The empirical description of the level density parameter<i>a</i>in the semi-classical model

Kaczmarczyk, Maria

doi:10.1088/0954-3899/26/3/304

Cited by 8 publications

(15 citation statements)

References 8 publications

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“…It is worth pointing out that although the quantity agreement between experimental neutron resonance level density and those calculated from formula (7) (in both calculation variants, with the parameters given in tables 1 and 2) appears to be in the range of one order of magnitude, it is not worse than the results obtained, e.g., in [10][11][12].…”

Section: Discussion Of the Calculation Resultsmentioning

confidence: 56%

The choice of the optimum terms for semi-empirical description ofs-wave neutron resonance level densities

Kaczmarczyk¹,

Łasoń²

2006

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

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This paper presents a function describing the dependence of the neutron resonance level density ρ on the neutron number N in the target nucleus. The function describes quite well, with an accuracy of one order, the experimental data for 284 nuclides. Moreover, it adequately describes the general tendency and shell model effects for magic nuclei and for nuclei close to magic ones. The achieved agreement between the values obtained from the proposed description and the experimental data ρ exp can be improved if the ρ exp values are normalized energetically and reduced to a narrow range of angular momentum J.

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Section: Discussion Of the Calculation Resultsmentioning

confidence: 56%

The choice of the optimum terms for semi-empirical description ofs-wave neutron resonance level densities

Kaczmarczyk¹,

Łasoń²

2006

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

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“…Sonnentrucker et al (1999) have also found two clouds with different radial velocities observed in the 661 nm diffuse interstellar band. Kaczmarczyk (2000) recently identified two components of the interstellar C 2 bands in the ultraviolet spectra of the star X Per, also corresponding to two gaseous layers with different radial velocities. Cernis (1993) has proposed a model of distribution of the two dust layers, based on his finding that the distance of the Perseus clouds increases with the apparent approach to the Galactic equator.…”

Section: Discussionmentioning

confidence: 99%

Interstellar extinction in the California Nebula region

Straižys

Cernis

Bartasiute

2001

A&A

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Abstract. Vilnius seven-color photometry has been obtained for 238 stars down to ∼13 mag in the area of the California Nebula in Perseus. For nearly all of the stars, photometric spectral classes, luminosity classes, absolute magnitudes, interstellar reddenings, extinctions and distances are determined. The "extinction versus distance" diagrams give evidence for the presence of one dust layer at ∼160 pc distance in the direction of the California Nebula and its nearest surroundings and of two dust layers at distances of 160 pc and 300 pc northwest of the nebula, in the direction of the dark clouds L 1449 and L 1456. The front layer contributes extinction between 0.3 and 1.3 mag, and the second layer gives about 1 mag of additional extinction. It appears likely that the front dust layer is the extension of the Taurus dark clouds. The second dust layer probably belongs to the complex of dark clouds found in other areas of the southern part of Perseus (in the directions of the open cluster IC 348, the reflection nebula NGC 1333, etc.). Both cloud complexes run more or less parallel to the Galactic plane.

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“…Relatively simple combinatorial calculations [8,9] allow one to obtain the formulae, which are simple and convenient for calculating the particle-hole state densities. The final results, which are obtained on this basis for level densities ρ, can be improved if energy gaps , resulting from the shell model, are introduced into the equidistant single particle level scheme (as in our previous papers [10][11][12]), although then many more difficulties are encountered. Such a procedure, when used for determining a maximum number k of particles, raised above the Fermi level [10], resulted in the correct reproduction of the form of the dependence of the reduced neutron widths n 0 on the neutron number N in the nucleus [10].…”

Section: Introductionmentioning

confidence: 98%

The shell effects ins-wave neutron resonance level densities ρ according to combinatorial calculations and on the basis of the semi-classical approach

Kaczmarczyk¹

2005

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

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The results of calculations of level densities ρ, in the vicinity of the neutron binding energy Sn, are presented. These results were obtained using the Böhning combinatorial method for the calculation of particle-hole state densities dependent on the number of decompositions of the nucleus excitation energy to energies of independent fermions. The calculation was based on the semi-classical model description in the computation of particle-hole state densities and then of the level densities ρ, and takes into account the existence of energy gaps Δ, located near the Fermi level, in a single particle level scheme. This procedure considerably improved and extended the Böhning calculation method. The results, which were obtained in this way for ρ, for 220 nuclei, reproduce the regularities observed in the experimental values of ρ, which are dependent on the neutron number N, and they agree with the experimental data within two orders of magnitude. In addition, the neutron resonance densities ρ were calculated on the basis of the particle-hole state densities obtained using the analytical formula from Böhning's paper. To make the calculations possible, the values of ‘complexity’ k, as given in the semi-classical model, and the spin factors R(J), according to the paper by Ryckbosch, were used.

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The empirical description of the level density parameterain the semi-classical model

Cited by 8 publications

References 8 publications

The choice of the optimum terms for semi-empirical description ofs-wave neutron resonance level densities

The choice of the optimum terms for semi-empirical description ofs-wave neutron resonance level densities

Interstellar extinction in the California Nebula region

The shell effects ins-wave neutron resonance level densities ρ according to combinatorial calculations and on the basis of the semi-classical approach

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