helium envelopes change the outcome of direct white dwarf collisions?
Collisions of white dwarfs (WDs) have recently been invoked as a possible
mechanism for type Ia supernovae (SNIa). A pivotal feature for the viability of
WD collisions as SNIa progenitors is that a significant fraction of the mass is
highly compressed to the densities required for efficient Ni production
before the ignition of the detonation wave. Previous studies have predominantly
employed model WDs composed entirely of carbon-oxygen (CO), whereas WDs are
expected to have a non-negligible helium envelope. Given that helium is more
susceptible to explosive burning than CO under the conditions characteristic of
WD collision, a legitimate concern is whether or not early time He detonation
ignition can translate to early time CO detonation, thereby drastically
reducing Ni synthesis. We investigate the role of He in determining the
fate of WD collisions by performing a series of two-dimensional hydrodynamics
calculations. We find that a necessary condition for non-trivial reduction of
the CO ignition time is that the He detonation birthed in the contact region
successfully propagates into the unshocked shell. We determine the minimal He
shell mass as a function of the total WD mass that upholds this condition.
Although we utilize a simplified reaction network similar to those used in
previous studies, our findings are in good agreement with detailed
investigations concerning the impact of network size on He shell detonations.
This allows us to extend our results to the case with more realistic burning
physics. Based on the comparison of these findings against evolutionary
calculations of WD compositions, we conclude that most, if not all, WD
collisions will not be drastically impacted by their intrinsic He components.Comment: 5 Pages, 2 Figure, 3 Table
The structure of detonation waves in supernovae revisited
The structure of a thermonuclear detonation wave can be solved accurately
and, thus, may serve as a test bed for studying different approximations that
are included in multidimensional hydrodynamical simulations of supernova. We
present the structure of thermonuclear detonations for the equal mass fraction
of C and O (CO) and for pure He (He) over a wide range of
upstream plasma conditions. The lists of isotopes we constructed allow us to
determine the detonation speeds, as well as the final states for these
detonations, with an uncertainty of the percent level (obtained here for the
first time). We provide our results with a numerical accuracy of ,
which provides an efficient benchmark for future studies. We further show that
CO detonations are pathological for all upstream density values, which differs
from previous studies, which concluded that for low upstream densities CO
detonations are of the Chapman-Jouget (CJ) type. We provide an approximate
condition, independent of reaction rates, that allows to estimate whether
arbitrary upstream values will support a detonation wave of the CJ type. Using
this argument, we are able to show that CO detonations are pathological and to
verify that He detonations are of the CJ type, as was previously claimed for
He. Our analysis of the reactions that control the approach to nuclear
statistical equilibrium, which determines the length-scale of this stage,
reveals that at high densities, the reactions
BHe plays a significant role, which was
previously unknown.Comment: 33 pages, 27 figures, 14 tables. Revised following a referee repor
An exact integral relation between the Ni56 mass and the bolometric light curve of a type Ia supernova
An exact relation between the Ni56 mass and the bolometric light curve of a
type Ia supernova can be derived as follows, using the following excellent
approximations: 1. the emission is powered solely by Ni56-> Co56 ->Fe56; 2.
each mass element propagates at a non-relativistic velocity which is constant
in time (free coasting); and 3. the internal energy is dominated by radiation.
Under these approximations, the energy E(t) carried by radiation in the ejecta
satisfies: dE/dt=-E(t)/t-L(t)+Q(t), where Q(t) is the deposition of energy by
the decay which is precisely known and L(t) is the bolometric luminosity. By
multiplying this equation by time and integrating over time we find:
E(t)*t=\int_0^t Q(t')t'dt' -\int_0^t L(t')t'dt'. At late time, t>> t_peak, the
energy inside the ejecta decreases rapidly due to its escape, and thus we have
\int_0^t Q(t')t'dt'=\int_0^t L(t')t'dt'. This relation is correct regardless of
the opacities, density distribution or Ni56 deposition distribution in the
ejecta and is very different from "Arnett's rule", L_peak ~ Q(t_peak). By
comparing \int_0^t Q(t')t'dt' with \int_0^t L(t')t'dt' at t~40 day after the
explosion, the mass of Ni56 can be found directly from UV, optical and infrared
observations with modest corrections due to the unobserved gamma-rays and due
to the small residual energy in the ejecta, E(t)*t>0.Comment: 1 paragrap
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