TALYS calculation and a short review of the experimental status of proton capture studies onp-nuclei: A guide to future investigation

Hydrogen and helium are the two most abundant elements in the Universe and were formed in the primordial or Big Bang nucleosynthesis. The stellar nucleosynthesis starts with a sequential reaction called the pp1-chain [1−3], which involves fusion of H to form He. Once the H fuel becomes exhausted, He starts burning to form the next most abundant elements, namely carbon and oxygen. The next important process is the CNO cycle [1−3], whose end product is the same as that of the pp1 chain. After He burning stops, depending on the stellar temperature and mass, the different successive phases of C, O, Ne, and Si burning take place until iron is produced. The charged particle reactions are the primary processes in nucleosynthesis till massA≈ 60 is reached, above which neutron capture through s (slow) and r (rapid) processes [1−3] becomes the dominant process.

It has been observed that among the heavier elements (A>60), there is a small fraction of proton-rich nuclei which are 10−1000 times less abundant than s- or r-nuclei and cannot be synthesized through these neutron capture processes because they are on the neutron deficient side of theβ-stability line. This group, consisting of approximately 35 nuclei between Se (Z=34) and Hg (Z=80), is synthesized by a different astrophysical process traditionally called thep-process orγ-process, and these nuclei are referred to as thep-nuclei [1−6]. Various studies indicate that the lighterpnuclei might be dominantly produced in the rpandνpprocesses and that the heavierpnuclei are synthesized through a sequence of photodisintegrations on the seeds ofr- ands-process nuclei [7]. Recent studies suggest that some of thepnuclei can also be produced in charged particle reactions [7].

In recent years, both theoretical and experimental investigations have been conducted to understand thep-process nucleosynthesis [5−7]. To solve the problem of the origin of thep-nuclei, it is essential to make use of both astrophysical and nuclear models as well as the available experimental information. Precise measurements enable constraining our models, and well tested nuclear models can provide an estimate of how reliable the measurements are. The experimental data are still inadequate because the production of these nuclei seems to require several processes.

The present study was undertaken with the intention of providing a useful guide to plan future experiments for measuring proton capture cross-sections on thep-nuclei using gamma-ray spectroscopy as a tool. For proper planning of experiments and careful analysis of their outcome, it is essential to have a clear knowledge of quantities such asQ-value, Coulomb barrier, Gamow energy, and decay properties of the system under study. It is also crucial to make a careful review of the experimental techniques and methods of analysis adopted by various researchers to extract useful and reliable data. This study is an attempt to summarize such information in a concise format to be readily available for scientists aiming to experimentally investigate proton capture cross-sections on thep-nuclei. The theoretical calculations were performed using TALYS code. These results, when compared with existing experimental data, help identify the systems which require reinvestigation or those for which no or scarce experimental data exist.

Nuclear reaction rates are essential ingredients for investigation of energy generation and nucleosynthesis processes in stars. Astrophysical reaction rates describing the change in the abundances due to nuclear reactions taking place in an astrophysical environment are functions of the densities of the interacting nuclei, their relative velocities, and reaction cross-sections [6,8]. The role of nuclear physics in understanding the process of nucleosynthesis and stellar evolution involves measurements or computations of fundamental quantities such as reaction cross-sections, nuclear masses, andβ-decay rates.

As mentioned in the previous section, the majority ofpnuclei are synthesized through a sequence of photodisintegration reactions. In principle, photodisintegration cross-sections can be experimentally determined by photon induced reaction studies [9,10]. However, in an experiment performed in laboratory, the target nucleus is always in the ground state, whereas in a stellar environment, thermally populated excited states significantly contribute to the reaction rate. It has been shown that the influence of thermal population is much less pronounced in capture reactions [11]. In addition, there is a lack of availability of appropriateγ-sources. Therefore, it is advantageous to measure the capture cross-sections; the photodisintegration rates can be derived by applying the principle of detailed balance [3]. The various important capture reactions to understand thep-process nucleosynthesis are (n,γ), (p,γ), (α,γ),etc. In the present study, we focused on the proton capture (p,γ) reaction.

The charged particle induced nuclear reactions take place within a narrow energy window called Gamow window $ (\Delta {E}_{0}) $ around the effective burning energy known as Gamow peakE₀, which lies well below the Coulomb energyE_c. The Gamow peak arises from folding the Coulomb penetration probability with the Maxwell-Boltzmann velocity distribution and is expressed as

where $ b=31.28{Z}_{1}{Z}_{2}{A}^{1/2} $ keV^1/2is the barrier penetrability. The corresponding expression for the Gamow window is

Ideally, nuclear astrophysics experiments should be performed within the energy region given byE₀± ΔE₀. The cross-section for charge particle reactions forE < E_c(Eis the center of mass energy for the reacting system) is given by

whereS(E) is the astrophysicalS-factor, which includes relevant information on nuclear physics. The factorηis known as the Sommerfield parameter and is expressed as $\eta \left(E\right)=\dfrac{{Z}_{1}{Z}_{2}{\rm e}^{2}}{{\textit ћ}v}$ , whereZ₁andZ₂are the atomic numbers of the interacting nuclei,υis their relative velocity, andћ= $ \dfrac{h}{2\pi } $ . The reaction rate for a pair of interacting nuclei is given by

In the above expressions,k_Bis the Boltzman constant, $\mu ={{m}_{1}{m}_{2}}/({{m}_{1}+{m}_{2}})$ is the reduced mass of the interacting particles, andTis the stellar temperature.

The importance of any particular nuclear reaction depends on the temperature and density of the specific stellar environment. Hence, each nuclear reaction must be treated as a unique process. The energy region of the chosen nuclear reaction process depends on the relevant stellar environment. The reaction cross-section is measured by the number of reactions taking place and can be determined using various methods. Although the most common method is based on the detection of the light outgoing particle, which is an in-beam method, it is seldom adopted [12] for measuring particle capture cross-sections of astrophysical importance because reaction cross-sections are extremely small and difficult to separate from the beam induced background. The other possibility is the determination of the number of heavy residual nuclei, which requires a special experimental technique based on combining a recoil mass separator and inverse kinematics [13]. The third method is often conducted when the heavy residual nucleus is radioactive. This is the activation method [14], in which the cross-section is determined by detecting the decay or activity from the residual nucleus.

Measuring cross-sections in the astrophysically relevant region (Gamow window) is often impossible for various reasons. In many cases, low energy beams are not available. Even if it is possible to achieve a beam at the required energy, the cross-sections can be so small that it is generally impossible to separate the targeted data from the natural and cosmic-ray induced background. Hence, experiments are often performed at a higher energy and extrapolation provides the cross-section at the relevant astrophysical energies. In a simple case, the cross-section drops drastically with energy without exhibiting any significant structures. In this scenario, comparatively few points will be enough to constrain theoretical cross-section calculations. Sometimes, the extrapolation process becomes complicated owing to the presence of resonances, and the Breit-Wigner [15] formula is used to extrapolate the cross-sections to the region where no experimental data exist. The present study considers only non-resonant systems.

This study is an attempt to provide guidance for future experimental studies involvingp-nuclei. Neutron, proton, and alpha induced reactions play key roles in many astrophysical processes including thep-process nucleosynthesis. Very few charged–particle reactions have been experimentally investigated above the iron region. In general, investigations of gamma rays emitted from the radioactive nuclide have a very wide application scope for cross-section measurements. This is owing to the fact that gamma rays emitted from most radionuclides have a wide range of energies (40−1000 keV) with relatively high penetrating power, thereby ensuring minimal losses by absorption in a sample during measurement. This property, along with recent developments in high-resolution and high-efficiency gamma-ray detectors, makes gamma-ray spectroscopy a powerful technique for nuclear cross-section measurements.

The present study includes a short review of experimental studies on the cross-sections of proton captures onp-nuclei through detection of gamma rays. TALYS calculations were performed to obtain theoretical estimates of these cross-section values (discussed in Sec. III.A). The current status of the corresponding experimental studies was reviewed following those reported in the KADoNis database [16]. These experimental results were compared with theoretical predictions from the TALYS calculations perfomed.

The values of the Coulomb barrier (E_c),Q-values, Gamow peak (E₀), and Gamow window (ΔE₀) are represented against the corresponding mass numbers inFig. 1(a)−(c)). The points representingE_chave been joined by lines to facilitate visual analysis. The Coulomb barrier was obtained from the fusion evaporation code PACE4 [17]. TheQ-values were obtained from the NNDC website [18]. The values of the Gamow peaks and Gamow windows were calculated using Eqs. (1) and (2), respectively. The value ofTwas set to 3×10⁻⁹K (T9 =3) to calculate the Gamow peak and Gamow window.

Figure 1.Plots of Coulomb barrier (E_c),Q-values, Gamow peak (E₀), and Gamow window (ΔE₀) against mass number.

The knowledge of lifetime values of the daughter nucleus is essential to choose a proper method for detection of gamma rays. For example, if the nucleus produced after proton capture has a stable ground state, then the in-beam technique is the only possible investigation method. However, if the ground state has a moderate half-life, activation analysis is the preferred investigation method. The values of the abundances or half-lives (T_1/2) of the target nuclei [19], half-lives (T_1/2) of the ground state of the daughter nucleus following proton capture, and a few significant gamma transitions of the nucleus formed following the subsequent decay (β, EC, IT) are listed inTable 1. These values were obtained from the NNDC website [20]. Some experimental parameters adopted by various authors are listed inTable 2. The references corresponding to the experimental studies reported in the literature are included inTable 1.

In the present study, we focused on previous studies where stablep-nuclei were bombarded with a proton beam and the capture cross-sections were measured by detecting the decaying gamma rays. As seen fromTable 1, the abundances of thesep-nuclei are considerably low with the exception of some of them, such as Mo, Ru, In, and Sm. In a proton capture reaction experiment, in which thep-nuclei are being used as the target, low abundance results in very low yield, necessitating high beam current and prolonged activation to obtain conceivable statistics for deducing the reaction cross-sections with considerable certainity. The half lives of the daughter nuclei are small (of the order of minutes or 1−2 hrs.) in most cases, making the detection process very difficult or even impossible. Systems with comparatively large half lives for the daughter nuclei,viz.⁹⁸Ru,¹⁰⁸Cd,¹²⁶Xe,¹³²Ba,¹³⁸Ce,¹⁴⁴Sm,¹⁵²Gd,¹⁶⁴Er,¹⁶⁸Yb,¹⁷⁴Hf and¹⁸⁰Ta, can be more easily studied using the activation technique. The nuclei, which exhibit much larger half lives (of the order of many days or years), are generally studied using the in-beam technique. The fourth column ofTable 1lists the gamma rays to be detected for measuring the reaction cross-sections. The intensities of very low energy gamma rays, which cannot be detected owing to experimental limitations, can be deduced by measuring intensities of the higher energy transitions (in parenthesis) leading to the low energy lines after correcting for the corresponding branching transitions.

FromTable 2, we observe that the majority of the systems were experimentally studied using the activation method and a single HPGe detector. Both natural and enriched targets were used either as thick, self-supporting or thin, backed. The most common backing material used is Al. The use of Al as backing material, having much lower Z than the target material, helps avoid interferences from the events occurring from the interaction between the projectile and backing. The beam current used in all the experiments was reasonably high to achieve sufficient yield. The systemp+⁹²Mo was studied in both activation and in-beam methods. For in-beam studies [12], an enriched self-supported target and 13 HPGe detectors were used, whereas for activation measurements, [23] backed target and a single HPGe detector were used. The cross-section results from in-beam studies [12] were compared with earlier activation measurements [23] and they were found to be in reasonable agreement, except for a few discrepancies.

Figures 1(a) and (b) represent the variation of the Coulomb barrier andQ-value of the reactions against mass numbers of thep-nuclei. The variation of Gamow peaks with corresponding mass numbers are represented inFig. 1(c), in which the Gamow window is denoted as error bars. Note fromFig. 1(a) that, as expected, the Coulomb barrier increases with the mass number. TheQ-value (Fig. 1(b)) was found to be within the range of 3−5 MeV with the exception of¹¹³In,¹³⁸La, and¹⁸⁰Ta, for which the value is within ~7−8 MeV. The Gamow window was found to be within the range of ~0.5 to 7.5 MeV.

TALYS is a computer code system for analysis and prediction of nuclear reactions [33]. It is a nuclear physics tool that can be used for the analysis of nuclear reaction experiments, either in a default mode when no measurements are available, or after finely tuning the adjustable parameters of the various reaction models using available experimental data. Rather than providing a detailed description of only one or a few reaction channels, TALYS outputs a simultaneous prediction of many nuclear reaction channels. TALYS is meant for the analysis of data in the energy range of 1 keV−200 MeV. The lower limit is the energy above the resolved resonance range, which is not necessarily exactly 1 keV.

In this study, TALYS calculations were performed to obtain theoretical estimates of the proton-capture cross-section values. The results are represented against the proton energy inFigs. 2and3. The corresponding experimental values obtained from the KaDONiS [16] database are included for comparison inFig. 2. The corresponding values given in the TENDL tabulation [34] are also included. TENDL is the commonly referred nuclear data library that provides the output of the TALYS nuclear model code system. It was reported by the authors [33] that for protons, libraries produced by default TALYS calculations perform reasonably well. The present TALYS calculations were performed with the default parameters [33]. TALYS calculations were also performed for all the otherp-nuclei for which no experimental data have been reported. These results are represented inFig. 3. The plots also include the corresponding results from TENDL tabulation.

Figure 2.Plots of the proton capture cross-section values vs. energy in the Gamow region. Experimental values (solid star), TALYS calculation results (open circle), and results from TENDL tabulation (open triangle) are compared. The theoretical values are connected by straight lines to facilitate visual analysis.

Figure 3.Plots of the cross-section values from TALYS calculation (open circle) and TENDL tabulation (open triangle) for the systems for which no experimental data have been reported. The theoretical values are connected by straight lines to facilitate visual analysis.

As mentioned above, TALYS can generate nuclear data for all open reaction channels after finely tuning the adjustable parameters of the various reaction models using available experimental data. TALYS incorporates a completely integrated optical model and recent optical model parameterizations for many nuclei. The central assumption of this optical model is that the complicated interaction between an incident particle and a nucleus can be represented by a complex mean-field potential, which divides the reaction flux into two parts: one representing the shape elastic scattering and the other representing all competing non-elastic channels. The phenomenological OMP for nucleon-nucleus scattering,U, is defined as [33]

whereV_V,SOandW_V,_D,SOare the real and imaginary components of the volume-central (V), surface central (D),and spin-orbit (SO) potentials, respectively.Eis the energy of the incident particle in MeV in the laboratory frame. All components are separated in energy-dependent parts (VV, WV, WD, VSO,andWSO) and energy–independent radial partsf[33]. The form factorf(r, Ri, ai) is a Woods-Saxon shape expressed as

The default optical model potentials (OMPs) used in TALYS are the local and global parameterizations of Koning and Delaroche [35]. Gamma-ray transmission coefficients are important for radiative capture reactions involving gamma emission. These coefficients depend on the gamma–ray energies and gamma-ray strength functions (GSF) [33].

In the present study, we performed a few calculations by changing the OMPs,a_vandr_v,as well as the GSF for three nuclei, namely⁹²Mo,¹²⁰Te, and¹⁵⁶Dy, to obtain a preliminary idea of how they affect the cross-section values. Ther_vvalue was varied within the range from approximately 0.12 to 0.15; and the corresponding default value is approximately 1.2. Thea_vvalue was changed within the range from approximately 0.06 to 0.73; the corresponding default value is approximately 0.67. The Gamma-strength normalization factors were varied from 0.1 to 1.1. The corresponding plots are shown inFig. 4. Note from this figure that, within the Gamow energy region (2−5 MeV), the cross-section values apparently do not change significantly with GSF,a_v, andr_v. The variation becomes more pronounced as we move to higher energies. These data are not sufficient to make any conclusive comments about the dependence of the cross-section values on OMPs and GSFs. This is work in progress towards a more elaborate and detailed study for a potential separate publication.

Figure 4.Plots of the cross-section values from TALYS calculations with different values ofa_v,r_v, and GSF for⁹²Mo,¹²⁰Te, and¹⁵⁶Dy.

The present study aims at providing a guide to study the p-nuclei by presenting a short review of the present status of the investigations in this field and estimates of radiative proton capture cross-sections obtained from TALYS calculations. It was observed that in the majority of the experimental investigations, a single HPGe detector was used to detect the gamma rays. As mentioned earlier, and according toFig. 2, the proton capture cross-sections are generally very small. Hence, more powerful detectors such as Clover can be used to improve the detection efficiency.Table 2shows that natural targets were used in most experiments. The presence of isotopes other than the one of primary interest gives rise to events that often eclipse the event of interest. To improve the relative yield of the gamma rays of interest, experiments may be repeated with enriched targets in systems where previous investigations were performed using natural targets. It is evident from the present review that there are very fewp-nuclei above a massA~100, for which experimental cross-section data have been reported. There is a notable demand of experimental investigations on p-nuclei. Most of the systems were investigated through the activation technique. For these systems, where reliable data exist from activation studies, in-beam measurements may be performed. This will help study those systems for which activation studies are not viable and identify and correct for the beam induced background and angular distribution effects, which are major sources of errors in in-beam investigations.

The TALYS calculations were performed to obtain theoretical estimates of the proton capture cross-section values on thep-nuclei. These values were compared with the corresponding experimental data reported in the literature and data from the TENDL tabulation. Although the experimental data seem to agree well with the theoretical estimates within the Gamow region, we should keep in mind that the cross-section values in this region are extremely small, approximately few μb or even smaller. Hence, even very little differences between experimental and theoretical values cannot be ignored. Note that both theoretical and experimental cross-section values show a similar nature of rise and fall with the change in the incident energy. As we move to higher energy, the differences between experimental and theoretical values appear to become more pronounced. All the aforementioned calculations were performed using default parameter values. Preliminary results are presented, depicting the behaviour of the cross-section values over a short range of few optical model parameters and gamma strength functions. This is work in progress; calculations over a wider range for all the parameters and allp-nuclei are expected to provide sufficient predictive power to the various nuclear models and give an indication of the reliability of the measurements.