High-resolution radioactive beam study of the 26Al(d,p\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^{26}\hbox {Al}(d,p$$\end{document}) reaction and measurements of single-particle spectroscopic factors

We present a detailed comparison of shell model calculations with inverse kinematic transfer reaction data, obtained using a radioactive beam. Experimentally extracted spectroscopic factors from the 26Al(d,p)27Al\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^{26}\hbox {Al}(d,p)^{27}\hbox {Al}$$\end{document} reaction for both even and odd parity states are found to be exceptionally well reproduced by the shell model and a high level of consistency is observed between bound isobaric analog states in 27Al\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^{27}\hbox {Al}$$\end{document} and 27Si\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^{27}\hbox {Si}$$\end{document}, populated via (d, p) and (d, n) transfer, respectively. Furthermore, an evaluation of key resonances in the astrophysical 26Al(p,γ)27Si\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^{26}\hbox {Al}(p,\gamma )^{27}\hbox {Si}$$\end{document} reaction indicates that shell model calculations provide relatively accurate predictions for the existence of strong resonances and mirror nucleus comparisons appear to hold exceptionally well for proton-unbound levels. Consequently, we expect that the utilization of both techniques will likely be a very effective tool in the investigation of stellar processes outside the current reach of experiment.

In analogy with electrons in atoms, certain numbers of protons and neutrons in nuclei lead to particularly stable configurations. These so-called "magic" numbers were first reproduced in their entirety, by Goeppert-Mayer, Jensen and Suess, in 1949 [1,2], and established the nuclear shell model as a bedrock of nuclear physics research. Since then, the shell model description of the quantum many-body problem has been developed to become the principal mechanism for understanding nuclear structure across the chart of isotopes [3]. In particular, by considering only those particles that exist outside of an "inert" doubly-magic core to be active, shell model calculations have been able to act as powerful tools for predicting the spins, parities and nuclear matrix elea e-mail: g.lotay@surrey.ac.uk ments of excited states in the sd shell [4]. However, in order to extend and explicate the predictive power of the shell model for nuclei far from stability, there is a need to perform detailed studies of shell model wave functions up to regions of high excitation energy and weak binding.
Single-particle spectroscopic factors, C 2 S, obtained from transfer reactions provide one of the most fundamental tests of wave functions incorporated in the nuclear shell model. Specifically, they quantify the occupancy of single-particle orbits in a nucleus and, as such, represent an essential check of model spaces used in current calculations. Detailed, highresolution measurements of spectroscopic factors, and precise comparisons with shell model predictions, have largely involved reactions with stable target nuclei [5]. In this Letter, we present such an analysis for a study of the (d, p) reaction using a beam of radioactive 26 Al nuclei in inverse kinematics. This represents a benchmark for comprehensive, highresolution transfer reaction studies using radioactive beams and, as such, provides key information for the broader development of worldwide initiatives in this area [6][7][8][9][10][11]. Spectroscopic factors are reported for 17 excited states and excellent agreement is obtained with nuclear shell model wave function predictions. Furthermore, we explore the robustness of the mirror symmetry in the T = 1/2, A = 27 system, for the first time, through a comparison of the present data with more limited information obtained for analog levels in 27 Si via 26 Al(d, n) transfer [12]. Isospin symmetry is observed to hold extremely well up to high excitation energies. Moreover, shell model calculations and transfer reaction estimates of resonance strengths for the 26 Al( p, γ ) 27 Si reaction, which destroys the cosmic γ -ray emitter 26 Al in stars [13], are found The experimental setup used for this study has already been reported in an earlier paper [14] and, as such, we will provide a brief summary of the key features here. An intense, ∼ 1 pnA beam of radioactive 26 Al at 6 A MeV was used to bombard a thin ∼ 60 µg/cm 2 thick (CD 2 ) n target in order to populate excited states in 27 Al via the 26 Al(d, p) transfer reaction-it is expected that the population of excited states is purely via the ground state component of the beam (the ground to isomeric state ratio was measured to be ∼ 17000:1). Resulting protons were detected with three MSL type S2 silicon strip detectors [16], placed upstream of the target position, covering an angular range θ C M ∼ 0.5 • −24 • (although it should be noted that only the most strongly populated states could be analysed for angles >12 • ). Using such a configuration allowed for the state of the art in resolution performance for an inverse kinematic transfer reaction study using a radioactive beam to be achieved (∼40 keV FWHM-see Fig. 1 of Ref. [14]). Figure 1 illustrates the angular distributions obtained for excited states observed in the current study. Levels in 27 Al [15] corresponding to low orbital angular momentum, , transfers are observed to be selectively populated at the forward center-of mass angular range covered in the present experimental set-up.
For the determination of spectroscopic factors, C 2 S, measured differential cross sections were compared with theoretical distributions obtained from adiabatic distorted wave approximation (ADWA) calculations using the code TWOFNR [17]. Here, the deuteron wave function of the Table 1 Properties of excited states in 27 Al in comparison with shell model calculations [4] and mirror states in 27 Si. Also included are spectroscopic factors for excited levels in 27 Si obtained from a previous (d, n) reaction study [12]. Excitation energies for states in 27 Al and 27 Si are adopted from Ref. [15] and excitation energies listed for SM are for states in 27 Si Argonne AV18 np interaction [18], as well as the Koning-Delaroche global optical model parameterization [19], were used to calculate the distorting potential [20]. Radii were obtained by the Hartree-Fock (HF) method of Ref. [21], except in the case HF-unbound, p-wave orbitals, for which radius and diffuseness parameters of 1.25 and 0.65 fm, respectively, were used. Table 1 presents a summary of extracted spectroscopic factors for excited levels in 27 Al, together with a comparison to shell model calculations and mirror analogs in 27 Si populated via (d, n) transfer [12]. The information obtained for = 0 and = 2 transfers is also shown in graphical form in Fig. 2. Shell model calculations of spectroscopic factors for positive parity states were performed using the USDB-cdpn interaction [4], in which cdpn refers to the addition of the Coulomb, charge-dependent and charge asymmetric nuclear Hamiltonian obtained by Ormand and Brown in a proton-neutron basis [22]. For negative par-ity states, we adopt the shell model calculations of Ref. [12] that used the 1hω basis introduced by Brown [23] to allow for the excitation of one nucleon from 0 p to 1s-0d or the excitation of one nucleon from 1s-0d to 0 p-1 f . In considering the observed even-parity states, it is clear from Table 1 and Fig. 2 that there is striking agreement between spectroscopic factors extracted from the 26 Al(d, p) reaction and shell model calculations (to within a factor ∼ 2) up to high excitation energy. Somewhat surprisingly, very good agreement between experiment and shell model predictions is obtained even for relatively small values down to C 2 S ∼ 0.01. The only significant systematic discrepancy found is for some states (e.g. E x = 3004 and 5500 keV), where experiment gives a significantly larger = 2 strength than predicted by the shell model, as illustrated in Fig. 2 (b). However, the = 0 spectroscopic factors for these states are still in excellent agreement with theoretical predictions.  A possible explanation for the rather impressive predictive power of the shell model may relate to the nature of the 5 + ground state of 26 Al. In particular, the addition of a neutron, via low-transfers, to this π(1d 5/2 ) −1 ⊗ ν(1d 5/2 ) −1 shell model configuration state, will result in relatively pure, high-spin states in the residual nucleus, 27 Al. These states are likely to exhibit a strong single-particle character and, as such, may be well represented in the shell model. Furthermore, while the present (d, p) reaction study is the first experimental investigation of neutron spectroscopic factors in 27 Al, other known properties such as excitation energies and spin-parity assignments will have been used as input data to generate the sd-shell model interaction.
Examining negative parity states populated in 26 Al(d, p) transfer, we find that only the 7948 and 7997 keV levels have angular distributions characteristic of odd-transfers. The 7997 keV excited state in 27 Al can be described by pure = 1 transfer with C 2 S = 0.04(1), in excellent agreement with the nuclear shell model and supporting an assignment of 9/2 − for this level [24]. Similarly, the angular distribution of the 11/2 − , 7948 keV excited state can be well-fitted by pure = 1 transfer with C 2 S = 0.04 (1).
For the majority of states, there is very good agreement for spectroscopic factors between mirror levels in 27 Al and 27 Si and with shell model calculations. In particular, several bound excited states in 27 Si at 5547, 6734 and 7129 keV, as well as a proton-unbound level at 7739 keV, which were strongly populated in the (d, n) reaction [12], are found to have spectroscopic factors in almost complete agreement with their mirror analogs in 27 Al at 5667, 6948, 7289 and 7997 keV, respectively. The one exception to this observed agreement, between mirror states, is the proton-unbound level in 27 Si at 7652 keV. The previously reported C 2 S ( =1) value of 0.22(5) [12] is not consistent with the presently extracted neutron spectroscopic factor of the mirror analog at 7948 keV in 27 Al. However, in Ref. [12], spectroscopic factors were obtained from an angle-integrated measurement of the cross section, which does not allow for the discrimination between different -components of the wave function. Shell model calculations predict an additional, strong C 2 S ( =3) = 0.48 component for the 7652 keV state and, in an earlier ( 3 He, d) study, the angular distribution for this level can be almost entirely fit with = 3 transfer [28]. Intriguingly, a slightly better fit to the present data for the mirror state in 27 Al at 7948 keV can also be achieved by including a large = 3 component. However, we draw attention to the fact that the current work is not very sensitive to such -transfers, due to the limited angular range, and we refrain from making any definitive statements about = 3 spectroscopic factors.
Considering states above the proton-emission threshold in 27 Si at 7643.25(16) keV [29], a key application of the present study relates to nuclear astrophysics. In particular, shell model calculations and information on mirror states can  26 Al + p resonances determined from different methodologies. Total widths have been determined from lifetimes reported in Ref. [24], unless otherwise indicated, and resonance strengths for the (d, p) reaction and shell model have been evaluated using spectroscopic factors presented in Table 1. For states with multiple -transfers, only the lowest -value has any influence on the overall resonance strength. Particle widths and resonance strengths are given in meV  [24] is incompatible with the predicted proton width. As such, a lower limit of 1 fs has been assumed for this state b Taken as the average of Refs. [26,27] c Taken as the average of Refs. [25,26] be used to determine the properties of experimentally inaccessible astrophysical resonances in ( p, γ ) capture reactions, as separately illustrated in Refs. [30][31][32] and Refs. [14,33], respectively. Here, high-lying excited levels in 27 Al represent analogs of proton-unbound resonant states in 27 Si that dominate the 26 Al( p, γ ) reaction in explosive stellar phenomena. This reaction governs the destruction of the cosmic γ -ray emitting nucleus 26 Al and, as such, directly affects a distinctive astronomical observable [13]. A subset of states in 27 Al of relevance for this reaction have already been considered in earlier work by our collaboration [14]. Here, a summary of 26 Al( p, γ ) resonance strengths obtained from different methodologies is presented in Table 2. It should be noted that the 11/2 − resonance at 189 keV was previously reported as having C 2 S ( =1) = 0.14(3) [14]. However, it has since been determined that incorrect nodes in TWOFNR were used in the earlier analysis of negative parity levels [14] (transfer to the 0 p orbital was used instead of 1 p). This does not affect any of the conclusions made in Ref. [14] and brings the extracted spectroscopic factor into more consistent agreement with shell model calculations. We find that resonance strengths determined from the current (d, p) reaction data and shell model calculations are in excellent agreement with direct measurements, highlighting the usefulness of indirect studies for the evaluation of stellar reaction rates. Specifically, we have definitively shown that, for three key resonances in the 26 Al( p, γ ) reaction, neutron spectroscopic factors in 27 Al may be successfully used to obtain the proton partial widths of particle-unbound levels in the mirror nucleus 27 Si. It may seem somewhat surprising that isospin symmetry holds for unbound levels in the T = 1/2, A = 27 system. However, it should be noted that, in this case, the states of astrophysical interest lie very close to the particle-emission threshold and the height of Coulomb barrier is such that they are strongly shielded against proton decay. Consequently, they act as though they are effectively bound and both the shell model and the (d, p) data are able to accurately reproduce their properties. A limitation of the mirror analysis technique relates to proton-unbound states with Γ p > Γ γ . Here, the lifetime of the excited level must be known precisely in order to accurately estimate the resonance strength. Furthermore, for shell model calculations, both the energy and the level ordering of all resonant states must be determined experimentally, prior to an evaluation of the stellar reaction rate. This is illustrated in Table 1, in which shell model energies can differ from experimental values by up to ∼500 keV.
In summary, a detailed spectroscopic study of the 26 Al(d, p) transfer reaction with a radioactive beam has been used to perform a precise test of the nuclear shell model. Extracted spectroscopic factors are found to be exceptionally well reproduced by shell model calculations, even for C 2 S values as small as 0.01, and a comparison with the mirror nucleus 27 Si suggests strong isospin symmetry in the T = 1/2, A = 27 system. Furthermore, 26 Al + p resonance strengths determined from neutron spectroscopic factors and shell model calculations are found to be in excellent agreement with direct measurements [25][26][27]. This highlights the significant accuracy of shell model predictions and opens up fascinating opportunities for investigating astrophysical reactions outside the reach of current experimental technology. However, it is possible that the T = 1/2, A = 27 system represents a special case. In particular, the preferential population of relatively pure configuration, high-spin states from both proton and neutron transfer on the 5 + ground state of 26 Al, could be viewed as rather exotic. Consequently, we strongly encourage further investigation to elucidate how general the present results are across the chart of the nuclides. For example, in the specific case of negative parity states in the T = 1/2, A = 31 system, values of C 2 S approximately 10 times smaller than those predicted by the shell model have recently been reported for proton-unbound levels in 31 S [34].