Nuclear masses and deformations

Myers, William D.; Świa̧tecki, W.J.

doi:10.1016/0029-5582(66)90639-0

Cited by 1,090 publications

(944 citation statements)

References 26 publications

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“…The fit of LGM binding energies to this four parameter formula is quite good. We compare the four parameters deduced from LGM to liquid-drop model values [143] in the table. Considering the simplicity of the model, the agreement is gratifying.…”

Section: Isospin Dependent Lgm Including Coulomb Interactionmentioning

confidence: 99%

Liquid-Gas Phase Transition in Nuclear Multifragmentation

Gupta

Mekjian

Tsang

2001

Advances in the Physics of Particles and Nuclei

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The equation of state of nuclear matter suggests that at suitable beam energies the disassembling hot system formed in heavy ion collisions will pass through a liquid-gas coexistence region. Searching for the signatures of the phase transition has been a very important focal point of experimental endeavours in heavy-ion collisions, in the last fifteen years. Simultaneously theoretical models have been developed to provide information about the equation of state and reaction mechanisms consistent with the experimental observables.

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Section: Isospin Dependent Lgm Including Coulomb Interactionmentioning

confidence: 99%

Liquid-Gas Phase Transition in Nuclear Multifragmentation

Gupta

Mekjian

Tsang

2001

Advances in the Physics of Particles and Nuclei

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“…The In figure 2 we plotted the individual errors: differences of log 10 T theor − log 10 T exp in four groups of alpha emitters. Vertical dashed lines are marking magic numbers of neutrons, either spherical (50,82,126) or deformed (152, 162, 172). One can see that the best result is always obtained for even-even alpha emitters.…”

Section: Semfis (Semiempirical Relationship Based On Fission Theormentioning

confidence: 99%

“…E corr is a correction energy similar to the Strutinsky [49] shell correction, also taking into account the fact that Myers-Swiatecki's liquid drop model (LDM) [50] overestimates fission barrier heights, and the effective inertia in the overlapping region is different from the reduced mass. The turning points of the WKB integral are:…”

Section: Introductionmentioning

confidence: 99%

Alpha decay calculations with a new formula

Akrawy¹,

Poenaru

2017

J. Phys. G: Nucl. Part. Phys.

106

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A new semi-empirical formula for calculations of α decay halflives is presented. It was derived from Royer relationship by introducing new parameters which are fixed by fit to a set of experimental data. We are using three sets: set A with 130 e-e (even-even), 119 e-o (even-odd), 109o-e, and 96 o-o, set B with 188 e-e, 147 e-o, 131 o-e, and 114 o-o, and set C with 136 e-e, 84 e-o, 76 o-e, and 48 o-o alpha emitters. A comparison of results obtained with the new formula and the following well known relationships: semFIS (semiempirical based on fission theory); ASAF (analytical superAsymmetric fission) model, and UNIV (universal formula) is made in terms of rms standard deviation. We also introduced a weighted mean value of this quantity, allowing to compare the global properties of a given model. For the set B the order of the four models is the following: semFIS; UNIV; newF, and ASAF. Nevertheless for even-even alpha emitters UNIV gives the 2nd best result after semFIS, and for odd-even parents the 2nd is newF. Despite its simplicity in comparison with semFIS the new formula, presented in this article, behaves quite well, competing with the others well known relationships

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“…We then add to equation (1) ′ a shell correction term that was originally developed for isolated nuclei by Myers & Swiatecki (1966) and extended to nuclei in the drippedneutron regime by Sato (1979):…”

Section: Inner Crustmentioning

confidence: 99%

Spin-Down of Neutron Stars and Compositional Transitions in the Cold Crustal Matter

Iida

Sato

1998

The Hot Universe

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Transitions of nuclear compositions in the crust of a neutron star induced by stellar spin-down are evaluated at zero temperature. We construct a compressible liquiddrop model for the energy of nuclei immersed in a neutron gas, including pairing and shell correction terms, in reference to the known properties of the ground state of matter above neutron drip density, 4.3 × 10 11 g cm −3 . Recent experimental values and extrapolations of nuclear masses are used for a description of matter at densities below neutron drip. Changes in the pressure of matter in the crust due to the stellar spin-down are calculated by taking into account the structure of the crust of a slowly and uniformly rotating relativistic neutron star. If the initial rotation period is ∼ ms, these changes cause nuclei, initially being in the ground-state matter above a mass density of about 3 × 10 13 g cm −3 , to absorb neutrons in the equatorial region where the matter undergoes compression, and to emit them in the vicinity of the rotation axis where the matter undergoes decompression. Heat generation by these processes is found to have significant effects on the thermal evolution of old neutron stars with low magnetic fields; the surface emission predicted from this heating is compared with the ROSAT observations of X-ray emission from millisecond pulsars and is shown to be insufficient to explain the observed X-ray luminosities.

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Nuclear masses and deformations

Cited by 1,090 publications

References 26 publications

Liquid-Gas Phase Transition in Nuclear Multifragmentation

Liquid-Gas Phase Transition in Nuclear Multifragmentation

Alpha decay calculations with a new formula

Spin-Down of Neutron Stars and Compositional Transitions in the Cold Crustal Matter

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