Results 21 to 30 of about 6,528,274 (245)

Search for neutron-hidden neutron interbrane transitions with MURMUR, a low-noise neutron passing-through-walls experiment [PDF]

open access: yesEPJ Web of Conferences, 2019
Multi-braneworld universe is at the heart of many scenarios of physics beyond the Standard Model and the cosmological model ΛCDM. It is thus an important concern to constrain these scenarios which also allow for experiments below the GeV scale. MURMUR is
Stasser Coraline   +2 more
doaj   +1 more source

Nuclear Energy Levels in 44Ca using FPD6pn Interaction

open access: yesEast European Journal of Physics, 2023
Nuclear energy levels; total angular moment, even-even parity, and even odd parities for nucleons that were present outside closed core for the isobars 44Ca nuclei, which occupied low levels fp-LS shell (1f7/2,1f5/2, 2p3/2,2p1/2), within shell model ...
Maryam K. Hassan, Firas Z. Majeed
doaj   +1 more source

s-process Nuclear Reaction Rates [PDF]

open access: yesEPJ Web of Conferences, 2023
In stars the 13C(α, n)16O and 22Ne(α, n)25Mg reactions are the two main sources of neutrons for the so-called slow neutron capture process (s-process), which is one of the main mechanisms for the stellar synthesis of heavy elements.
Rapagnani David
doaj   +1 more source

Journey to the cosmos: Navigating stellar evolution with differential equations

open access: yesAlifmatika, 2023
Differential equations are a fundamental and versatile mathematical tool that finds widespread application across diverse academic disciplines, from physics and biology to economics and engineering.
Anshuman Jha   +3 more
doaj   +1 more source

Influence of Nuclear Reaction Rate Uncertainties on Neutron Star Properties Extracted from X-Ray Burst Model–Observation Comparisons [PDF]

open access: yesAstrophysical Journal, 2018
Type-I X-ray bursts can be used to determine properties of accreting neutron stars via comparisons between model calculations and astronomical observations, exploiting the sensitivity of models to astrophysical conditions.
Z. Meisel, G. Merz, Sophia Medvid
semanticscholar   +1 more source

Investigation of the production of cobalt-60 via particle accelerator [PDF]

open access: yesNuclear Technology and Radiation Protection, 2017
The production process of cobalt-60 was simulated by a particle accelerator in the energy range of 5 to 100 MeV, particle beam current of 1 mA, and irradiation time of 1 hour to perform yield, activity of reaction, and integral yield for charged
Artun Ozan
doaj   +1 more source

Pynucastro: an Interface to Nuclear Reaction Rates and Code Generator for Reaction Network Equations [PDF]

open access: yesJournal of Open Source Software, 2018
pynucastro addresses two needs in the field of nuclear astrophysics: visual exploration of nuclear reaction rates or networks and automated code generation for integrating reaction network ODEs.
D. Willcox, M. Zingale
semanticscholar   +1 more source

Optical Radiation from the Sputtered Species under Excitation of Ternary Mixtures of Noble Gases by the 6Li(n,α)3H Nuclear Reaction Products

open access: yesEurasian Chemico-Technological Journal, 2021
The present paper examines the luminescence of ternary Ar-Kr-Xe and Ne-Ar-Kr mixtures of noble gases in the spectral range from 300 to 970 nm, excited by the 6Li(n,α)3H nuclear reaction products in the core of a nuclear reactor.
K. Samarkhanov   +7 more
doaj   +1 more source

SkyNet: A Modular Nuclear Reaction Network Library [PDF]

open access: yes, 2017
Almost all of the elements heavier than hydrogen that are present in our solar system were produced by nuclear burning processes either in the early universe or at some point in the life cycle of stars.
J. Lippuner, L. Roberts
semanticscholar   +1 more source

Collective Inertial Masses in Nuclear Reactions

open access: yesFrontiers in Physics, 2020
Toward the microscopic theoretical description for large amplitude collective dynamics, we calculate the coefficients of inertial masses for low-energy nuclear reactions.
Kai Wen   +3 more
doaj   +1 more source

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