s-Processing in Asymptotic Giant Branch Stars in the Light of Revised Neutron-Capture Cross Sections

: Current AGB stellar models provide an adequate description of the s-process nucleosynthesis that occurs. Nonetheless, they still suffer from many uncertainties related to the modeling of the 13 C pocket formation and the adopted nuclear reaction rates. For many important s-process isotopes, a best set of neutron-capture cross sections was recently re-evaluated. Using stellar models prescribing that the 13 C pocket is a by-product of magnetic-buoyancy-induced mixing phenomena, s-process calculations were carried out with this database. Signiﬁcant effects are found for a few s-only and branching point isotopes, pointing out the need for improved neutron-capture cross section measurements at low energy.


Introduction
Asymptotic giant branch (AGB) stars are major production sources for heavy elements in the Universe. In particular, they were recognized to be responsible for the nucleosynthesis of the main and strong components (nuclei heavier than Sr) of the solar s-process (slow neutron-capture process) distribution (see, e.g., Busso et al. [1] for a review). AGB stars' interior consists of a carbon-oxygen core surrounded by a thin He-rich shell (He-intershell) and an extended H-rich envelope. These stars experience periodic He-shell flashes, called thermal pulses (TPs), inducing convective motions throughout the He-intershell that mix the products of the 3α reaction. The large amount of energy released during the TP also induces the expansion and cooling of the intershell region; as a consequence, the H-burning shell, previously active at the base of the envelope, dies down. After that, the convective envelope penetrates the He-intershell underlying region and brings freshly synthesized materials to the surface. This phenomenon is called third dredge-up (TDU). During a TDU, hydrogen is partially mixed from the convective envelope into the 12 C-rich Heintershell, where it is consumed through the 12 C(p, γ) 13 N(β + ) 13 C chain, thus forming a 13 C-enriched layer, the so-called 13 C pocket. Such a 13 C burns in radiative conditions, when the temperature attains ∼90 MK, via the 13 C(α, n) 16 O reaction during the long interpulse phase separating two subsequent TPs [2]. The 13 C(α, n) 16 O reaction is the main source through which low-mass AGB stars release neutrons and produce s-elements (see, e.g., Cristallo et al. [3]). An additional neutron burst is driven by the 22 Ne(α, n) 25 Mg reaction that is only marginally triggered at the base of the convective TP, due to the moderate temperatures (T 300 MK).
To date, the mechanism responsible for the creation of the 13 C pocket is far from being well known. Several mixing processes have been proposed over the last years, involving convective overshoot [4], rotation-induced mixing [5][6][7], opacity-induced overshoot [8][9][10], or mixing induced by internal gravity waves [11][12][13]. More recently, the suggestion that stellar magnetic activity might be responsible for the formation of the 13 C pocket through mixing induced by magnetic buoyancy has been proposed [14,15]. Post-process calculations of such a 13 C reservoir have shown to be able to reproduce the distribution of s-elements in the solar main component [15], heavy-element isotopic compositions of presolar grains [16], and most of n-capture elements abundances observed in Ba-stars and post-AGB stars [17]. These studies have been confirmed by numerical simulations of the formation of a magnetically-buoyancy-induced 13 C pocket in a new series of FRUITY stellar evolutionary models [18]. New FRUITY Magnetic models have also been found to be successful in reproducing the observed fluorine vs. average s-element enhancements in intrinsic carbon and extrinsic stars [19], and in a Galactic chemical evolution context, the observed trends of yttrium abundance in the inner part of the Galactic disk [20].
Besides the complexities associated with the modeling of the 13 C pocket formation, AGB s-process predictions also show large sensitivity to the adopted (n, γ) reaction rates. To date, the vast majority of experimentally measured neutron-capture cross sections are known with a precision of a few percent (see, e.g., Käppeler et al. [21]). For detailed AGB s-process nucleosynthesis simulations, Maxwellian averaged cross sections (MACS) ranging from thermal energies of about 8 keV, proper of the 13 C pocket radiative burning, to about 23-25 keV, during a TP, have to be considered. To cover the whole energy range, energy-differential cross sections are needed in the neutron energy region between about 0.1 keV and 1 MeV [21,22]. When experimental data in this range is missing, evaluated cross sections from data libraries have to be taken into account. In addition, many of the available experimental measurements, based on activation and time-of-flight (TOF) techniques, were performed relative to gold cross section as a standard. Recently, TOF measurements of the energy-dependent gold cross section [23,24] found a ∼5% higher value than the recommended cross section used as a standard for astrophysical applications [25]. The adoption of the new recommended value for the 197 Au(n, γ) 198 Au have been studied for several TOF measurements in Reifarth et al. [22], in which several measurements carried out relative to this standard were re-examined. For these, a corresponding set of new recommended MACS was also provided. The stellar neutron cross section database "ASTrophysical Rate and rAw data Library" (ASTRAL) presents a list of these re-evaluated experimental MACS for energies between kT = 1 keV and 500 keV. The current version "v0" includes 64 new recommended cross sections (see Reifarth et al. [22] for more details).
In this work, the recommended MACS from the ASTRAL v0 database are used to investigate the impact on the s-process nucleosynthesis occurring in low-mass AGB stars, by computing selected stellar models. The results are then compared with those obtained by the previously adopted set of (n, γ) cross sections and with isotopic ratios of heavy elements measured in presolar SiC grains.

Stellar Models
Stellar models presented in this work have been computed with the FUNS (FUll Network Stellar) evolutionary code; see Straniero et al. [26] and references therein). The adopted network includes almost 500 isotopes (from H to Bi) and more than 800 nuclear reactions. Low-temperature C-enhanced molecular opacities computed by means of the AESOPUS tool [27] are used to take into account the variation of the envelope chemical composition determined by the carbon dredge-up during the TP-AGB phase [28]. A scaled-solar composition as provided by Lodders [29] is adopted. Accordingly, a mixinglength parameter α m.l. = 1.86, has been derived by computing a standard solar model (see Vescovi et al. [30] for more details on the followed procedure). For the mass-loss rate, we adopted a Reimers' formula with η = 0.4 for the pre-AGB evolution, while for the AGB phase, we used the rate as derived by Abia et al. [31]. In Vescovi et al. [18], mixing triggered by magnetic buoyancy was implemented in the FUNS code starting from the formalism developed by Nucci and Busso [32]. In brief, during a TDU, the peculiar density profile of the radiative layers below the convective envelope guarantees that if magnetic flux tubes are there formed, they are subject to buoyancy phenomena and can induce a stable mass circulation. In particular, the formation and buoyant rise of magnetic flux tubes in the He-intershell of an AGB star may induce, for mass conservation, the partial mixing of hydrogen necessary for the development of the 13 C pocket. The efficiency of such mixing relies on the magnitude of the toroidal field necessary for the occurrence of magnetic buoyant instabilities and the initial velocity of magnetic flux tubes. Vescovi et al. [18] found that close-to-solar metallicity AGB models computed with a single configuration for the toroidal field strength (B ϕ = 5 × 10 4 G) and the initial buoyant velocity (u p = 5 × 10 −5 cm s −1 ), are able to account for the majority of the heavy-element isotope ratios measured in presolar silicon carbide (SiC) grains (see Vescovi et al. [18] for more details). In all the models presented in this work, we adopted the same configuration choice.
In order to assess the impact of the new (n, γ) cross sections evaluation on the sprocess, we computed three models of an AGB star with mass M = 2 M and metallicity Z = 0.01, 0.0167 (≡ Z ), 0.02, adopting two different sets of n-capture cross sections. In the reference models (hereinafter REF) we adopted the same nuclear network used in Vescovi et al. [18], while in the new models (hereinafter NEW) we adopted for 64 different cross sections the recent re-evaluation proposed by Reifarth et al. [22] (ASTRAL v0 database), where a detailed list of isotopes can be found.

Results and Discussion
In Figure 1  The NEW model shows small variations ( 5%) for the vast majority of the isotopes. Differences larger than ∼10% are obtained for 122 Te, 134 Ba, 136 Ba, and 154 Gd, whose production has been decreased mostly due to an increased MACS of the corresponding (n, γ) cross section (see Table 1). All of these isotopes are of pure s-process origin (s-only), being shielded against the β-decay chains from the r-process by stable isobars. The production of the s-dominated 137 Ba isotope is found to decrease by ∼20%, while the production of the short-lived isotope 182 Hf is enhanced by about 10%. The abundance of 122 Te is potentially affected by the β-decay of the branch point isotope 122 Sb. However, at TP temperatures, its half-life is of the order of a few hours, [37] so that the decay channel largely dominates over the neutron-capture rate. The abundance variation of 122 Te is therefore ascribed to the enhanced MACS (+13% at 30 keV; see Table 1). The production of the two s-only isotopes 134 Ba and 136 Ba occurs both during the 13 C pocket and the TP phases. Despite the fact the both these isotopes are underproduced in the NEW model with respect to the REF model, the 134 Ba/ 136 Ba ratio is however not modified, since it is largely sensitive to the branch at 134 Cs, in particular to its β − -decay rate which decreases up to two orders of magnitude at 300 MK [37]. The 137 Ba/ 136 Ba ratio instead decreases by ∼12%. The final abundance of 154 Gd is determined by the competition between neutron capture on 154 Gd and β-decay rate of the close unstable isotope 154 Eu (see also Mazzone et al. [34]); as a whole, the decrease of the 154 Gd is slightly lower than the change of the neutron-capture cross sections (+24% at 30 keV). The production of the short-lived 182 Hf (t 1/2 = 8.9 Myr) is regulated by the branch at 181 Hf. According to Takahashi and Yokoi [37], its half-life strongly reduces during TPs, passing from a terrestrial value of 42.39 d to 1.26 d at 300 MK. This causes the s-path to proceed towards 182 W and the 182 Hf production to be low. However, the radiogenic contribution of 182 Hf occurring at the end of the TP-AGB phase is important to explain the solar abundance of 182 W. Present AGB estimations for the s-process main component can account for 65-70% of solar 182 W [17,38], while its r-process contribution is well justified by the Galactic enrichment of r-process elements [39]. However, Lugaro et al. [40] have pointed out that the present AGB contributions to 182 Hf and 182 W may have so far been underestimated. Based on the work of Bondarenko et al. [41], Lugaro et al. [40] suggested that the β-decay rate in stellar conditions remains pretty unchanged with respect to its terrestrial value, thus allowing an increased feeding of 182 Hf and, in turn, of 182 W after the TP-AGB phase. In this sense, further experimental evidence is demanding. In our computations, we cautiously adopt the decay rate given by Takahashi and Yokoi [37] for 181 Hf. By using the new ASTRAL v0 values for (n, γ) cross section in our calculations, the 182 Hf is increased by ∼10%. This is due to the enhanced MACS for hafnium isotopes, whose net effect is to increment the neutron density and thus the neutron-capture strength of the branching point at the unstable 181 Hf. This result is of relevance for the origin of 182 Hf in the early Solar System (see, e.g., Wasserburg et al. [42] for a review), in particular for the estimation of its s-and r-process contributions [39,43].
Analogous results are obtained for the M = 2 M Z = Z AGB model (see Figure 2). In this case, because of the decreased amount of iron seed in comparison to the number of neutrons produced by the 13 C burning, a higher production of heavy s-process elements (Ba-La-Ce-Nd-Sm) is obtained, thus magnifying the effects of the revised cross sections on isotopes belonging to the second s-process peak. Noteworthy variations ( 10%) are in fact found for 142 Nd. 142 Nd is a neutron-magic nucleus (N = 82), whose solar abundance is almost entirely due to its s-process component, since 142 Ce shields it against the r-process. During the s-process nucleosynthesis, the 142 Nd abundance is marginally affected by branching in the neutron-capture path corresponding to 141 Ce and 142 Pr. Most of 142 Nd is synthesized during the radiative burning of the 13 C pocket when the s-path proceeds close to the neutron-magic nuclei. The new MACS is smaller than the previous estimation by [33] of ∼14% at thermal energies of 8 keV, typical of the 13 C radiative burning [44], while the value at 30 keV is almost the same. Actually, because of the presence of many resonances in the low-energy region for this isotope, the adoption of a specific evaluated cross section available in data libraries affects the computation of the MACS at low thermal energy. Therefore, the discrepancy between the two evaluations derives from the different library adopted (see Reifarth   The above results are confirmed by the M = 2 M Z = 0.01 NEW model (see Figure 3), for which the higher neutron-to-seed ratio and temperatures attained during TPs cause a significant difference also for the 176 Hf abundance. 176 Hf and its parent 176 Lu are two s-only isotopes. 176 Lu was originally considered as a possible nuclear chronometer for the age of s-elements because of its long half-life. However, at temperatures typical of the s-process, it exhibits a quite strong dependency on temperature [46] due to the coupling between the short-lived isomer (t m 1/2 = 3.66 h) and the long-lived ground state (t g 1/2 = 36 Gyr; see Söderlund et al. [47]). During the 13 C pocket phase the temperatures are so low (∼80-100 MK) that the two states actually behave as separate nuclei, being internal transitions highly forbidden by nuclear selection rules. On the other hand, at the higher temperatures of the TPs, overlying mediating states are excited and can decay to the longlived ground state as well (see, e.g., Heil et al. [48]). This increases the 176 Lu g production at the expense of 176 Hf, whose production is suppressed because of the enhanced (n, γ) branch feeding 176 Lu. The production of 176 Lu g is then determined by the partial (n, γ) cross section of the ground state 176 Lu g to the total cross section. In our models, this ratio is set to 0.20 for temperatures lower than 200 MK and 0.25 for higher temperatures (see Cristallo et al. [49]). The new ASTRAL v0 evaluations indicate that both the production and the destruction channels of the long-lived 176 Lu g are greater than the REF case (see Table 1). Moreover, the destruction cross section of 176 Hf is slightly larger. As a whole, the NEW model shows an abundance of 176   Accordingly to the current paradigm, ancient carbon-rich AGB stars that evolved prior to the formation of the Solar System are the progenitor of about 90% of presolar SiC grains, termed the mainstream (MS) grains, recovered in pristine meteorites (see Zinner [50] for a review). Isotopic s-element abundance ratios measured in those grains have been shown to provide accurate constraints on the 13 C pocket (e.g., Liu et al. [51]). In addition, the typical Si isotope ratios of MS grains suggest that their parent stars should have close-to-solar (e.g., Hoppe et al. [52]) or slightly super-solar metallicity [53], while Lugaro et al. [54] proposed that the large MS SiC grains (µm-sized) might come from AGB stars of about twice solar metallicity. More recently, based on chemical and chemo-dynamical models of the Galaxy coupled with dust yields resulting from AGB models, Cristallo et al. [55] showed that the majority of presolar SiC grains originated from AGB stars with M ∼ 2 M and Z ∼ Z (see also Gail et al. [56]). In this regard, magnetic models for 2 M AGB stars with close-tosolar metallicities show 13 C profiles flat and extended enough to provide a good match to measured grain data [18]. In Figure 4, we compare NEW and REF models with available laboratory measurements of isotope ratios of barium in presolar SiC grains. The isotope ratios are reported in the standard δ-notation, defined as the deviation in parts per thousand of the isotopic ratio measured in a grain with respect to the terrestrial ratio. indicating that this model has a neutron-to-seed ratio a little too high for describing the bulk of the data. In Vescovi et al. [18], the same model was shown to be able to explain the most anomalous Mo isotope ratios of Y and Z grains, which are thought to have originated in lower-than-solar metallicity AGB stars and have Mo isotopic compositions indistinguishable from MS grains (see Liu et al. [57] for more details). In this regard, however, recent analyses are revealing that the three groups of grains have also similar Sr and Ba isotopic compositions, thus questioning the low-metallicity stellar origin of Y and Z grains [58]. From the comparison with grain data, models computed with the REF data set seem to give a better match while models adopting the ASTRAL v0 set only provide a partial overlap. The latter, as a consequence of the reduced 136 Ba abundance, results in a systematic increase of all model predictions for δ( 138 Ba/ 136 Ba) by ∼100‰. Nonetheless, strong conclusions cannot be advanced due to the relative uncertainties in the neutron-capture MACS values for 136 Ba, 137 Ba, and 138 Ba. Even if they are typically less than 5%, the uncertainty in δ( 137 Ba/ 136 Ba) and δ( 138 Ba/ 136 Ba) predictions is up to a few tens of ‰. Uncertainties regarding neutron-capture reaction cross sections and beta decays for cesium isotopes further complicate the picture, possibly leading to larger spreads in 137 Ba and 138 Ba abundances [59]. Therefore, within experimental and model uncertainties, the majority of barium isotope ratios measured in presolar SiC grain are in agreement with both REF and NEW model predictions, the latter exhibiting larger differences in the data-model comparison.   [51,60,61]. In panel (a), the best-fit line of grain data (black solid) is shown (see text for details). Symbols corresponds to different TPs for the C-rich phase, i.e., when C/O > 1 in the envelope and condensation of SiC is most likely to occur. Plotted are 2σ errors.

Conclusions
In this work, we investigated the effects induced by the adoption of a new neutroncapture cross section database on the s-process nucleosynthesis in low-mass AGB stars. We found major variations (more than 10%) in the final surface abundance for a number of isotopes. Most of the differences are a consequence of the re-evaluated cross sections, which are systematically higher than previous evaluations due to the different adopted gold cross section as a reference. Remarkable exceptions are represented by (n, γ) cross section for 142 Nd and 137 Ba, whose recent re-evaluation greatly differ from previous results especially at low energy. Because of the scarcity of experimental data in this energy region, the MACS calculation is strongly influenced by the (n, γ) cross sections in the evaluated data libraries adopted, which rely on various statistical model calculations to extrapolate the measured cross sections to higher and lower energies, potentially leading to different MACS values.
We compared the isotopic composition of barium measured in presolar SiC grains of AGB origins with the result of s-process nucleosynthesis occurring in the AGB phases of stars of 2 M with close-to-solar metallicities. We found that, within the present uncertainties in the input neutron-capture cross sections, a good agreement between model predictions and observed isotopic ratios is obtained with both new and previous evaluated MACS data sets. In this regard, more experimental measurements at low energies are required to better constraint energy-dependent cross sections for Ba isotopes.
In the near future, we plan to extend the ASTRAL database performing a systematic re-evaluation of measurements performed with the activation technique and for which the revision of the 197 Au(n, γ) cross section provides a new spectrum-averaged cross section to be used as normalization. The revised data set will likely have a deep effect on s-process nucleosynthesis both occurring in AGB and massive stars.