94 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
Physical conditions for the r-process I. radioactive energy sources of kilonovae
Radioactive energies from unstable nuclei made in the ejecta of neutron star
mergers play principal roles in powering kilonovae. In previous studies
power-law-type heating rates (e.g., ~ t^-1.3) have frequently been used, which
may be inadequate if the ejecta are dominated by nuclei other than the A ~ 130
region. We consider, therefore, two reference abundance distributions that
match the r-process residuals to the solar abundances for A >= 69 (light
trans-iron plus r-process elements) and A >= 90 (r-process elements).
Nucleosynthetic abundances are obtained by using free-expansion models with
three parameters: expansion velocity, entropy, and electron fraction.
Radioactive energies are calculated as an ensemble of weighted free-expansion
models that reproduce the reference abundance patterns. The results are
compared with the bolometric luminosity (> a few days since merger) of the
kilonova associated with GW170817. We find that the former case (fitted for A
>= 69) with an ejecta mass 0.06 M_sun reproduces the light curve remarkably
well including its steepening at > 7 days, in which the mass of r-process
elements is ~ 0.01 M_sun. Two beta-decay chains are identified: 66Ni -> 66Cu ->
66Zn and 72Zn -> 72Ga -> 72Ge with similar halflives of parent isotopes (~ 2
days), which leads to an exponential-like evolution of heating rates during
1-15 days. The light curve at late times (> 40 days) is consistent with
additional contributions from the spontaneous fission of 254Cf and a few Fm
isotopes. If this is the case, the event GW170817 is best explained by the
production of both light trans-iron and r-process elements that originate from
dynamical ejecta and subsequent disk outflows from the neutron star merger.Comment: 15 pages, 5 figures, accepted for publication in Ap
Cold r-Process in Neutrino-Driven Winds
The r-process in a low temperature environment is explored, in which the
neutron emission by photodisintegration does not play a role (cold r-process).
A semi-analytic neutrino-driven wind model is utilized for this purpose. The
temperature in a supersonically expanding outflow can quickly drop to a few
10^8 K, where the (n, gamma)-(gamma, n) equilibrium is never achieved during
the heavy r-nuclei synthesis. In addition, the neutron capture competes with
the beta-decay owing to the low matter density. Despite such non-standard
physical conditions for the cold r-process, a solar-like r-process abundance
curve can be reproduced. The cold r-process predicts, however, the low lead
production compared to that expected in the traditional r-process conditions,
which can be a possible explanation for the low lead abundances found in a
couple of r-process-rich Galactic halo stars.Comment: 5 pages, 3 figures, accepted for publication in ApJ
Neutron Star Mergers as the Origin of r-Process Elements in the Galactic Halo Based on the Sub-halo Clustering Scenario
Binary mergers (NSMs) of double neutron star (and black hole-neutron star)
systems are suggested to be major sites of r-process elements in the Galaxy by
recent hydrodynamical and nucleosynthesis studies. It has been pointed out,
however, that the estimated long lifetimes of neutron star binaries are in
conflict with the presence of r-process-enhanced halo stars at metallicities as
low as [Fe/H] ~ -3. To resolve this problem, we examine the role of NSMs in the
early Galactic chemical evolution on the assumption that the Galactic halo was
formed from merging sub-halos. We present simple models for the chemical
evolution of sub-halos with total final stellar masses between 10^4 M_solar and
2 x 10^8 M_solar. Typical lifetimes of compact binaries are assumed to be 100
Myr (for 95% of their population) and 1 Myr (for 5%), according to recent
binary population synthesis studies. The resulting metallcities of sub-halos
and their ensemble are consistent with the observed mass-metallicity relation
of dwarf galaxies in the Local Group, and the metallicity distribution of the
Galactic halo, respectively. We find that the r-process abundance ratios [r/Fe]
start increasing at [Fe/H] <= -3 if the star formation efficiencies are smaller
for less massive sub-halos. In addition, the sub-solar [r/Fe] values (observed
as [Ba/Fe] ~ -1.5 for [Fe/H] < -3) are explained by the contribution from the
short-lived (~1 Myr) binaries. Our results indicate that NSMs may have a
substantial contribution to the r-process element abundances throughout the
Galactic history.Comment: 5 pages, 2 figures, accepted for publication in ApJ
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
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
The rp-Process in Neutrino-driven Winds
Recent hydrodynamic simulations of core-collapse supernovae with accurate
neutrino transport suggest that the bulk of the early neutrino-heated ejecta is
proton rich, in which the production of some interesting proton-rich nuclei is
expected. As suggested in recent nucleosynthesis studies, the rapid
proton-capture (rp) process takes place in such proton-rich environments by
bypassing the waiting point nuclei with the beta-lives of a few minutes via the
faster capture of neutrons continuously supplied from the neutrino absorption
by protons. In this study, the nucleosynthesis calculations are performed with
the wide ranges of the neutrino luminosities and the electron fractions (Ye),
using the semi-analytic models of proto-neutron star winds. The masses of
proto-neutron stars are taken to be 1.4 Msolar and 2.0 Msolar, where the latter
is regarded as the test for somewhat high entropy winds (about a factor of
two). For Ye > 0.52, the neutrino-induced rp-process takes place in many wind
trajectories, and the p-nuclei up to A ~ 130 are synthesized with interesting
amounts. However, 92Mo is somewhat underproduced compared to those with similar
mass numbers. For 0.46 < Ye < 0.49, on the other hand, 92Mo is significantly
enhanced by the nuclear flows in the vicinity of the abundant 90Zr that
originates from the alpha-process at higher temperature. The nucleosynthetic
yields are averaged over the ejected masses of winds, and further the Ye
distribution predicted by the recent hydrodynamic simulation of a core-collapse
supernova. Comparison of the mass-Ye-averaged yields to the solar compositions
implies that the neutrino-driven winds can be potentially the origin of light
p-nuclei up to A ~ 110, including 92,94Mo and 96,98Ru that cannot be explained
by other astrophysical sites.Comment: 29 pages, 18 figures, accepted for publication in Ap
The r-Process in the Proto-Neutron-Star Winds with Anisotropic Neutrino Emission
The astrophysical origin of the r-process nuclei is still unknown. Even the
most promising scenario, the neutrino-driven winds from a nascent neutron star,
encounters severe difficulties in obtaining requisite entropy and short dynamic
timescale for the r-process. In this study, the effect of anisotropy in
neutrino emission from a proto-neutron star surface is examined with
semi-analytic neutrino-driven wind models. The increase of neutrino number
density in the wind owing to the anisotropy is modeled schematically by
enhancing the effective neutrino luminosity. It is shown that the neutrino
heating rate from neutrino-antineutrino pair annihilation into
electron-positron pairs can significantly increase owing to the anisotropy and
play a dominant role for the heating of wind material. A factor of five
increase in the effective neutrino luminosity results in 50% higher entropy and
a factor of ten shorter dynamic timescale owing to this enhanced neutrino
heating. The nucleosynthesis calculations show that this change is enough for
the robust r-process, producing the third abundance peak A = 195 and beyond.
Future multi-dimensional studies with accurate neutrino transport will be
needed if such anisotropy relevant for the current scenario (more than a factor
of a few) is realized during the wind phase (~1-10 s).Comment: 8 pages, 3 figures, accepted for publication in ApJ Letter
Uncertainties in the nu p-process: supernova dynamics versus nuclear physics
We examine how the uncertainties involved in supernova dynamics as well as in
nuclear data inputs affect the nup-process in the neutrino-driven winds. For
the supernova dynamics, we find that the wind termination by the preceding
dense ejecta shell, as well as the electron fraction (Y_{e, 3}; at 3 10^9 K)
play a crucial role. A wind termination within the temperature range of (1.5-3)
10^9 K greatly enhances the efficiency of the nu p-process. This implies that
the early wind phase, when the innermost layer of the preceding supernova
ejecta is still 200-1000 km from the center, is most relevant to the
nup-process. The outflows with Y_{e, 3} = 0.52-0.60 result in the production of
the p-nuclei up to A=108 with interesting amounts. Furthermore, the p-nuclei up
to A=152 can be produced if Y_{e, 3} = 0.65 is achieved. For the nuclear data
inputs, we test the sensitivity to the rates relevant to the breakout from the
pp-chain region (A < 12), to the (n, p) rates on heavy nuclei, and to the
nuclear masses along the nup-process pathway. We find that a small variation of
the rates of triple-alpha and of the (n, p) reaction on 56Ni leads to a
substantial change in the p-nuclei production. We also find that 96Pd (N=50) on
the nup-process path plays a role as a second seed nucleus for the production
of heavier p-nuclei. The uncertainty in the nuclear mass of 82Zr can lead to a
factor of two reduction in the abundance of the p-isotope 84Sr.Comment: 20 pages, 22 figures, accepted for publication in Ap
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