Energy levels of light nuclei

Purcell, J.E.; Kelley, J. H.; Kwan, E.; Sheu, C.G.; Weller, H. R.

doi:10.1016/j.nuclphysa.2010.08.012

Cited by 52 publications

(43 citation statements)

References 759 publications

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“…In the last column, δv ij is the expectation value of the difference between v 18 and v 8 , which is the part of the NN interaction that is treated perturbatively because v 8 is used in the propagation Hamiltonian. The sum of the six contributions K through V R ijk does not quite match the total energy reported in Table I (Brida et al, 2011;Lovato et al, 2013;McCutchan et al, 2012;Pastore et al, 2013Pastore et al, , 2014Pieper and Carlson, 2015;Wiringa et al, 2013), compared to experimental values (Amroun et al, 1994;NNDC, 2014;Nörtershäuser and et al, 2009;Nörtershäuser et al, 2011;Purcell et al, 2010;Shiner et al, 1994;Tilley et al, 2002Tilley et al, , 2004. Numbers in parentheses are statistical errors for the GFMC calculations or experimental errors; errors of less than one in the last decimal place are not shown.…”

Section: Light Nuclei a Energy Spectramentioning

confidence: 83%

Quantum Monte Carlo methods for nuclear physics

et al. 2015

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Quantum Monte Carlo methods have proved very valuable to study the structure and reactions of light nuclei and nucleonic matter starting from realistic nuclear interactions and currents. These ab-initio calculations reproduce many low-lying states, moments and transitions in light nuclei, and simultaneously predict many properties of light nuclei and neutron matter over a rather wide range of energy and momenta. We review the nuclear interactions and currents, and describe the continuum Quantum Monte Carlo methods used in nuclear physics. These methods are similar to those used in condensed matter and electronic structure but naturally include spin-isospin, tensor, spin-orbit, and three-body interactions. We present a variety of results including the low-lying spectra of light nuclei, nuclear form factors, and transition matrix elements. We also describe low-energy scattering techniques, studies of the electroweak response of nuclei relevant in electron and neutrino scattering, and the properties of dense nucleonic matter as found in neutron stars. A coherent picture of nuclear structure and dynamics emerges based upon rather simple but realistic interactions and currents.

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Section: Light Nuclei a Energy Spectramentioning

confidence: 83%

Quantum Monte Carlo methods for nuclear physics

et al. 2015

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“…[33], EM moments are from Refs. [34][35][36][37], and point radii are converted from the charge radii given in Refs. [38][39][40][41][42].…”

Section: Resultsmentioning

confidence: 99%

Quantum Monte Carlo calculations of electromagnetic moments and transitions inA≤9nuclei with meson-exchange currents derived from chiral effective field theory

et al. 2013

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Quantum Monte Carlo calculations of electromagnetic moments and transitions are reported for A ≤ 9 nuclei. The realistic Argonne v18 two-nucleon and Illinois-7 three-nucleon potentials are used to generate the nuclear wave functions. Contributions of two-body meson-exchange current (MEC) operators are included for magnetic moments and M 1 transitions. The MEC operators have been derived in both a standard nuclear physics approach and a chiral effective field theory formulation with pions and nucleons including up to one-loop corrections. The two-body MEC contributions provide significant corrections and lead to very good agreement with experiment. Their effect is particularly pronounced in the A = 9, T = 3/2 systems, in which they provide up to ∼ 20% (∼ 40%) of the total predicted value for the 9 Li ( 9 C) magnetic moment.

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“…However, the abundance of 3 H for the first 100-200 s after the Big Bang cannot be much smaller than that of 2 H since the neutron capture reaction, in spite of the reduction of neutron numbers down to 0.2 of the proton numbers, can go on deuteron at any energy. In addition, the half-life of 3 H is 4500 (8) days [24] and do not make a real contribution to the decrease of the number of 3 H at the first few minutes after the Big Bang.…”

Section: Nomentioning

confidence: 96%

New results for reaction rate of the proton radiative capture on 3 H

Dubovichenko

Dzhazairov-Kakhramanov

Afanasyeva

2017

Nuclear Physics A

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Calculations of the reaction rate of the proton radiative capture on 3 H at temperatures from 0.01 Т 9 up to 5 Т 9 , which are based on the theoretical results for the astrophysical S-factor and take into account the latest experimental data, were carried out. Theoretical results for the S-factor at energies from 1 keV up to 5 MeV were obtained in the framework of the modified potential cluster model with the classification of orbital states according to Young tableaux. On the basis of used nuclear model of the interaction of p and 3 H particles there was shown possibility of description the latest experimental data for the S-factor at the energy range from 50 keV up to 5 MeV. Numbers: 21.60.Gx, 25.40.Lx, 26.35.+c, 26. Reaction No.12 proceeds with comparatively low probability, since the E1 process is forbidden by the isospin selection rules. This leads to the factor   J J J

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Energy levels of light nuclei

Cited by 52 publications

References 759 publications

Quantum Monte Carlo methods for nuclear physics

Quantum Monte Carlo methods for nuclear physics

Quantum Monte Carlo calculations of electromagnetic moments and transitions inA≤9nuclei with meson-exchange currents derived from chiral effective field theory

New results for reaction rate of the proton radiative capture on 3 H

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