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Testing the role of SNe Ia for Galactic chemical evolution of p-nuclei with 2D models and with s-process seeds at different metallicities

The bulk of p isotopes is created in the 'gamma processes' mainly by sequences of photodisintegrations and beta decays in explosive conditions in Type Ia supernovae (SNIa) or in core collapse supernovae (ccSN). The contribution of different stellar sources to the observed distribution of p-nuclei in the Solar System is still under debate. We explore single degenerate Type Ia supernovae in the framework of two-dimensional SNIa delayed-detonation explosion models. Travaglio et al. (2011, TRV11) discussed the sensitivity of p-nuclei production to different SNIa models, i.e. delayed detonations of different strength, deflagrations, and the dependence on selected s-process seed distributions. Here we present a detailed study of p-process nucleosynthesis occuring in SNIa with s-process seeds at different metallicities. Based on the delayed-detonation model DDT-a of TRV11, we analyze the dependence of p-nucleosynthesis on the s-seed distribution obtained from different strengths of the 13C-pocket. Using a Galactic chemical evolution code (see Travaglio et al. 2004) we study the contribution of SNIa to the solar stable p-nuclei. We find that explosions of Chandrasekhar-mass single degenerate systems produce a large amount of p-nuclei in our Galaxy, both in the range of light (A<120) and heavy p-nuclei, at almost flat average production factors (within a factor of about 3). We discussed in details p-isotopes such as 94Mo with a behavior diverging from the average, which we attribute to uncertainties in the nuclear data or in SNIa modelling.

explained in the framework of explosions of Chandrasekhar-mass white dwarfs resulting from the single-degenerate progenitor channel, we find that they are responsible for at least 50% of the p-nuclei abundances in the Solar System. Subject headings: hydrodynamic, supernovae, nucleosynthesis, p-process They noticed that for a flat s-seed enhanced distribution the production factors of light p-nuclei show a strong deficiency in the range 78 Se to 98 Ru. From this, they concluded that SNIa may have contributed to the enrichment of p-nuclei more effectively than ccSNe.
In our previous TRV11 paper, we obtained a consistent production of p-nuclei in the single-degenerate Chandrasekhar mass WD explosion scenario. We presented two-dimensional hydrodynamic models of SNIa. The corresponding nucleosynthesis was calculated in a post-processing step following the thermal history of Lagrangian tracer particles. We found a significant production of p-nuclei from these stellar explosions, at the same level compared to 56 Fe for light as well as heavy p-nuclei. We demonstrated that our model is able to produce light and heavy p-nuclei in one single process. In our analysis, we assumed enhanced s-seed distributions directly obtained from a sequence of thermal pulses in the material accreted onto the exploding white dwarf from a normal companion star (see Gallino et al. 1998). In the context of light-p nuclei production, the major problem discussed in TRV11 is the resulting abundance of 94 Mo, found to be far too low relative to the abundances of the other light-p nuclei. We also found an important contribution from p-process nucleosynthesis to 80 Kr and 86 Sr (originally considered s-only nuclei), to the neutron magic 90 Zr, and to the neutron-rich 96 Zr (due to neutron captures from the residual abundance of 22 Ne during the explosive phase). Concerning the heavy p-isotopes, the s-process nature of 152 Gd has been later confirmed by different works on s-process nucleosynthesis (Gallino et al. 1998;Bisterzo et al. 2010), where a predominant s-process origin was demonstrated (see also discussion in TRV11).
In the present paper we investigate for the first time in the literature the effect of metallicity on p-process nucleosynthesis in SNIa, starting with a range of s-seed distributions obtained for different metallicities. Using a simple chemical evolution code (Travaglio et al. 2004), we estimate the contribution of SNIa to the solar p-process composition. The same study was recently done for radiogenic p-isotopes by Travaglio et al. (2014).
It is currently impossible to discuss the interplay between the role of SNeIa and ccSNe in the production of p-nuclei in the Galaxy. Infact a complete study of p-nucleosynthesis with metallicity is missed for ccSNe. But also from the observational point of view, unfortunatey there is no way to measure observed chemical evolution of p-nuclei since they are too rare with respect to the s-and r-fractions. For example, there are recent attempts to observe elements like Mo and Ru (very debated for p-process nucleosynthesis studies) in field stars of the Galaxy at different metallicities (see e.g. Hansen et al. 2014;Peterson 2013). Only a small fraction of the elements Mo and Ru are p: 14.84% of the total Mo is 92 Mo and only 9.25% is 94 Mo; for Ru, only 5.5% of the element is 96 Ru and 1.88% is 98 Ru. The p-fractions indicated above are therefore too small to be of any interest when the elements are observed in field stars. Only when will be possible to observe isotopes of Mo and Ru in the spectra then we will be able to give interesting indications on the details of their nucleosynthesis processes.
For this work, the adopted SNIa model (described in detail in TRV11) is summarized in Section 2, together with a brief description of the tracer particles method used for nucleosynthesis calculations. In Section 3 the s-process seed distributions considered in our study are described in detail. The resulting p-process production and the effect of metallicity on p-nuclei is discussed in Section 4, where also an analysis of the various production mechanisms of the p-nuclei will be performed, taking into account nuclear uncertainties. In Section 5 we analyzed in detail how s-seeds with different atomic mass number contribute to the p-nuclei production. Galactic chemical evolution calculations are presented in Section 6, and the contribution of SNIa to the solar system p-nuclei abundances is studied. In Section 7 we discuss the contribution of SNIa to the production of radiogenic 92 Nd, 146 Sm and 97,98 Tc. Finally, conclusions and work in progress are drawn in Section 8.

Type Ia supernova models and tracer particles
We used the SNIa-explosion model (DDT-a) described in detail by TRV11. It is a representative example of the single-degenerate scenario in which the WD has accreted material from a main-sequence or evolved companion star until it finally approaches the Chandrasekhar mass and explodes as a delayed detonation. The model is based on the two-dimensional simulations presented by Kasen et al 2009. The explosion itself is simulated in 2D by means of the combustion code LEAFS (Reinecke et al. 1999;Reinecke et al. 2002;Röpke 2005;Röpke & Hillebrandt 2005) which follows the evolution with an Eulerian grid. In order to compute for each zone of the star the history of temperature and density over time for each zone of the star we introduce a Lagrangian component in the form of tracer particles. With the tracer-particle method it is possible to reconstruct the ensuing nucleosynthesis. The nuclear post-processing calculations are performed separately for each tracer. Summing the chemical composition over all tracer particles gives the total yields. The tracer particles method was first introduced by Nagataki et al. (1997) for ccSSNe, and by Travaglio et al. (2004bTravaglio et al. ( , 2005 for SNIa. For 2D simulations it has been verified that 51,200 particles as used here, uniformly distributed in mass coordinates, give sufficient resolution (Seitenzahl et al. 2010). For each tracer particle we follow the explosive nucleosynthesis with a detailed nuclear reaction network for all isotopes up to 209 Bi. We select tracers within the typical temperature range for p-process production, i.e. (1.5 − 3.7) × 10 9 K, and analyze their behavior in detail, exploring the influence of different s-process seeds on the p-process nucleosynthesis. In order to determine the s-process enrichment prior to the explosion, we assume recurrent flashes occurring in the He-shell during the accretion phase with neutrons mainly released by the amount of protons are ingested in the top layers of the He intershell. Protons are captured by the abundant 12 C and convert it into 13 C via 12 C(p,γ) 13 N(β + ν) 13 C at T ≃ 1 × 10 8 K.
3. s-seeds at different metallicities In our model, p-process nucleosynthesis occurs in SNIa starting from a pre-explosion s-process enriched seed composition. Therefore, it is essential to determine the s-process enrichment prior to the explosion. Here, we assume enhanced s-distributions produced directly by a sequence of thermal-pulse instabilities in the accreted material. This idea has been described in detail by TRV11 and was previously discussed by Iben (1981), Iben & Tutukov (1991), and Howard & Meyer (1993).
To be more specific, we assume recurrent flashes to occur in the He-shell during the accretion phase. The matter accumulated onto the carbon-oxygen white dwarf (hereafter CO-WD) therefore becomes enriched in s-nuclei. However, the mass involved and the physical properties of the 13 C-pocket, providing the free neutrons for the s-process, still have to be considered as free parameters. Since no physical models are available we explore different s-process distributions in order to better understand the dependence of our results on these initial seeds (see also the discussion in TRV11 and Travaglio et al. 2012).
For the present work we calculate s-process distributions for 8 metallicities, i.e. Z =0.02, 0.019, 0.015, 0.012, 0.011, 0.010, 0.006, 0.003 (a refined s-seed metallicity grid is necessary for chemical evolution calculations since the s-seeds are strongly dependent on metallicity), and we interpolate for all the other metallicities in between in order to calculate Galactic chemical evolution. We also investigate the effect of the s-seeds with different et al. 2010 for a detailed discussion of 13 C-pocket profiles). The s-process seeds adopted are shown in Figure 1 for the ST×2 13 C-pocket case, and metallicites of Z =0.01, 0.006, 0.004, 0.003. In Figure 2 we show the average of four 13 C-pockets at different metallicities. In all figures the s-seed abundances are normalized to the solar abundances of Lodders (2009).
As discussed by Gallino et al. (1998) andTravaglio et al. (1999), the synthesis of heavy nuclei requires neutron captures starting from Fe seeds, so that the s-process is expected to decrease with decreasing metallicity, i.e. to be of secondary nature. However, the abundances produced depend not only on the initial Fe concentration but also on the neutron exposure. The concentration of 13 C in the pocket is of primary-like nature (it is built from H and freshly made C, and hence is independent of metallicity), while the abundance of the neutron absorber 56 Fe varies linearly with Z. Therefore, for a given amount of 13 C in the pocket, the neutron exposure (proportional to the ratio 13 C/ 56 Fe) is expected to increase linearly with decreasing metallicity. This dependence would compensate for the secondary nature of the s-elements, if the yields of s-nuclei were linearly dependent on both neutron exposure and Z. In addition, the behavior of 208 Pb has to be considered separately (Travaglio et al. 2001). The gradual increase of the neutron exposure towards low metallicities masks the expected secondary behavior (see also Clayton 1988), resulting in a rather complex dependence of s-process yields on metallicity. For the lower metal content the neutron flux feeds Pb (in particular 208 Pb). A clear understanding of the s-seeds behavior versus metallicity, including the production of neutron-magic 208 Pb at the termination of the s-process path, is very important for the nature of p-process (see Section 4). Figure 1 shows a variation by a factor of ≃10 for the abundances of the light s-only isotopes (up to A ≃140) when Z = varies from 0.003 to 0.01, and a spread of ≃5 for heavy s-only nuclei (with A >140). For 208 Pb, the variation is by a factor of ≃8, but its trend is inverted with respect the behavior of other s-only isotopes (i.e. lower Z gives higher 208 Pb abundance). In Figure 2 we plot the average of four different 13 C-pockets (ST×2, ST×1.3, ST, ST/1.5) for the metallicities discussed above. The behavior of the s-only isotopes is different from that seen in Figure 1: still a rough dependence on Z for light s-nuclei in the range 90< A < 120 is observed, but the variation is now reduced by a factor of 3. The spread is progressively decreasing for higher metallicities. Further on, for heavy s-isotopes In the region between the magic neutron number nuclei N =82 and N =126, an almost flat s-process production factor ensues. A similar trend occurs at a fixed metallicity by increasing the 13 C-pocket strength. We recall here that case STx2 is around the maximum 13 C-pocket strength we can reach, beyond which further proton ingestion during a third dredge up episode from the envelope would result in a decrease of 13 C and production of the neutron poison 14 N (see the review by Busso, Gallino, & Wasserburg 1999). In other words, with decreasing metallicity the otherwise flat s-process distribution near the neutron magic numbers N = 50 amd N = 82, corresponding to atomic mass numbers around A =90 and A =140, and also at the termination of the s-path at around A =208 are progressively distorted.

p-process at different metallicities
The p-process nucleosynthesis is calculated using a nuclear network with 1024 species from neutrons and protons up to 209 Bi combined with neutron, proton, and α-induced We discuss in this Section the sensitivity of p-process production to s-seeds at different metallicites. We analyze the primary/secondary nature of the resulting p-nuclei. According to Rauscher et al. (2013) (and references therein) the p-process is of secondary nature and scales with the amount of seed nuclei in the star. In this work we present our results obtained with SNIa models which only partly confirm this statement.
In Figure 4 we plot the resulting p-process abundances, starting from 74 Se, obtained by using different s-seeds at different metallicities. On the axis of ordinates the production factor of each isotope is plotted with respect to solar, normalized to 56 Fe. Note that the abundances of p-nuclei heavier than A = 100 are much higher than a factor of ∼3 times their solar value. However, in this Figure we plot the nucleosynthesis resulting from one single star and not the integrated abundances over all the Galaxy (see Section 6 for discussion). The choice for these 13 C-pockets and metallicities will be used for our best fit of Galactic chemical evolution calculation.
In order to better understand the dependence of p-nuclei production on metallicity and the 13 C-pocket, we show in two separate figures ( Figure 5 and Figure 6) the behavior of p-process nucleosynthesis as a function of metallicity and the 13 C-pocket, respectively.
From Figure 5 we can see that the first three p-only isotopes, 74 Se, 78 Kr, and 84 Sr, show a secondary behavior: their abundances scale almost linearly with Z. They depend mainly (for about 60-70%) on the light (up to A ≃140) s-seeds that, as shown in Figure 1 and is not p-only it has to be included in the discussion, see also TRV11) and 92 Mo and up to 138 Ba, the p-nuclei show a very weak dependence on Z. The isotopes in this atomic mass-number range are mainly produced by photodisintegration from the heavy s-seeds isotopes, thus showing a primary-like behavior (see Figure 6). Isotopes in the region from 136 Ce up to 196 Hg scale with metallicity but show the opposite trend, i.e. highest abundances for the lowest metallicities. TRV11 (see also Dillmann et al. 2008a) discussed the fact that Pb-seeds are converted to nuclei of lower mass by photodisintegration sequences starting with (γ,n) reactions. Therefore, an important contribution to the heavy p-only isotopes is obtained.
We also found, as discussed in TRV11, that the isotopes 113 In, 115 Sn, 138 La, 152 Gd, and 180m Ta, diverge from the average p-process production. Among them, 152 Gd and 180m Ta have an important contribution from the s-process in AGB stars (Arlandini et al. 1999), or the neutrino process in ccSN (Woosley et al. 1990;Wanajo et al. 2011). Both 113 In and 115 Sn are not fed by the p-process nor by the s-process. For these, we refer to the discussion of Dillmann et al. (2008b) and TRV11.
The still puzzling 94 Mo deserves special attention. Can nuclear uncertainties account for the low 94 Mo yield, compared to the other p nuclei, in our models? Howard et al. (1991) demonstrated that most of the 94 Mo is produced from 98 Mo through a (γ,n) chain.
We confirmed that a similar reaction chain also acts in our models. To illustrate this, Figure 8 shows three exemplary trajectories for which time-integrated reaction flows are plotted in Figures 9−11. The flow shown in Figure 9 gives a maximum production of 94 Mo (the corresponding trajectory is labeled " 94 Mo max " in Figure 8). The one shown in Figure   10 also favors 94 Mo production but at a lower level (the corresponding trajectory is labeled " 94 Mo drop " in Figure 8). In both cases, 94 Mo is fed through (γ,n) reaction sequences, with the strongest flow originating at 98 Mo, which,in turn, is replenished to some extent also by a small flow originating from 100 Mo. It should be noted that the reactivities for this (γ,n) sequence are experimentally well constrained, as they involve stable nuclei and the corresponding (n,γ) reaction cross sections have been measured (Dillmann et al. 2006).
Thermal population of excited states does not play a role in these nuclei and thus the measured (n,γ) cross sections allow to compute the (n,γ) and (γ,n) rates without further theory uncertainties (Rauscher 2012(Rauscher , 2014. Therefore this part of the flow does not bear large nuclear uncertainties, it is rather determined by the seed abundances received by the stable Mo isotopes. Some production of 94 Mo is also found via 95 Tc(γ,p) 94 Mo. Its contribution to 94 Mo, however, is an order of magnitude lower than that of the (γ,n) sequence and thus it does not contribute appreciably to the uncertainty although the 94 Mo(p,γ) reactivities are unmeasured.
Consequently, the only significant nuclear uncertainty is found in the destruction of The comparison between the " 94 Mo max " and " 94 Mo drop " trajectories in Figure 8 shows that " 94 Mo drop " reaches a slightly higher peak temperature. This higher temperature not only increases the (γ,n) flow, that destroys 94 Mo without increasing the production notably but also enables further destruction of 94 Mo by 94 Mo(γ,α) 90 Zr. The latter reaction is offset by a slight enhancement in 95 Tc(γ,p) 94 Mo but the flow through this reaction is still lower by a factor of 0.1 than the increased destruction flow. This illustrates that 94 Mo can only be produced within a narrow temperature window: at low temperature, the (γ,n) flow is small or non-existent, at too high temperature 94 Mo is destroyed by additional reactions.
Prerequisite for the efficient production of 94 Mo by photodisintegration in any site is that the mainly contributing trajectories spend as much time as possible in this temperature window.
Finally, Figure 11 shows the flows for a trajectory leading to a minimal production of 94 Mo although the achieved peak temperature is similar to that in the " 94 Mo max " case (the corresponding trajectory is labeled " 94 Mo min " in Figure 8; incidentally this is the same trajectory giving a maximum 92 Nb production as shown in Figure 5 of Travaglio et al. 2014). Inspection of the flows shows that all (γ,n) flows in this region are significantly suppressed compared to the " 94 Mo max " case in Figure 9. The 94 Mo−→ 93 Mo flow is too small to show in the plotted range. The 91 Zr−→ 92 Zr flow is even replaced by its reverse.
The key to understanding the difference is the fact that the " 94 Mo min " trajectory reaches photodisintegration temperatures only at much higher density (note the logarithmic scale of the horizontal axis in Figure 8). At all times, A(n,γ)B and B(γ,n)A rates are competing.
Their relative strengths are on one hand determined by the reaction Q-value (which is given through the well-known nuclear masses) but on the other hand (n,γ) rates also scale with the available neutron density whereas (γ,n) do not (Rauscher 2011). At the temperatures at which photodisintegration of nuclei in the Mo region becomes possible, heavier nuclei are already significantly destroyed because they are less tightly bound (their Q-value for (n,γ) is lower than that of lighter nuclei; see also Rauscher et al. 2013). This allows (n,γ) reactions to occur in the lighter region and at high density they will be faster than their (γ,n) counterparts. This illustrates the important point that significant production of p-nuclei in a γ-process is possible only when the densities remain limited, i.e. it depends sensitively on the thermodynamic histories of the explosive layers. For example, a model in which more trajectories experience lower densities during γ-processing would lead to increased 94 Mo production. However, since this scenario will affect all (n,γ)/(γ,n) ratios and thus it is unclear whether it would lead to an enhancement of the final 94 Mo with respect to the other light p-nuclides. This has to be investigated in detail in future calculations because the impact of enhanced (n,γ) rates at higher density is not trivial as it depends on the specific Q-values in the (γ,n) chains producing specific isotopes. Furthermore, it will also impact other reaction types (such as (p,n), (p,γ), and their reverses) in different ways and thus the final outcome strongly depends on the actual reaction sequences producing and destroying a specific nucleus. This may change the ratio of the 94 Mo abundance also relative to abundances of other p-nuclei but it remains an open question whether the required relative increase by a factor of 10 can be achieved.

The role of s-seeds of different atomic mass number for p-process nucleosynthesis
In order to understand in detail the s-seed origin of each p-nucleus, we performed the following study: fixing the metallicity (Z = 0.006, i.e., to a value where we find the highest production of p-nuclei in our Galactic chemical evolution calculations, see Section 6) and fixing a 13 C-pocket (i.e., STx2 which is the highest value we used), we first tested the role of the s-seed 208 Pb alone, by assigning solar abundances to all other s-seed nuclei. Details of the resulting effect on p-nucleosynthesis are given in Table 1 (third column for the 208 Pb only case, and second column for the standard case). A 208 Pb seed alone contributes about 30% to 74 Se, and 10-20% (or less) to all the other light-p nuclei up to 158 Dy (with the exception of 144 Sm, where 208 Pb alone accounts for about 45%). The contribution to the isotopes between 162 Er and 190 Pt from 208 Pb is about 40%. Finally, for the heaviest of the p-only nuclei, 196 Hg, we find the highest share ( 60%) in production originating from 208 Pb.
In Table 2 we list all s-isotopes which we find to have p-contribution. For these isotopes we report in the last column the effect of 208 Pb. We find that most of these isotopes (from 80 Kr up to 176 Hf), the 208 Pb seed contributes about 10-20% (or less). A similar analysis has been carried out accounting for either as s-nuclei either the only heavy s-nuclei (140 ≤ A < 208) or the light s-nuclei (70 ≤ A < 140) only. The results are shown in Table 1: in Column 6 the results for the heavy s-seed only case and in Column 7 the light s-seed only case are given. Not surprisingly, the heavy s-nuclei are most important for the heavy p-nuclei, in particular for 184 Os (100% of contribution), 158 Dy (89%), 136,138 Ce (about 84% and 75%, respectively), 190 Pt (about 73%), and 156 Dy (about 70%), but there are also significant contributions of about 40-60% are to the other heavy p-isotopes in the region from 144 Sm up to 196 Hg. We also find ∼30-40% of the light p-nuclei up to 132 Ba to originate from heavy s-seeds, with the exception of 94 Mo and 130 Ba, which have a lower share of ∼15%. In contrast, light s-seeds are the main producers of the light p-isotopes, and they account for about 73% for 74 Se and 94 Mo (where important contribution from other stellar sources or errors in reaction rates can be estimated), and finally 130 Ba (about 80%). All other light-p isotopes are produced from light-s seeds with typical sharesin the rage from 40 to 60%. The heaviest p-nuclei are almost unaffected by the light-s seeds.
In the fourth columns of Table 1 and Table 2 we show results of a second test for comparison, where we retain a metallicity of Z = 0.006, but reduce the strenght of the 1, 2). Comparing the two cases presented in Table 1 (column 3 and 5), we notice that typically the case with STx2 13 C-pocket and a 208 Pb seed contributes by a factor of ∼2 to the light-p nuclei with respect to the case STx1.3 13 C-pocket and 208 Pb seed. For the abundance of 144 Sm we obtain identical results for STx2 and STx1.3 cases. In contrast, however, we observe an increased production of the heavy-p nuclei for the case STx2 and 208 Pb seed by ∼10%. The only exception is for the heaviest p-nucleus 196 Hg, where we find a highest abundance in the case STx1.3 208 Pb alone. The reason for this behavior is that at the same metallicity (Z = 0.006) the 13 C-pocket STx1.3 is less efficient than the 13 C-pocket STx2 for the production of heavy-s as well as for 208 Pb.

Galactic chemical evolution
The main goal of this work is to provide predictions for Galactic chemical evolution of p-nuclei. For this, we employ the Galactic chemical evolution code presented by Travaglio et al. 1999Travaglio et al. , 2001Travaglio et al. , 2004. The model considers the Galaxy as the evolution of three interconnected zones, halo, thick disk and thin disk. The matrix of the isotopes within the chemical evolution code was set to cover all the light nuclei up to the Fe-group, and all the heavy nuclei along the s-process path up to 209 Bi. For the present work we extended the matrix of the isotopes to account for the p-nuclei and we followed their evolution over time/metallicity until solar metallicity was reached. We included in the code the p-nuclei abundances obtained from our SNIa model at various metallicities as discussed in Section 4, and interpolate between them smoothly. In Figure 7 we show the resulting p-process production factors taken at the epoch of Solar System formation for nuclei in the atomic mass number range 70 ≤ A ≤ 210. To be more clear we note that for these results we only include SNIa for the contribution to p-nuclei. Our choice for the s-seeds was introduced in Section 3 (see Figure 3). As discussed in the previous section, it is clear that a few nuclei originally ascribed to the p-only group ( 113 In, 115 Sn, 138 La, 152 Gd, and 180m Ta) are far below the average of the other p-nuclei. Thus, if this model is correct, they should be ascribed to different astrophysical sources. As shown in Figure 7 and detailed in Table 3, we find in our Galactic chemical evolution calculations that all the other p-only isotopes are-within a factor of about three-produced at the Solar System composition. The lightest p-nucleus 78 Kr and the heaviest 158 Dy and 180 W can be ascribed to the same production site when an additional uncertainty factor of two is included (which seems reasonable given the large uncertainties in photodisintegration rates). Therefore, for the first time, we are able to explain the synthesis of almost all p-isotopes production in one single scenario. The most striking problem we face is the very low relative abundance of the true p-only 94 Mo with respect the the average of all other p-only nuclei, which is possibly related to the theoretical estimate of the neutron capture on unstable 93 Mo. The effect of the nuclear uncertainties will be explored in a forthcoming paper. Figure 7 and Table 4 also show that neutron magic 90 Zr and especially 96 Zr receive an important contribution by the p-process (about 20% and 40%, respectively). Moreover, it is not excluded that the most proton-rich s-only isotopes for a given element may receive some contribution from the p-process. As illustrated in Figure 7, this is the case for 80 Kr and 86 Sr, with p-contribution of the order of 10%. However, before examining the problem in more detail, an analysis of the uncertainties in the involved reaction rates is necessary.
Out of the light p-nuclei the isotopes 78 Kr, 94 Mo, 108 Cd, and 114 Sn are by a factor of three or more (for 94 Mo) less abundant compared to the solar value. Among the heavy-p nuclei 158 Dy is also by more than a factor of three below the solar abundance. In contrast, we found 180 W higher by a factor of more than three with respect to solar. Under the hypothesis that SNIa are responsible for 2/3 of solar 56 Fe, and assuming that our DDT-a model represents the typical SNIa with a frequency of 70% (Li et al. 2011), we conclude that they are responsible for at least 50% of all p-nuclei.
With the same approach, Travaglio et al. (2014) discussed the origin of the short-lived radionuclides 92 Nb and 146 Sm. They compared the value of the ratio between the abundances of these radionuclides and those of the corresponding stable reference isotopes 92 Mo and 144 Sm to what has been recently measured in meteorites ).
The conclusion is that SNIa can also play a key role in the production of 92 Nb and 146 Sm, but nuclear uncertainties have to be taken into account.
In the framework of Galactic chemical evolution of p-nuclei, the role of ccSN has also to be taken into account. Rauscher et al. (2002) followed the γ-process through the presupernova stages and the supernova explosion. As expected for the weak s-process A ≤ 124 and 150 ≤ A ≤ 165 the production of the p-isotopes is down by about a factor of 3 − 4. While the main γ-process synthesizes p-nuclei through photodisintegration reactions during the SN shockfront passage, some of the models showed pre-explosive p-production due to a high entropy in the O/Ne shell of the evolved star. Most of this is wiped out again when the supernova shock sweeps through the layer. Nevertheless, depending on the adopted convection model (see also Bazan & Arnett 1994), some light, strongly bound p-nuclei may survive from pre-explosive production. This behavior complicates predictions for the contribution of ccSNe to the solar composition of p-nuclei. In addition, it has to be taken into account that the SNIa scenario discussed here may not explain all normal events. Thus, alternative scenarios for p-process nucleosynthesis in binary systems should be explored, such as SNeIa from WD-WD mergers (e.g. Pakmor et al. 2010Pakmor et al. , 2012 or double detonations in sub-Chandrasekhar mass WDs (e.g. Fink et al. 2010).

Conclusions
We have presented results of detailed p-process nucleosynthesis calculations for two-dimensional models of delayed detonations in Chandrasekhar-mass WDs resulting from the single degenerate progenitor scenario. In these SNIa models, the nucleosynthesis was followed by the tracer-particles method. The initial s-seeds were assumed to be created during the mass accretion phase. Since up to now no nucleosynthesis calculations of the accretion phase are available our hypothesis is based on the assumption that a small amount of protons are ingested at the top layers of the He intershell. Following the work of TRV11 on the nucleosynthesis for a solar metallicity SNIa model in the same scenario, we tested and discussed the consequences of different amounts of 13 C and different metallicites on the synthesis of p-nuclei. We demonstrated that the 208 Pb s-seed alone plays an important role for p-nuclei production, due to photodisintegration chains starting from the heaviest nuclei and going down in mass number. We analyzed the dependence of all the p-isotopes on metallicity, and we identified the isotopes with a weak (like 92 Mo and 138 Ba) and a strong (in particular the lightest p-isotopes, 74 Se, 76 Kr, and 84 Sr) dependence on Z.
We discussed the still puzzling origin of 94 Mo. Clearly, nuclear uncertainties cannot account for the factor of 10 deficiency in 94 Mo abundance relative to other p-abundances.
The 94 Mo production was found to depend on the seeds in the Mo isotopes as well as on the density at which the photodisintegration process occurs. This leaves room for possible variations in the hydrodynamic history of the mainly contributing explosive trajectories which could change the relative p-abundances.
By means of a simple Galactic chemical evolution code, including p-process contributions at different metallicities, we explored the SNIa contribution to the p-nuclei abundances in the Solar System. We concluded that p-nuclei are mainly of primary-like origin, and that SNIa can contribute at least 50% to the solar abundance of all p-nuclei provided that they result from standard Chandrasekhar-mass delayed-detonations forming in the single-degenerate progenitor channel. Thus we identified a stellar source which, in principle, is able to produce light and heavy p-nuclei almost at the same level relative to Seitenzahl, I.R., Röpke, F.K., Fink, M., & Pakmor, R. 2010, MNRAS, 407, 229 Thielemann, F.-K., Nomoto, K., & Hashimoto, M. 1996, ApJ, 460, 408 Travaglio, C., Galli, D., Gallino, R., Busso, M., Ferrini, F., & Straniero, O. 1999       ( * ) -Isotopes pointed with * have to be excluded from the p-only list, as discussed by TRV11.