18,494 research outputs found
A mobile antineutrino detector with plastic scintillators
We propose a new type segmented antineutrino detector made of plastic
scintillators for the nuclear safeguard application. A small prototype was
built and tested to measure background events. A satisfactory unmanned field
operation of the detector system was demonstrated. Besides, a detailed Monte
Carlo simulation code was developed to estimate the antineutrino detection
efficiency of the detector.Comment: 23 pages, 11 figures; accepted for publication in Nuclear Instruments
and Methods in Physics Research
Probing r-Process Production of Nuclei Beyond Bi209 with Gamma Rays
We estimate gamma-ray fluxes due to the decay of nuclei beyond Bi209 from a
supernova or a supernova remnant assuming that the r-process occurs in
supernovae. We find that a detector with a sensitivity of about 10**(-7)
photons/cm**2/s at energies of 40 keV to 3 MeV may detect fluxes due to the
decay of Ra226, Th229, Am241, Am243, Cf249, and Cf251 in the newly discovered
supernova remnant near Vela. In addition, such a detector may detect fluxes due
to the decay of Ac227 and Ra228 produced in a future supernova at a distance of
about 1 kpc. As nuclei with mass numbers A > 209 are produced solely by the
r-process, such detections are the best proof for a supernova r-process site.
Further, they provide the most direct information on yields of progenitor
nuclei with A > 209 at r-process freeze-out. Finally, detection of fluxes due
to the decay of r-process nuclei over a range of masses from a supernova or a
supernova remnant provides the opportunity to compare yields in a single
supernova event with the solar r-process abundance pattern.Comment: 24 pages, 3 figures, to appear in the October 10, 1999 issue of Ap
Supernovae as the Site of the r-Process: Implications for Gamma-Ray Astronomy
We discuss how detection of gamma-ray emission from the decay of r-process
nuclei can improve our understanding of r-process nucleosynthesis. We find that
a gamma-ray detector with a sensitivity of 10**(-7)/cm**2/s at 100-700 keV may
detect the emission from the decay of Sb125, Cs137, Ce144, Eu155, and Os194
produced in a future Galactic supernova. In addition, such a detector may
detect the emission from the decay of Sn126 in the Vela supernova remnant and
the diffuse emission from the decay of Sn126 produced by past supernovae in our
Galaxy. The required detector sensitivity is similar to what is projected for
the proposed Advanced Telescope for High Energy Nuclear Astrophysics (ATHENA).
Both the detection of gamma-ray emission from the decay of several r-process
nuclei (e.g., Sb125 and Os194) produced in future Galactic supernovae and the
detection of emission from the decay of Sn126 in the Vela supernova remnant
would prove that supernovae are a site of the r-process. Furthermore, the
former detection would allow us to determine whether or not the r-process
nuclei are produced in relative proportions specified by the solar r-process
abundance pattern in supernova r-process events. Finally, detection of diffuse
emission from the decay of Sn126 in our Galaxy would eliminate neutron
star/neutron star mergers as the main source for the r-process nuclei near mass
number A=126.Comment: 14 pages, AASTeX, submitted to the Astrophysical Journa
Neutrino-induced nucleosynthesis and the site of the r process
If the r process occurs deep within a type II supernova, probably the most popular of the proposed sites, abundances of r-process elements may be altered by the intense neutrino flux. We point out that the effects would be especially pronounced for eight isotopes that can be efficiently synthesized by the neutrino reactions following r-process freeze-out. We show that the observed abundances of these isotopes are entirely consistent with neutrino-induced nucleosynthesis, strongly arguing for a supernova r-process site. The deduced neutrino fluences place stringent constraints on the freeze-out radius and dynamic time scale of the r process
Quantum state tomography with quantum shotnoise
We propose a scheme for a complete reconstruction of one- and two-particle
orbital quantum states in mesoscopic conductors. The conductor in the transport
state continuously emits orbital quantum states. The orbital states are
manipulated by electronic beamsplitters and detected by measurements of average
currents and zero frequency current shotnoise correlators. We show how, by a
suitable complete set of measurements, the elements of the density matrices of
the one- and two-particle states can be directly expressed in terms of the
currents and current correlators.Comment: 4 pages, 2 figure
Diverse Supernova Sources for the r-Process
(Abridged) It is shown that a semi-quantitative agreement with the gross
solar r-process abundance pattern near and above mass number A=130 can be
obtained by a superposition of two distinctive kinds of supernova r-process
events. These correspond to a low frequency case L and a high frequency case H,
which takes into account the low abundance of I129 and the high abundance of
Hf182 in the early solar nebula. The lifetime of Hf182 associates the events in
case H with the most common Type II supernovae. These events would be mainly
responsible for the r-process nuclei near and above A=195. They would also make
a significant amount of the nuclei between A=130 and 195, including Hf182, but
very little I129. In order to match the solar r-process abundance pattern and
to satisfy the I129 and Hf182 constraints, the events in case L, which would
make the r-process nuclei near A=130 and the bulk of those between A=130 and
195, must occur 10 times less frequently but eject 10--20 times more r-process
material in each event. We speculate that the usual neutron star remnants, and
hence prolonged ejection of r-process material, are associated with the events
in case L, whereas the more frequently occurring events in case H have ejection
of other r-process material terminated by black hole formation during the
neutrino cooling phase of the protoneutron star.Comment: 23 pages, AAS LATEX, 8 Postscript figure
NASA Workshop on future directions in surface modeling and grid generation
Given here is a summary of the paper sessions and panel discussions of the NASA Workshop on Future Directions in Surface Modeling and Grid Generation held a NASA Ames Research Center, Moffett Field, California, December 5-7, 1989. The purpose was to assess U.S. capabilities in surface modeling and grid generation and take steps to improve the focus and pace of these disciplines within NASA. The organization of the workshop centered around overviews from NASA centers and expert presentations from U.S. corporations and universities. Small discussion groups were held and summarized by group leaders. Brief overviews and a panel discussion by representatives from the DoD were held, and a NASA-only session concluded the meeting. In the NASA Program Planning Session summary there are five recommended steps for NASA to take to improve the development and application of surface modeling and grid generation
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