Low energy (p,\gamma) reactions in Ni and Cu nuclei using microscopic optical model

Low energy () reactions in Ni and Cu nuclei using microscopic optical model

Abstract

Radiative capture reactions for low energy protons have been theoretically studied for Ni and Cu isotopes using the microscopic optical model. The optical potential has been obtained in the folding model using different microscopic interactions with the nuclear densities from Relativistic Mean Field calculations. The calculated total cross sections as well as the cross sections for individually low lying levels have been compared with measurements involving stable nuclear targets. Rates for the rapid proton capture process have been evaluated for astrophysically important reactions.

PACS Numbers :25.40.Lw, 24.10.Ht, 27.40.+z, 27.50.+e

Optical model potentials constructed utilizing microscopic densities from standard nuclear models have proved to be very successful in describing low energy nuclear reactions. Elastic scattering calculations using such potentials have been able to explain the observed cross sections even in nuclei far off the stability valley. Low energy projectiles probe only the outermost part of the target nuclei. Hence the nuclear skin plays a very important role in such reactions. Theoretical models can provide a good description of the density profile and is capable of producing excellent estimates of reaction cross sections. Alternatively, the ability of different models to reproduce the nuclear density profile may be compared from their ability to predict reaction cross sections.

Proton capture reactions at low energy are important to understand the astrophysical process. At energies below the Coulomb barrier the cross sections are small. However, as the Gamow window lies entirely below the barrier, estimation of the cross section below the barrier is of crucial importance. We note that capture may lead to the ground state, to the excited states or to the continuum of the compound nucleus.

Relativistic Mean Field (RMF) approach is now a standard tool in low energy nuclear structure. It has been able to explain different features of stable and exotic nuclei like ground state binding energy, deformation, radius, excited states, spin-orbit splitting, neutron halo, etc[1]. RMF is known to provide a good description of various features in mass region [See [2] and Refs. therein]. There are different variations of the Lagrangian density as well as a number of different parametrizations. In the present work we have employed three such densities, NL3[3], TM1[4], and FSU Gold[5], to study ( reactions in stable Ni and Cu nuclei. The NL3 density contains, apart from the usual terms for a nucleon meson system, nonlinear terms involving self coupling of scalar-isoscalar meson. The TM1 density includes additional terms describing self-coupling of the vector-isoscalar meson. The FSU Gold density includes coupling between the vector-isoscalar meson and the vector-isovector meson as well. We note that results of our cross section calculation for all the three Lagrangian densities are practically identical and present the results for FSU Gold only.

In the conventional RMF+BCS approach, the equations obtained are solved under the assumptions of classical meson fields, time reversal symmetry, no-sea contribution, etc. Pairing is introduced under the BCS approximation. Usually the resulting equations are solved in a harmonic oscillator basis [6]. However, since we need the densities in co-ordinate space, a solution of the Dirac and Klein Gordon equations in co-ordinate space has been preferred. This approach has earlier been used [7, 2, 8] to study neutron rich nuclei in different mass regions. We have found that the present method describes the properties of the nuclei with equally well as the more involved Relativistic Hartree Bogoliubov approach. In the second and the third columns of Table 1, we compare the results for the binding energy values for the stable isotopes for FSU Gold. The valence neutron proton correlation correction has been taken care of following the prescription of Ref.[11]. Much more important from the point of the density profile are the next two columns where we compare the measured charge radii () with theory. The latter values have been obtained from the point proton distribution () using the simple prescription , all quantities given in . The results show that RMF can describe the ground state of these nuclei with sufficient accuracy.

B.E.(MeV)
Exp. Theo. Exp. Theo. JLM DDM3Y
Ni 506.46 508.83 3.775 3.751 0.85 0.85
Ni 526.84 527.50 3.812 3.779 0.60 0.60
Ni 534.66 535.05 3.822 3.792 0.70 0.70
Ni 545.26 544.71 3.841 2.828 0.60 0.60
Ni 561.76 561.97 3.859 3.827 0.95 0.80
Cu 551.38 551.17 3.883 3.848 0.55 0.55
Cu 569.21 569.43 3.902 3.866 0.95 0.95
Table 1: Experimental binding energies[9] and radii[10] compared with calculated values for the FSU Gold Lagrangian density. The values used in different isotopes are also indicated in the last two columns. See text for details.

The optical model potentials for the reactions are obtained using two effective interactions derived from the nuclear matter calculation in the local density approximation, i.e. by substituting the nuclear matter density with the density distribution of the finite nucleus. Thus the microscopic nuclear potentials have been obtained by folding the effective interactions with the microscopic densities from the RMF calculation. The Coulomb potentials have been similarly generated by folding the Coulomb interaction with the microscopic proton densities. We have already used such potentials to calculate life times for proton, alpha and cluster radioactivity[12] as well as elastic proton scattering[7] in different mass regions of the periodic table.

One of the interactions chosen in the present work is the interaction of Jeukenne, Lejeune, and Mahaux (JLM)[13] in which further improvement is incorporated in terms of the finite range of the effective interaction by including a Gaussian form factor. We have used the global parameters for the effective interaction and the respective default normalizations for the potential components from Refs. [14] and [15] with Gaussian range values of and .

We have also used the density dependent interaction DDM3Y[16, 17] in the present work. This was obtained from a finite range energy independent M3Y interaction by adding a zero range energy dependent pseudopotential and introducing a density dependent factor. This interaction has been employed widely in the study of nucleon nucleus as well as nucleus nucleus scattering, calculation of proton radioactivity, etc. The density dependence has been chosen in the form [17]. The constants were obtained from nuclear matter calculation[18] as and . For scattering we have taken real and the imaginary parts of the potential as 0.9 times and 0.1 times the DDM3Y potential, respectively.

The reaction calculations have been performed with the computer code TALYS 1.2[19] assuming spherical symmetry for the target nuclei. The DDM3Y interaction is not a standard part of TALYS but can easily be incorporated. Since nuclear matter-nucleon potential does not include a spin-orbit term, the TALYS 1.2 code obtains the spin-orbit potential from the Scheerbaum prescription[20] coupled with the phenomenological complex potential depths and .

(1)

The depths are functions of energy, given by and , in MeV. This has been used in the calculations of both the interactions.

The TALYS code has a number of features useful to study reactions. We have employed the full Hauser-Feshbach calculation with transmission coefficients averaged over total angular momentum values and with corrections due to width fluctuations. Hilaire’s microscopic level density values included in the code has been used though we have confirmed that the results are not substantially modified if a different level density formulae is assumed. Up to twenty five discrete levels of the compound nucleus have been included in the calculation. The gamma ray strength has been calculated in the Hartree-Fock-Bogoliubov model. However, we find that though the trends have been correctly reproduced in all the cases, the actual values of the cross sections are often overpredicted. Thus the gamma ray strength was visually normalized to match with the experimentally observed cross sections using the parameter in the code though no fit was performed. In the last two columns of Table 1 we tabulate the values of this parameter used for the different targets. We should also mention that in the case of Ni, the experimental values from different measurements differ by a large amount and we have chosen the latest measurements to determine .

In Figure 1, we have compared our results with various experimental measurements in Ni isotopes and have found reasonable agreement. in Figure 2, we present the results for stable Cu isotopes. As the astrophysically important Gamow window lies in the region 1.1 to 3.3 MeV for these nuclei, we compare the results up to 3.5 MeV proton energy. As already mentioned, is the only parameter that we have modified to normalize the experimental data. All the other parameters in the Lagrangian density and the interaction are standard ones and have not been changed. The DDM3Y and the JLM interactions perform almost identically in almost all the nuclei. The former sometimes appears to produce slightly better results, but in view of the large disagreement between different measurements, this conclusion remains very tentative. We see that our calculation can explain cross section values ranging over three orders of magnitude and also beyond the neutron evaporation threshold. We note here that the default local and global optical potentials [30] in the TALYS package also can be used with suitable normalization of gamma ray strength to produce comparable results for certain energy ranges. For example, with , the results for the low energy values for DDM3Y and results using the default potentials are nearly identical in Ni() reaction but above the neutron evaporation threshold, the predictions by the default potentials, using the same value, are definitely poorer compared to those of the microscopic calculations.

The cross-sections corresponding to the different low lying levels of the compound nucleus has been measured in some of the above reactions. In Figure 3, we show the results for the ground state and the first two excited states in the Cu()Zn reactions using the inputs of the TALYS 1.2 code and the corresponding experimental measurements. Similar agreements are also observed in Ni isotopes. The results are for JLM interaction only. The DDM3Y results are nearly identical. We may conclude the present method to be suitable to describe the proton capture cross section by stable Ni and Cu isotopes.

With the success of the present approach, we have employed it to calculate the astrophysical rapid proton capture rate in Ni and Cu nuclei. Nucleosynthesis theories[34] suggest that the above process is very important in Ni and Cu for which we present our results in Figure 4. Since the laboratory cross sections are not available for the two unstable targets, we have assumed . We also compare our results with two theoretical calculations, based on the Hauser-Feshbach formalism code NON-SMOKER[35] and Shell model[36], respectively. The stellar enhancement factor has not been incorporated in the results. The results for DDM3Y interaction are nearly identical and have not been plotted. We note that there are substantial differences between the three calculations in the case of Ni, particularly the NON-SMOKER results being much larger compared to the present ones. We find that the cross sections from the NON-SMOKER code [35] are very much larger than experimental measurements as one goes to proton rich Ni isotopes. Thus we may expect the astrophysical rates from [35] to be greater in Ni.

In summary, cross sections for low energy () reactions for stable Ni and Cu nuclei have been calculated using the TALYS code. The microscopic optical potential has been obtained by folding two different microscopic interactions, JLM and DDM3Y, with the densities of the target nuclei obtained from three different RMF Lagrangian densities, viz. NL3, TM1, and FSU Gold. Astrophysical rates for the process have been calculates and compared with standard calculations in two important nuclei Ni and Cu.

Acknowledgement

This work has been carried out with financial assistance of the UGC sponsored DRS Programme of the Department of Physics of the University of Calcutta. The author gratefully acknowledges the hospitality of the ICTP, Trieste where a part of the work was carried out.

Figure 1: Cross sections for () reactions in stable Ni isotopes. The mass numbers of the target nuclei are indicated. The data are form Refs. [21] (open square), [22] (filled square), [23] (filled circle), [24] (open circle), [25] (filled triangle), [26] (open triangle) and [27] (diamond). The solid and the dashed lines refer to results for JLM and DDM3Y interactions, respectively.
Figure 2: Cross sections for () reactions in stable Cu isotopes. The data are from [27](open square),[28](filled square) and [29] (open circle). See caption of Figure 1 for details.
Figure 3: Partial cross sections for Cu() reactions to the low lying states in Zn. Open (filled) symbols refer to data from [31]([32]). Squares, circles and triangles represent data for transition to the ground state and to the first excited state (multiplied by 10) and the second excited state (multiplied by 100), respectively. The mass numbers of the target nuclei are indicated.
Figure 4: Astrophysical proton capture rates in (a) Ni and (b)Cu given by present work (solid line), NON-SMOKER calculation [35](dashed line) and Shell Model results[36] (dotted line).

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