10,417 research outputs found
Production of 92Nb, 92Mo, and 146Sm in the gamma-process in SNIa
The knowledge of the production of extinct radioactivities like 92Nb and
146Sm by photodisintegration processes in ccSN and SNIa models is essential for
interpreting abundances in meteoritic material and for Galactic Chemical
Evolution (GCE). The 92Mo/92Nb and 146Sm/144Sm ratios provide constraints for
GCE and production sites. We present results for SNIa with emphasis on nuclear
uncertainties.Comment: 6 pages, 4 figures, Proceedings of the 13th Symposium on Nuclei in
the Cosmos (NIC XIII), July 2014, Debrecen, Hungar
Liftable vector fields over corank one multigerms
In this paper, a systematic method is given to construct all liftable vector
fields over an analytic multigerm of
corank at most one admitting a one-parameter stable unfolding.Comment: 34 pages. In ver. 2, several careless mistakes for calculations in
Section 6 were correcte
Systematic study of the SO(10) symmetry breaking vacua in the matrix model for type IIB superstrings
We study the properties of the space-time that emerges dynamically from the
matrix model for type IIB superstrings in ten dimensions. We calculate the free
energy and the extent of space-time using the Gaussian expansion method up to
the third order. Unlike previous works, we study the SO(d) symmetric vacua with
all possible values of d within the range , and observe clear
indication of plateaus in the parameter space of the Gaussian action, which is
crucial for the results to be reliable. The obtained results indeed exhibit
systematic dependence on d, which turns out to be surprisingly similar to what
was observed recently in an analogous work on the six-dimensional version of
the model. In particular, we find the following properties: i) the extent in
the shrunken directions is given by a constant, which does not depend on d; ii)
the ten-dimensional volume of the Euclidean space-time is given by a constant,
which does not depend on d except for d = 2; iii) The free energy takes the
minimum value at d = 3. Intuitive understanding of these results is given by
using the low-energy effective theory and some Monte Carlo results.Comment: 33 pages, 10 figures; minor corrections, reference added. arXiv admin
note: substantial text overlap with arXiv:1007.088
Abundance Uncertainties Obtained With the PizBuin Framework For Monte Carlo Reaction Rate Variations
Uncertainties in nucleosynthesis models originating from uncertainties in
astrophysical reaction rates were estimated in a Monte Carlo variation
procedure. Thousands of rates were simultaneously varied within individual,
temperature-dependent errors to calculate their combined effect on final
abundances. After a presentation of the method, results from application to
three different nucleosynthesis processes are shown: the -process and
the s-process in massive stars, and the main s-process in AGB stars
(preliminary results). Thermal excitation of nuclei in the stellar plasma and
the combined action of several reactions increase the final uncertainties above
the level of the experimental errors. The total uncertainty, on the other hand,
remains within a factor of two even in processes involving a large number of
unmeasured rates, with some notable exceptions for nuclides whose production is
spread over several stellar layers and for s-process branchings.Comment: 8 pages, 4 figures; Proceedings of OMEG 2017, Daejeon, Korea, June
27-30, 2017; to appear in AIP Conf. Pro
Theory considerations for nucleosynthesis beyond Fe with special emphasis on p-nuclei in massive stars
T. Rauscher, N. Nishimura, and R. Hirschi, ‘Theory considerations for nucleosynthesis beyond Fe with special emphasis on p-nuclei in massive stars’, in proceedings CETUP* 2015 – Workshop on Dark Matter, Neutrino Physics and Astrophysics PPC 2015 – IXth International Conference on Interconnections between Particle Physics and Cosmology. Deadwood, South Dakota, USA. 15-17 July 2015. Barbara Szczerbinska, Rouzbeh Allahverdi, Kaladi Babu, Baha Balantekin, Bhaskar Dutta, Teruki Kamon, Jason Kumar, Farinaldo Queiroz, Louis Strigari, and Rebecca Surman eds., AIP Conference Proceedings 1743, 040008 (2016); doi: http://dx.doi.org/10.1063/1.4953300ISBN 9780735414006. Published by AIP Publishing.Nucleosynthesis of heavy elements requires the use of different experimental and theoretical methods to determine astrophysical reaction rates than light element nucleosynthesis. Additionally, there are also larger uncertainties involved in the astrophysical models, both because the sites are not well known and because of differing numerical treatments in different models. As an example for the latter, the production of p-nuclei is compared in two different stellar models, demonstrating that a model widely used for postproduction calculations may have a zone grid too coarse to follow the synthesis of p-nuclei in detail
Sensitivity to neutron captures and β-decays of the enhanced s-process in rotating massive stars at low metallicities
© 2018 IOP Publishing Ltd. Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. https://creativecommons.org/licenses/by/3.0/The s-process in massive stars, producing nuclei up to A ≈ 90, has a different behaviour at low metallicity if stellar rotation is significant. This enhanced s-process is distinct from the s-process in massive stars around solar metallicity, and details of the nucleosynthesis are poorly known. We investigated nuclear physics uncertainties in the enhanced s-process in metalpoor stars within a Monte-Carlo framework. We applied temperature-dependent uncertainties of reaction rates, distinguishing contributions from the ground state and from excited states. We found that the final abundance of several isotopes shows uncertainties larger than a factor of 2, mostly due to the neutron capture uncertainties. A few nuclei around branching points are affected by uncertainties in the β-decay.Peer reviewe
Particle Energization in an Expanding Magnetized Relativistic Plasma
Using a 2-1/2-dimensional particle-in-cell (PIC) code to simulate the
relativistic expansion of a magnetized collisionless plasma into a vacuum, we
report a new mechanism in which the magnetic energy is efficiently converted
into the directed kinetic energy of a small fraction of surface particles. We
study this mechanism for both electron-positron and electron-ion (mi/me=100, me
is the electron rest mass) plasmas. For the electron-positron case the pairs
can be accelerated to ultra-relativistic energies. For electron-ion plasmas
most of the energy gain goes to the ions.Comment: 7 pages text plus 5 figures, accepted for publication by Physical
Review Letter
The s-process nucleosynthesis : Impact of the uncertainties in the nuclear physics determined by monte carlo variations
We investigated the impact of uncertainties in neutron-capture and weak reactions (on heavy elements) on the s-process nucleosynthesis in low-mass stars and massive stars using a Monte-Carlo based approach. We performed extensive nuclear reaction network calculations that include newly evaluated temperature-dependent upper and lower limits for the individual reaction rates. We found β-decay rate uncertainties affect only a few nuclei near s-process branchings, whereas most of the uncertainty in the final abundances is caused by uncertainties in the neutron capture rates. We suggest a list of uncertain rates as candidates for improved measurement by future experiments.Peer reviewe
- …