2,137 research outputs found
Neutrino Capture and r-Process Nucleosynthesis
We explore neutrino capture during r-process nucleosynthesis in
neutrino-driven ejecta from nascent neutron stars. We focus on the interplay
between charged-current weak interactions and element synthesis, and we
delineate the important role of equilibrium nuclear dynamics. During the period
of coexistence of free nucleons and light and/or heavy nuclei, electron
neutrino capture inhibits the r-process. At all stages, capture on free
neutrons has a larger impact than capture on nuclei. However, neutrino capture
on heavey nuclei by itself, if it is very strong, is also detrimental to the
r-process until large nuclear equilibrium clusters break down and the classical
neutron-capture phase of the r-process begins. The sensitivity of the r-process
to neutrino irradiation means that neutrino-capture effects can strongly
constrain the r-process site, neutrino physics, or both. These results apply
also to r-process scenarios other than neutrino-heated winds.Comment: 20 pages, 17 figures, Submitted to Physical Review
General relativistic effects on neutrino-driven wind from young, hot neutron star and the r-process nucleosynthesis
Neutrino-driven wind from young hot neutron star, which is formed by
supernova explosion, is the most promising candidate site for r-process
nucleosynthesis. We study general relativistic effects on this wind in
Schwarzschild geometry in order to look for suitable conditions for a
successful r-process nucleosynthesis. It is quantitatively discussed that the
general relativistic effects play a significant role in increasing entropy and
decreasing dynamic time scale of the neutrino-driven wind. Exploring wide
parameter region which determines the expansion dynamics of the wind, we find
interesting physical conditions which lead to successful r-process
nucleosynthesis. The conditions which we found realize in the neutrino-driven
wind with very short dynamic time scale ms and
relatively low entropy . We carry out the -process and
r-process nucleosynthesis calculation on these conditions by the use of our
single network code including over 3000 isotopes, and confirm quantitatively
that the second and third r-process abundance peaks are produced in the
neutrino-driven wind.Comment: Accepted for publication in Ap
Neutrino-Induced Fission and r-Process Nucleosynthesis
An r-process scenario with fission but no fission cycling is considered to
account for the observed abundance patterns of neutron-capture elements in
ultra-metal-poor stars. It is proposed that neutrino reactions play a crucial
role in inducing the fission of the progenitor nuclei after the r-process
freezes out in Type II Supernovae. To facilitate neutrino-induced fission, the
proposed r-process scenario is restricted to occur in a low-density environment
such as the neutrino-driven wind from the neutron star. Further studies to
develop this scenario are emphasized.Comment: 11 pages, 2 figures, to appear in ApJ
Neutrinos, Weak Interactions, and r-process Nucleosynthesis
Two of the key issues in understanding the neutron-to-proton ratio in a
core-collapse supernova are discussed. One of these is the behavior of the
neutrino-nucleon cross sections as supernova energies. The other issue is the
many-body properties of the neutrino gas near the core when both one- and
two-body interaction terms are included.Comment: To be published in the Proceedings of "International Symposium on
Structure of Exotic Nuclei and Nuclear Forces (SENUF 06)", March 2006, Tokyo,
Japa
Primordial Black Holes and -Process Nucleosynthesis
We show that some or all of the inventory of -process nucleosynthesis can
be produced in interactions of primordial black holes (PBHs) with neutron stars
(NSs) if PBHs with masses make up a few percent or more of the dark matter. A
PBH captured by a neutron star (NS) sinks to the center of the NS and consumes
it from the inside. When this occurs in a rotating millisecond-period NS, the
resulting spin-up ejects of relatively cold
neutron-rich material. This ejection process and the accompanying decompression
and decay of nuclear matter can produce electromagnetic transients, such as a
kilonova-type afterglow and fast radio bursts. These transients are not
accompanied by significant gravitational radiation or neutrinos, allowing such
events to be differentiated from compact object mergers occurring within the
distance sensitivity limits of gravitational wave observatories. The PBH-NS
destruction scenario is consistent with pulsar and NS statistics, the dark
matter content and spatial distributions in the Galaxy and Ultra Faint Dwarfs
(UFD), as well as with the -process content and evolution histories in these
sites. Ejected matter is heated by beta decay, which leads to emission of
positrons in an amount consistent with the observed 511-keV line from the
Galactic Center.Comment: 6 pages + 3 page supplement, 3 figures; matches published versio
Astrophysical Models of r-Process Nucleosynthesis: An Update
An update on astrophysical models for nucleosynthesis via rapid neutron
capture, the r process, is given. A neutrino-induced r process in supernova
helium shells may have operated up to metallicities of ~10^-3 times the solar
value. Another r-process source, possibly neutron star mergers, is required for
higher metallicities.Comment: 8 pages, invited talk given at 11th International Symposium on Origin
of Matter and Evolution of Galaxies (OMEG11), Wako, Japa
Active-Sterile Neutrino Transformation and r-Process Nucleosynthesis
The type II supernova is considered as a candidate site for the production of
heavy elements. Since the supernova produces an intense neutrino flux, neutrino
scattering processes will impact element formation. We examine active-sterile
neutrino conversion in this environment and find that it may help to produce
the requisite neutron-to-seed ratio for synthesis of the r-process elements.Comment: 5 pages including 2 figures, to appear in the Proceedings of the
Conference on the Intersections of Nuclear and Particle Physics 200
Neutrino-nucleus interaction and supernova r-process nucleosynthesis
We discuss various neutrino-nucleus interactions in connection with the
supernova r-process nucleosynthesis, which possibly occurs in the
neutrino-driven wind of a young neutron star. These interactions include
absorptions of electron neutrinos and antineutrinos on free nucleons,
electron-neutrino captures on neutron-rich nuclei, and neutral-current
interactions of heavy-flavor neutrinos with alpha particles and neutron-rich
nuclei. We describe how these interactions can affect the r-process
nucleosynthesis and discuss the implications of their effects for the physical
conditions leading to a successful supernova r-process. We conclude that a low
electron fraction and/or a short dynamic time scale may be required to give the
sufficient neutron-to-seed ratio for an r-process in the neutrino-driven wind.
In the case of a short dynamic time scale, the wind has to be contained during
the r-process. Possible mechanisms which can give a low electron fraction or
contain the wind are discussed.Comment: 8 pages, uses espcrc1.sty (included), Invited talk at the 4th
International Conference on Nuclei in the Cosmos, Notre Dame (1996
Neutrino-induced neutron spallation and supernova r-process nucleosynthesis
In order to explore the consequences of the neutrino irradiation for the
supernova r-process nucleosynthesis, we calculate the rates of charged-current
and neutral-current neutrino reactions on neutron-rich heavy nuclei, and
estimate the average number of neutrons emitted in the resulting spallation.
Our results suggest that charged-current captures can be important in
breaking through the waiting-point nuclei at N=50 and 82, while still allowing
the formation of abundance peaks. Furthermore, after the r-process freezes out,
there appear to be distinctive neutral-current and charged-current
postprocessing effects. A subtraction of the neutrino postprocessing effects
from the observed solar r-process abundance distribution shows that two mass
regions, A=124-126 and 183-187, are inordinately sensitive to neutrino
postprocessing effects. This imposes very stringent bounds on the freeze-out
radii and dynamic timescales governing the r-process. Moreover, we find that
the abundance patterns within these mass windows are entirely consistent with
synthesis by neutrino interactions. This provides a strong argument that the
r-process must occur in the intense neutrino flux provided by a core-collapse
supernova.Comment: 34 pages, 4 PostScript figures, RevTe
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