# New reaction rates for improved primordial D/H calculation and the cosmic evolution of deuterium

###### Abstract

Primordial or big bang nucleosynthesis (BBN) is one of the three historical strong evidences for the big bang model. Standard BBN is now a parameter free theory, since the baryonic density of the Universe has been deduced with an unprecedented precision from observations of the anisotropies of the cosmic microwave background (CMB) radiation. There is a good agreement between the primordial abundances of He, D, He and Li deduced from observations and from primordial nucleosynthesis calculations. However, the calculated abundance is significantly higher than the one deduced from spectroscopic observations and remains an open problem. In addition, recent deuterium observations have drastically reduced the uncertainty on D/H, to reach a value of 1.6%. It needs to be matched by BBN predictions whose precision is now limited by thermonuclear reaction rate uncertainties. This is especially important as many attempts to reconcile Li observations with models lead to an increased D prediction. Here, we re-evaluates the d(p,He, d(d,n)He and d(d,p)H reaction rates that govern deuterium destruction, incorporating new experimental data and carefully accounting for systematic uncertainties. Contrary to previous evaluations, we use theoretical ab initio models for the energy dependence of the –factors. As a result, these rates increase at BBN temperatures, leading to a reduced value of D/H = (2.45 (2), in agreement with observations.

## I Introduction

The standard hot big–bang model is supported by three pieces of observational evidence: the cosmic expansion (the Hubble law),
the Cosmic Microwave Background (CMB)
radiation, and primordial or big bang nucleosynthesis (BBN).
There is a good agreement between primordial abundances of He, D, He and Li deduced from observations and from primordial
nucleosynthesis calculations.
It is worth remembering that BBN has been essential in the past, first to estimate the baryonic density
of the Universe, and give an upper limit on the number of neutrino families.
The number of light neutrino families was later determined from the measurement of the
width by LEP experiments at CERN. The observations
of the anisotropies of the cosmic microwave background by
WMAP WMAP9 , and more recently the Planck Planck13 ; Planck15 space missions, enabled the extraction of cosmological
parameters and, in particular, the baryonic density of the Universe. It was the last free parameter in BBN
calculations, now measured with an uncertainty of less than 1%: = 0.022250.00016 ^{1}^{1}1
We note , with the ratio of the baryonic to critical density and the
Hubble constant in 100 km s Mpc units.
Planck15 .
Higher precision standard BBN predictions are now needed for comparison with primordial abundances deduced from observations.

Calculations of the primordial abundance are in agreement with those deduced from observations in Hii (ionized hydrogen) regions of compact blue galaxies Ave15 . Contrary to , is both produced and destroyed in stars and thus its abundance evolution as a function of time is not well known and difficult to compare with predictions. It is well known that BBN calculations of Cyb08b ; CV10 ; Coc14b ; Cyb15 overpredict the observations by a factor of 3. This is the so-called “lithium problem”, which has not found a satisfactory solution yet Fie11 ; Coc14a (see also Ref. Fu15 ). Promising ideas revolve around stellar physics or exotic physics, now that a nuclear physics solution is highly unlikely Ham13 . Deuterium’s most primitive abundance is determined from the observation of very few cosmological clouds at high redshift, on the line of sight of distant quasars. Recent observations of damped Lyman- (DLA) systems at high redshift show a very small dispersion of deuterium abundance values, leading to a 1.6% uncertainty on the mean value that is marginally compatible with BBN predictions.

Here, we will focus on the re-evaluation of the most important BBN reaction rates for deuterium nucleosynthesis. Sensitivity studies (e.g., Ref. Cyb04 ; CV10 ) have shown that the d(d,n)He, d(d,p)H and d(p,He reactions are the most influential for the D/H predicted abundance: a 10% variation of their rates induces a relative variation of %, % and %, respectively, of D/H. Concerning these reactions, since the most recent dedicated BBN evaluations of reaction rates Cyb04 ; Ser04 ; Des04 , new experiments were performed Leo06 ; Tum14 . On the contrary, no new experiment concerning the d(p,He reaction has been performed and its rate uncertainty (5%–8% Des04 ; Ade11 ), according to Di Valentino et al. DiV14 , now dominates the error budget of D/H predictions.

The recent NACRE–II
^{2}^{2}2In the following, we use “NACRE” when referring to the Angulo et al. NACRE original evaluation,
and “NACRE–II” when referring to the recent sequel by Xu et al. NACRE2 .
NACRE2 evaluation provides new rates for these reactions.
However, too few explanations are given regarding the data selection, fitting, and uncertainty estimation.
Therefore, the published evaluated rates of these reactions are not suited to reach the precision
required for BBN calculations.
Here, we re–evaluate the d+d rates, to take advantage of the new precise measurement by Leonard et al. Leo06 , together with the d(p,He rate.
We use these new rates to derive BBN abundances and associated uncertainties.
We will then compare our new BBN predictions for deuterium with high-redshift observations in the framework of cosmic evolution models.

For our re-evaluations, we chose a compromise between adopting of the most recent, and more precise measurements only, (i.e., LUNA Cas02 for d(p,He and Leonard et al. Leo06 for d+d) on the one hand, and including all available experimental data in the fit on the other hand. The main difficulty in this analysis is the treatment and extraction of systematic uncertainties. Another difficulty is the choice of the fitting functions: polynomials NACRE ; Cyb04 , splines Nol00 or R–Matrix Des04 have been used. For these three reactions we chose instead, as fitting functions, results from nuclear reaction models. It has the advantages of smoothing the accidental fluctuations in experimental data and providing a better interpolation of the data. In the case of a single data set, the fitting process is reduced to a normalization, but when several data sets have to be considered, a global normalization is required, which is discussed in the Appendices. In addition, we found that, by using the theoretical ratio of d(d,n)He and d(d,p)H cross sections, it was possible to identify inconsistent data sets in an objective way.

This article is organized as follows. In Sections II and III, we discuss the normalization of d(p,He, d(d,n)He and d(d,p)H theoretical –factors to experimental data. (The normalization method is presented in Appendix A and the experimental data are discussed in Appendices B and C.) In Section IV, we present the new reaction rates (tabulated in Appendix D) and the Monte Carlo method for nucleosynthesis calculations. BBN results are discussed in Section V, while the cosmic deuterium evolution is presented in Section VI. Finally, we show in Section VII that the new precise D/H observations put a strong constrain on the proposed solution to the lithium problem.

## Ii The D(p,He –factor

The sensitivity of the D/H abundance ratio to d(p,He rate variations is CV10

(1) |

Therefore, a precision of 5% is required for the rate, to match the 1.6% uncertainty in the observed value. In the appendices, we detail our choice of the data sets we included in our analysis. Data sets for which no systematic uncertainty was quoted (or when the quoted uncertainty was too large) were excluded from the fit. Nevertheless they are reported in the figures and tables, where the scatter of values gives an idea of their systematic uncertainties.

NACRE NACRE used data from Refs. Gri62 ; Gri63 ; War63 ; Ber64 ; Fet65 ; Ste65 ; Gel67 ; Wol67 ; Sch95 ; Ma97 , plus a few high energy experiments and a polynomial fit, while Descouvemont et al. Des04 (DAACV hereafter) used a slightly different set of data, from Refs. Cas02 ; Gri62 ; Gri63 ; War63 ; Wol67 ; Ma97 ; Bai70 ; Sko79 ; Sch97 and included the data from Ref. Cas02 (post NACRE; from LUNA) with an R–matrix fit. Figure 1 summarizes all the experimental data that we collected (see Appendix B), together with the fitted curves from Refs. Des04 ; Ade11 and the theoretical –factor from Marcucci et al. Marcucci . This is the theoretical –factor that we renormalize to the data, as described in Appendix A: the renormalization factor () and the associated uncertainty () are obtained by minimization [see Eqs. (12) and (13)]. The results () of our analysis for the nine data sets Gri62 ; Gri63 ; War63 ; Wol67 ; Bai70 ; Ma97 ; Sch97 ; Cas02 ; Bys08b can be found in Table 1, column 3. Column 5 of the same table list the systematic uncertainties (), only available for the four most recent data sets, to which we restrict our subsequent analysis. The systematic uncertainties are quadratically added to the normalization factor uncertainties [Eq. (18)] before calculating the recommended normalization factor.

d(p,He | ||||
---|---|---|---|---|

Ref. | ||||

Bys08Bys08b | 3 | 1.03650.1457 | 0.1360 | 0.08 |

Cas02Cas02 | 51 | 1.02430.0092 | 0.5792 | 0.045 |

Sch97Sch97 | 7 | 0.96570.0062 | 11.1799 | 0.09 |

Ma 97Ma97 | 4 | 0.84690.0381 | 1.1052 | 0.09 |

Bai70*Bai70 | 11 | 0.91080.0143 | 0.3874 | n.a. |

Wol67*Wol67 | 3 | 0.92020.0514 | 0.2967 | n.a. |

War63*War63 | 3 | 0.88670.0581 | 0.2994 | n.a. |

Gri63*Gri63 | 12 | 1.17490.0535 | 0.2322 | n.a. |

Gri62*Gri62 | 3 | 0.91040.0374 | 1.7730 | n.a. |

= normalization factor, = number of data point and = systematic uncertainty. Data sets marked with an asterisk have not been used in the analysis because the evaluation of systematics is not available.

Figure 2 displays the normalization factors from Table 1, with error bars that incorporate the systematic uncertainty [Eq. (18)] when available. One observes that when the systematic uncertainties on normalization are included for the four selected data sets, the dispersion of values of normalization factors becomes compatible with the error bars. Hence, a simple weighted average [Eq. (17)] and associated uncertainty [Eq. (19)] seems to us sufficient, leading to (Fig. 2.) with a reduced chi–square of = 0.71. We checked that the method used in some other evaluations (e.g., Ref. Ser04 ), and discussed in Appendix A.2, gives a very close value, [from Eq. (16) minimization].

The zero energy theoretical –factor is given by eVb, which, after renormalization (), leads to eVb, in excellent agreement with the value eVb determined by Adelberger et al Ade11 . Hence, experimental data do not favor a global increase by a factor of as proposed by Di Valentino et al. DiV14 and the Planck collaboration Planck15 to better reproduce the Cooke et al. Coo14 deuterium observations (see § VI). Even when considering the experimental data that were not included in our fit (because their systematic uncertainties were not quantified; see Fig. 2), there is no evidence for such a global enhancement. Figure 3 displays the experimental –factor data, divided by the theoretical one Marcucci . Except for Griffith et al. Gri63 , low energy data are in excellent agreement with our recommended average (horizontal solid lines). At higher energies, previous phenomenological fits Des04 ; Cyb04 ; Ade11 closely follow the experimental data points (Fig. 3). In particular they are attracted by the Bailey et al. data Bai70 with very small error bars (Fig. 2) but unknown systematic uncertainty (see Appendix B). For this reason we do not use these data in our fit. As it is based on a theoretical model Marcucci that predict the shape of the –factor, our fit is little influenced by the Ma et al. data Ma97 with relatively large uncertainties (systematic uncertainties are not shown in Fig. 3 but displayed in Fig. 2). This explains that at BBN energies, the scarce data generally fall below our recommended average. Hence, while at low energy, our –factor is in excellent agreement with other evaluations, at BBN energies our recommended –factor is higher. As a result, the BBN deuterium production calculated with our rate will be reduced (see § V). Precise cross section measurements at BBN energies (100 keV) are hence strongly needed.

## Iii The D(d,n)He and D(d,p)H –factors

The sensitivity of the D/H abundance ratio to d(d,p)H and d(d,n)He rate variations is CV10

(2) |

so that a precision of better than 2% is required for these rates.

Data from Refs. Sch72 ; Gre95 ; Bro90 ; Kra87 were considered by the NACRE NACRE collaboration and were also used in the R–matrix evaluation of DAACV Des04 . Since DAACV, new measurements were performed by Leonard et al. Leo06 and by Tumino et al. Tum14 . Figures 4 and 5 display all the experimental data that we collected (see Appendix C). They show that the new, directly measured data Leo06 (labelled “Leo06” in Figures) follow reasonably well the DAACV R–matrix fit, even though it was calculated before the experiment was conducted. These figures also display the results from an ab initio calculation by Arai et al. Ara11 , which we normalize to the experimental data as described in Appendix A. This microscopic calculation uses a four-nucleon model with a realistic nucleon-nucleon interaction. It was shown that the tensor force plays an important role in the d+d reactions. However, the theoretical work of Ref. Ara11 was focused on low energies, and only partial waves up to have been included. For this reason, above MeV, the theory underestimates the data. Consequencely, we choose to limit the normalization to data below 0.6 MeV, which is well above the energy region important for BBN (dashed vertical lines).

Similar to our analysis of the d(p,He reaction (Section II) we assume different normalization factors in different experiments and allow them to be different for d(d,n)He and d(d,p)H. The results of our fits for the collected eleven data sets Pre54 ; Arn54 ; Gan57 ; Sch72 ; first ; Kra87 ; Bro90 ; Gre95 ; Leo06 ; Tum14 (Appendix C) can be found in Table 2 and in Figures 6 and 7. Because of the limited energy range, 0.015 MeV MeV (considering electron screening at low energy and nuclear model restrictions at high energy, see Appendix C), the number of adopted data points, , is smaller compared to the original publications. For instance, because of these limitations, we had to disregard the Shulte et al. Sch72 data and the lowest energy Krauss et al. Kra87 data.

In all experiment but one, we fitted the d(d,n)He and d(d,p)H data sets independently. Nevertheless, with a few exceptions, in a given experiment, the d(d,n)He (Fig. 6) and d(d,p)H (Fig. 7) normalization factors are very similar. For the Leonard et al. data Leo06 , we took advantage of the published error matrix and performed a fit taking into account all correlations between data points of different energies or reactions. This resulted in a simultaneous fit of both the d(d,n)He and d(d,p)H cross sections. The results, displayed in Fig. 6 and Fig. 7 as grey squares show little difference with the simple fit (blue) circles and are not used. As for the d(p,He reaction, we select the data sets for which the systematic uncertainties are published (see last column of Table 2). As discussed in more detail in Appendix C, we do not use the indirect measurement from Tumino et al. Tum14 as the energy dependence of their experimental –factors is slightly different from theory and other experiments, in particular for the d(d,n)He reaction as it can be seen in Figs. 4 and 6.

For the recommended normalization factor, we obtain and (weighted average error) for the d(d,n)He and d(d,p)H reactions with reduced chi–squares close to unity (1.33 and 0.92). (We obtained similar results, , and when using the alternative method presented in Appexdix A.2.) Figures 8 and 9 display the scatter of all experimental data, in the 0.015 MeV 0.6 MeV range, relative to the theoretical model from Ref. Ara11 . Data sets that significantly deviate from the fits were just not included in the fit (e.g., Tumino et al. Tum14 and Arnold et al. Arn54 for reasons discussed in Appendix C) or have large systematic uncertainties (Krauss et al. Kra87 ) that are not included in the error bars of these figures.

d(d,n)He | d(d,p)H | |||||
---|---|---|---|---|---|---|

Ref. | ||||||

Tum14* Tum14 | 29 | 0.8610 0.0064 | 1.0332 | 0.9322 0.0075 | 0.1582 | n.a. |

Leo06 Leo06 | 8 | 0.9333 0.0065 | 2.0327 | 0.9415 0.0061 | 5.3758 | 0.02 |

Gre95 Gre95 | 8 | 1.0158 0.0134 | 1.2472 | 0.9972 0.0134 | 0.9989 | 0.03 |

Bro90 Bro90 | 9 | 0.9644 0.0025 | 2.3659 | 0.9584 0.0020 | 1.9690 | 0.013 |

Kra87 (B) Kra87 | 7 | 0.8683 0.0220 | 0.2919 | 0.8637 0.0208 | 0.1001 | 0.064 |

Kra87 (M) Kra87 | 20 | 0.9185 0.0177 | 0.6236 | 0.8902 0.0171 | 0.1766 | 0.082 |

FRG85* first | 45 | 0.9913 0.0062 | 0.6509 | 0.9887 0.0060 | 0.5044 | n.a. |

Gan57* Gan57 | 36/18 | 0.9155 0.0013 | 22.8927 | 0.9223 0.0061 | 0.7350 | n.a. |

Arn54* Arn54 | 15 | 0.8860 0.0027 | 2.6995 | 0.9519 0.0029 | 2.1919 | n.a. |

Pre54* Pre54 | 5 | 0.9384 0.0275 | 0.0988 | 0.9475 0.0317 | 0.1186 | n.a. |

## Iv Reaction rates and uncertainties

The reaction rates were calculated by numerical integration of the theoretical –factors, after normalization. Above the energies imposed by the limitations of the models (2 MeV and 0.6 MeV, respectively, for d(p,He and d+d), the –factors are supplemented by the DAACV Des04 results. The influence of this high energy –factor merging is negligible at BBN temperatures, but allows for calculating the tabulated rates on a conventional temperature grid. Figure 10 shows the new rates compared to the DAACV Des04 that were used in previous works (e.g., Ref. Coc14b ). In the upper panel (d(p,He rate), we also display (dotted lines) the result of our numerical integration of the DAACV –factor within different energy intervals , with = 2, 3, 4 and 5, where and define the Gamow window (e.g., Eqs. (5) and (6) in NACRE NACRE ). In DAACV the rate was calculated this =2, not sufficient to reach the high precision needed here but that is required. Hence, to derive a more precise rate from our recommended –factors, we used a wider interval ( = 4) in our calculations. For each reaction, the 1 uncertainties on rates, , are obtained by using the 1 uncertainties on the normalization factors () to rescale the theoretical –factors, or by using the DAACV uncertainty on the –factor at the highest energies. It is worth noting that these rate uncertainties are statistically defined (1 limits), at variance with the limits provided in some other evaluations, e.g., NACRE NACRE and NACRE–II NACRE2 . The recommended reaction rates calculated from the –factors rescaled by can be found in Table 13, together with the uncertainty factors, (), defined Eval1 as

(3) |

Except at the highest energies where DAACV rate uncertainties are used, one simply has

(4) |

In the Monte Carlo calculations, the reaction rates , (with being the index of the reaction), are assumed to follow a lognormal distribution:

(5) |

where is sampled according to a normal distribution of mean 0 and variance 1 (Eq. (4) of Ref. Stats14 ). The and determine the location of the distribution and its width. For the d(p,He, d(d,n)He and d(d,p)H reactions, they are derived from the values listed in Table 13, using and . From the resulting histograms of calculated abundances, the median and 68% confidence interval is obtained from the 0.5, 0.16 and 0.84 quantiles Eval1 ; Stats14 .

## V BBN results

The standard analysis of the CMB data by the Planck satellite showed that the temperature and polarization angular power
spectra are consistent with a spatially- Euclidean CDM cosmological model with a power-law initial power spectrum
for adiabatic scalar perturbations.
The analysis includes parameters describing the baryonic and CDM densities, the cosmological constant, the amplitude and spectral index
of the primordial power spectrum and the optical depth due to reionization. Besides, the present photon temperature is well-measured
to be K Fix09 . Assuming thermal equilibrium prior to neutrino decoupling,
the radiation density is inferred by assuming that the effective number of neutrino families is Man05 .
Among the various combinations of the temperature, -polarization data and lensing of the CMB by the large scale structure of the universe
(see Table 4 of Ref. Planck15 ), we adopt the constraints obtained with the largest set of data (TT,TE,EE+lowP) without any external data and
without taking the lensing data into account. This gives a constraint on the baryonic density parameter = 0.022250.00016
with a 68% confidence level
^{3}^{3}3This corresponds to a number of baryons per photon of = (6.09140.04380),
using Coc14b ..
In full generality, when combining data one should consider a consistent code predicting both the BBN abundances and the CMB
angular power spectra. Note, in particular, that the latter requires us to determine the helium abundance which affects the recombination
process since helium recombines before hydrogen. The Planck results Planck15 used a posterior mean of
“predicted by BBN, with theoretical uncertainties dominating over the Planck error ….” (see Table 4 of Ref. Planck15 ).
One could introduce the new parameter but it is not free since it is related to through BBN.
The Planck analysis uses the PArthENoPE code Pis08 assuming a neutron mean lifetime of 880.3 s. Indeed,
what is meant by “theoretical uncertainties” includes “uncertainties in the neutron lifetime and a few nuclear reaction rates”.
This emphasizes the importance of the present analysis that uses, compared to thePArthENoPE code, improved
thermonuclear reaction rates relevant for D (and Li) nucleosynthesis.
As a first analysis, and in order to confront Planck results with our BBN predictions, we compare the independent predictions
of the CMB and BBN with 68% and 95% confidence level. Such a preliminary approach is sufficient to identify if there is any
tension between the two methods and to determine whether they are compatible at a given confidence level.

Table 3 shows the step by step progression of the He, D, He and Li abundances with improved input data (reaction rates and ). The first column (a) lists to the results of the Monte Carlo calculation from Ref. Coc14b (with =0.022180.00026 and for = 880.11.1 s) for comparison. The second column (b) uses the same 425–reaction network but for =0.02225 (and = 880.3 s). The largest difference, on , between the median of the Monte Carlo distribution of abundances (a), and the calculation using nominal values of parameters (b), is due to the non Gaussian shape of the Li/H abundance distribution, statistical fluctuations, and to minute updates of physical constants. Two rates affecting Be nucleosynthesis have been updated since DAACV Des04 . The He(Be rate from DAACV had been superseded by Cyburt & Davids Cyb08a , who included new results from LUNA. An improved evaluation of the He(Be reaction rate and associated uncertainty has been published deB14 since, using a Monte–Carlo based R–matrix analysis, and can be considered up to date. Even though the Be(n,He reaction cannot help solve the lithium problem, its rate was uncertain and affected the production at the few percent level. Until recently, the only published rate came from an evaluation by Wagoner Wag69 . Very recently, Hou et al. Hou15 clarified the origin of the Wagoner rate, but more importantly have re–evaluated it, based on He(,n)Be, He(,p)Li and Li(p,He experimental data, using charge symmetry and/or detailed balance principles. The next two columns (c and d) in Table 3 show the effect of updating the Be(n,) Hou15 and He(Be deB14 rates, respectively. The effects of using our new d(d,n)He and d(d,p)H and d(p,He rates instead of DAACV Des04 are displayed in the next columns, (e) and (f) respectively. As expected from Fig. 10, the D/H abundance is significantly reduced, together with a concomitant increase. The results of a Monte Carlo calculation, performed as in Ref. Coc14b , but with the updated rates and = 0.022250.00016 Planck15 (see above) and = 880.31.1 s PDG are shown in column (g), compared to observations (h). For deuterium, we obtain

(6) |

a | b | c | d | e | f | g (predicted) | h (observed) | |
---|---|---|---|---|---|---|---|---|

0.022180.00026 | 0.02225 | 0.02225 | 0.02225 | 0.02225 | 0.02225 | 0.022250.00016 | ||

0.24820.0003 | 0.2482 | 0.2482 | 0.2482 | 0.2484 | 0.2484 | 0.24840.0002 | 0.24490.0040Ave15 | |

/H ( | 2.635 | 2.635 | 2.635 | 2.526 | 2.452 | 2.450.05 | 2.530.04 Coo14 | |

/H () | 1.050.03 | 1.047 | 1.047 | 1.047 | 1.038 | 1.070 | 1.070.03 | 1.10.2 Ban02 |

/H () | 5.040 | 5.102 | 5.131 | 5.343 | 5.651 | 5.610.26 | 1.58Sbo10 |

Ref. Coc14b (a) ; Update of (b), Be(n,) (c), He(Be (d), d(d,n)He and d(d,p)H (e), and d(p,He (f) new rates, Monte Carlo (1) (g) and observations (h).

## Vi Cosmic deuterium evolution

Starting from our new BBN prediction [Eq. 6], it is interesting to follow the cosmic deuterium evolution. This isotope is a good tracer of stellar formation since it can only be destroyed after the BBN stage.

### vi.1 Observations

The primitive abundance of deuterium is determined from the observation of cosmological clouds at high redshift located on the line of sight of distant quasars. Very few observations are available so far. Pettini and Cooke Pet12 and, more recently Cooke et al. Coo14 observed, or reanalyzed, five DLA systems at redshift 2–3 and derived a mean value D/H = (2.530.04). Recently, Riemer-Sørensen et al. Rie15 re–measured the = 3.256 absorption system towards the quasar PKS 1937101 and have determined a robust value of D/H = (2.450.28). Finally Noterdaeme et al. Not12 measured D/H = (2.590.15) at = 2.621 towards CTQ 247. Our present BBN D/H calculated value of (2.450.10) (2) is in agreement with these observational constraints, although the observations tend to be slightly higher.

The D/H ratio can also be derived from observations of HD and H molecules in DLAs assuming that chemistry does not affect its value. The observed ratios take very different values, which may cast some doubt on this latter assumption Tum10 . Srianand et al. Sri10 , Ivanchik et al. Iva10 , and Balashev et al. Bal10 measured D/H = (1.17, (3.6 and (3.6 towards J1337+3152, Q 1232+082, and both J 0812+3208 and Q 1331+170 at = 3.102, 2.3377, and 2.626 and 1.777, respectively. Indeed, Le Petit et al. LeP09 modeled the deuterium chemistry and showed that the derived D/H ratio strongly depends on the initial physical conditions such as temperature and density. However, they considered dense clouds, whereas most DLAs are diffuse structures. Since the situation is not clear, it is premature to use these observational measurements to compare with the results of our models.

Recent local D/H observations added new constraints on the cosmic deuterium astration factor, , which is defined as the ratio of the BBN to the present deuterium abundances, D/D. In the local interstellar medium (ISM), Prodanović et al. Pro10a find their best estimate for the undepleted ISM deuterium abundance to be D/ H = (2.00.1), leading to 0.1. In the local galactic disk, Linsky et al. Lin06 analyzed spectra obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE ) satellite, together with spectra from the Copernicus and interstellar medium absorption profile spectrograph (IMAPS) instruments. This study reveals a very wide range in the observed D/H ratio. Spatial variations in the depletion of deuterium in dust grains could explain these local variations. Finally, they argue that the most representative value for the D/H ratio within 1 kpc of the Sun is (2.310.24). The deuterium astration factor, , is in this context less than 1.1. Finally, Savage et al. Sav07 use high-resolution ultraviolet spectra in the lower galactic halo and obtain D/H = . This value is consistent with the results mentioned above, but with a very large error bar.

### vi.2 Evolution

We now consider the cosmic evolution of D/H in a cosmological context in the light of the new, somewhat low, deuteriumm primordial value derived here. It is well known that, due to its fragility, deuterium is destroyed during the cosmic evolution (as soon as K). In this context, we follow the cosmic chemical evolution using a model developed in Refs. Dai06 ; Rol09 ; Van14 , based on a hierarchical model for structure formation Pre74 ; Wyi03 . A key ingredient to all evolution models is the global cosmic star formation rate, SFRs (a specific analysis devoted to different SFR is performed in Ref. Van14 ), whose evolution with redshift is constrained by many observations. Recent data from high redshift galaxy observations (the Hubble Ultra Deep Field) have significantly extended the range of redshifts for its determination, from = 4 up to 10 Bou14 ; Oes14 . Figure 11 shows the SFR fit using these observations (blue points and blue dotted line). On the other hand, observations of high gamma–ray bursts (GRBs) tend to favor a large amount of yet unobserved SFR at 9 Kis13 (black points and black solid line). Extracting the SFR from the GRB rate is not free from uncertainties and biases Tre13 . In the following, we will use the SFR derived from Ref. Tre13 (see Figure 11, black line), which is consistent with other observational constraints as shown by Vangioni et al. Van14 . To estimate the maximum astration factor of D, we have also considered an extreme case, adding an intermediate mass SFR component (between 2 and 8 ) which is shown in Fig. 11 by the black dashed curve. Note that the exact slope of the SFR at high redshift has no impact on the deuterium evolution (contrary to heavier elements). Indeed, it is well known that deuterium destruction is governed by low mass stars (since the gas is essentially trapped in these stars), whereas metallicity production (elements other than H and He) is governed by high mass stars, which, having short lifetimes, start rejection of enriched matter at high redshift. A weak destruction of deuterium is consequently not incompatible with a significant formation of heavy elements.

Assuming a given cosmic evolution of the star formation rate (SFR), the model follows the evolution of the baryons abundance in stars, in diffuse structures (interstellar medium, ISM) and in the intergalactic medium (IGM). The model includes a description of mass exchanges between the IGM and ISM (structure formation, galactic outflows), and between the ISM and the stellar component (star formation, stellar winds and supernova explosions). Once the cosmic SFR is specified, several quantities are obtained as a function of the redshift, namely the abundances of chemical elements, and more specifically deuterium. We consider for the present study the results of the best model described in Ref. Van14 , including a standard mode of Population II/I star formation between 0.1 and 100 . The initial mass function (IMF) slope is set to the Salpeter value, i.e., Sal55 ; Cha14 .

Figure 12 shows the evolution of D/H as a function of redshift, derived with the cosmic SFR shown in Figure 11 (solid black line). Black dotted curves correspond to our 2 BBN limits, whereas the red solid line corresponds to the mean. The resulting astration factor is =1.1. This cosmic evolution is in overall agreement with the observed values detailed above. Note, however, that a tension exists between the BBN value and the high redshift measurements in the sense that the latter seem somewhat high. However, note that, due to the extreme fragility of deuterium its potential destruction depends on many parameters of the star-formation history and, in particular, the IMF parameters. We illustrate the impact of the variation of the mass lower limit of the IMF. The dotted red curve corresponds to a lower mass limit of 0.5 instead of 0.1 (solid red line). In this case the astration factor is =1.15. Finally, we consider an extreme case by adding an intermediate mass star formation component (between 2–8 ) (dashed red line), leading to an astration factor of =1.25. Even when considering these extreme modifications of the IMF, the maximum variation is only 14% which is not a large uncertainty compared to the error bars on observational data. Recently, Prodanovic, Steigman and Fields Pro10b have studied the deuterium evolution and its link with structure formation. They show that a steady infall rate is required to reconcile the model with observations. Our cosmological model is in agreement with this result since in a hierarchical formation of structures, primordial gas is continuously accreted into structures throughout the evolution. We also find, as these authors that 80% of the initial interstellar gas is never processed within stars.

Since the paper is devoted to deuterium study we do not consider other elements.. Obviously, deuterium destruction can lead to production but while we have D/H cosmological observations, we have only /H local observations (in the galactic disk) and no constraints at high redshift. Chiappini et al. Chi02 and Vangioni–Flam et al. Van03 have analyzed the behavior of in the Galaxy. The best observational constraints come from Bania, Rood & Balser Ban02 . These data are concentrated in the galactic disk only, i.e. at high metallicity relative to the solar value ([O/H] between -0.6 and 0.2). Vangioni-Flam et al. have shown that it is not possible to obtain a strong constraint on the baryon density using due to this limited range of metallicity in the sample and to the limited understanding of the chemical and stellar evolution of this isotope.

To conclude, our results are in agreement with the observations, implying that the mean abundance of deuterium has only been reduced by a factor of 1.1 to 1.25 since its formation during BBN. There is, however, a tension between our BBN D/H value and the high- measurements, leaving little room for a high astration factor. In any case, due to the low abundance of the primordial D/H value and the local observed constraints, the astration factor, , is less than 1.25.

## Vii The lithium–deuterium anti–correlation

In spite of various efforts, there is still a factor of 3.5 (Table 3), between the predicted and observed lithium primordial abundances. Most proposed solutions to the lithium problem lead to an increase of the deuterium production Oli12 ; Coc14a ; Kus14 ; they are now strongly constrained by deuterium observations. We discuss here the relation between lithium (Be+Li) destruction and overproduction.

At CMB deduced baryonic density, is produced indirectly by He(Be, where Be will much later decay to , while Be is destroyed by Be(n,p)Li(p,He. The solutions to the lithium problem generally rely on an increased late time neutron abundance Alb12 ; Ren88 ; Jed04 to boost Be destruction through the Be(n,p)Li(p,He channel. These extra neutrons, inevitably, also boost the D and H production through the H(n,H and He(n,p)H channels, respectively Kus14 . For instance, Fig. 13 displays the effect of the injection of thermalized neutrons at a constant rate (as in Albornoz Vásquez et al. Alb12 ).

Even though other destruction channels by other thermalized ^{4}^{4}4As opposed to non–thermalized particles
originating from the decay of massive relic particles during BBN (see e.g., Ref. Cyb13 ).
particles (p, d, t, and )
have been investigated Cha11 , neutron capture remains the
only efficient one.
Neutron induced reaction rates vary far less with temperature compared to charged-particle induced reaction rates at BBN
temperatures. For instance, a factor of for the Be(p,B is to be compared to a factor 2 for the
Be(n,p)Li reaction, when the temperature drops from 1.0 to 0.1 GK.
This is obviously directly linked to Coulomb barrier penetration. After 700 s,
when the Be abundance has reached its maximum (Fig. 13), the temperature is lower than 0.5 GK.
This low temperature prevents charged particle reactions to be efficient, as it can be seen in Fig. 13 by the flat (dashed lines)
final evolution of the abundances.
(In any case, the Be(p,B reaction has such a low –value (0.1375 MeV), that the reverse reaction,
photo disintegration, is so effective that it prevents Be destruction by proton capture.)
This could only be circumvented by the presence of strong resonances in some charged particle induced
reactions, like Be(d,p)2.
However, experiments have not supported such a nuclear physics solution involving
new conventional neutron sources Coc12b or new resonances Kir11 ; Ham13 in reactions with
charged particle, suggesting non–conventional neutron sources as a solution.

Figure 14 is adapted from Fig. 9 in Ref. Coc14a summarizing the results of different models than include late time neutron injection aiming at reducing the Be+Li production, but at the expense of overproduction. These models involve mirror neutrons, dark matter decay or annihilation as extra neutron sources. The Figure also displays the results of a BBN calculation allowing for a coupled variation of constants as described in Ref. Coc12a , where the extra neutron source arises from the change induced in the H(n,)H rate.

Figure 13 shows that Be increased destruction by neutrons is counterbalanced by increased production. First, with a higher H abundance, due to the He(n,p)H increased efficiency, the H(Li channel, normally negligible at , may become dominant. Second, the Be increased destruction by Be(n,p)Li, produces that is not efficiently destroyed anymore by Li(p,He, because of the low temperature. This explains that when increasing the rate of injection of extra neutrons, the Li=Be+ abundance reaches a minimum as seen in Fig. 14 (or in Fig. 7 of Ref. Coc14a ). This lower limit on Li/H, due to the transition from Be to Li direct production (Figs. 13–14), can be compared to the minimum in Li/H as a function of .

Figure 13 also shows that the effect of Be destruction by extra neutrons is efficient only below 0.5 GK when the charged particle reactions are inefficient due to the Coulomb barrier and the low abundance of reactants. If we call the extra, late time, neutron overabundance, the extra destruction of Be is given by

(7) |

where the ’s are mole fractions, the baryonic density and the thermonuclear reaction rate. We neglect the He(Be channel at those low temperatures because of the Coulomb barrier (Fig. 13).

At the same time, an extra deuterium production from the n(p,)d reaction is unavoidable, so that

(8) |

Again, we neglect charged particle reactions and the He(n,p)H neutron drain, as we do not need to calculate . Putting Eqs. (7) and (8) together, one obtains

(9) |

Since, the ratio of Be(n,p)Li to H(n,H thermonuclear reaction rates is almost constant (6–8 for 0.11 GK), one can deduce that

(10) |

which is displayed (red dashed line) in Fig. 14. This is an approximation, as long as , but it gives a qualitative explanation for the lithium–deuterium anti–correlation in most models aiming at solving the lithium overproduction. Depending on the precise timing of neutron injection, and hence, of the temperature, the efficiency of neglected reactions [e.g., d+d and Li(p,He] need to be considered Kus14 , but which would increase the complexity of the calculations. Here, we only considered thermalized neutron injection, first, because thermalization of high energy neutrons is fast Alb12 . Second, it was already noted by Kusakabe et al. Kus14 that the ratio of H+n to Be+n cross sections increases with energy, rendering less efficient the injection of non–thermalized neutrons for destroying Be without overproducing deuterium, when compared with thermal neutron injection.

## Viii Conclusions

It has long been recognized that the agreement between BBN predictions and observations is quite satisfactory except for lithium. Now that the observations of D/H in cosmological clouds, thought to be representative of the primordial abundance, have reached a high precision Coo14 , nuclear cross sections of all reactions leading to deuterium destruction should be determined with an equivalent precision DiV14 , i.e. at the percent level. To improve the precision on the three main reaction rates governing deuterium destruction, we have re-evaluated existing experimental data, using –factors provided by ab initio theoretical models. This is at variance with most other reaction rate evaluations that rely on phenomenological approaches (e.g., polynomial or R–matrix) fits of experimental data. We paid special attention to systematic uncertainties in selection of the data sets to be considered. In particular, for the d(d,n)He and d(d,p)H –factors, we take advantage of the mostly model independent ratio of cross sections to evaluate experimental results. The three reaction rates are found to be slightly higher than the previous R–matrix analysis of DAACV Des04 , leading to a small but significant decrease of the D/H prediction, . We calculate the cosmological evolution of deuterium from BBN until present, within a hierarchical model of structure formation and obtained a value of D/H = , at the redshift ( 3.0) of the observed cosmological clouds. This predicted value is compatible at the level with the observations Coo14 .

Deuterium predictions are also highly important, in relation with the lithium problem. Most solutions involve a Be destruction by a late time neutron injection. We show that this is unavoidably correlated with an increase of the deuterium production by the effect of the H(n,H reaction. Hence, most solutions to the lithium problem are now severely constrained, also by deuterium precise observations.

Further progress in the domain are expected from future experiments, in particular, concerning the
d(p,He reaction, planned to be measured at the BBN energies, at the Gran Sasso National Laboratory (LUNA),
but also, possibly, from improved theory ^{5}^{5}5
A very recent, improved ab initio calculation of the d(p,He –factor Mar15 have lead to a reduced D/H prediction of
compared to the previous value of Planck15 )
..
Keeping systematic uncertainties on nuclear cross section measurements
at the percent level, is indeed a challenge. These systematics can be evaluated by comparing independent
measurements, with the help of theoretical –factors when data sets span different energy ranges.

###### Acknowledgements.

This work made in the ILP LABEX (under reference ANR-10-LABX-63) was supported by French state funds managed by the ANR within the Investissements d’Avenir programme under reference ANR-11-IDEX-0004-02 and by the ANR VACOUL, ANR-10-BLAN-0510.## Appendix A Normalization procedure

In other evaluations NACRE ; Des04 ; Cyb04 , the –factor shapes (polynomial, R–matrix) were fitted on experimental data. Here, we assume that theory () gives a good description of the shape but may need a scaling factor (i.e. ). Calculations involve an energy dependence, and an overall normalization. The energy dependence is essentially provided by the Coulomb functions, and is therefore more reliable than the normalization, which is more sensitive to the model assumptions. Accordingly, we introduce a possible scaling of the theoretical calculations with a renormalization factor , close to unity. By minimizing the ,

(11) |

where and are the experimental –factors and associated uncertainties, one obtains the scale factor best value () and associated uncertainty (for a given experiment labelled for future use) that are given by Eqs. (12) and (13) [Eqs. (6) and (7) in Cyb01 ]

(12) |

(13) |

This takes well into account the effect of statistical uncertainties but leaves aside systematic uncertainties, in particular on the normalization. Systematics coming from different normalizations, from one data set to the other, will play an essential role. It is usually recommended PDG , for incompatible data sets, to inflate the classical error [Eq. (13)], by a factor of so that the final reduced equals 1 (. This method has however been questioned. We present in this section several options that have been considered, apply them to experimental data sets in the following sections, and compare the results.

### a.1 The global data fit option

Cyburt, Fields & Olive Cyb01 used this procedure to re–normalize the NACRE –factor fits, this is identical to our goal except that we use theoretical –factor instead.

The value of the normalization factor, , is again given by Eq. (12) [their Eq. (6)], except that now the sum runs over all the data points () within all the data sets.

### a.2 The joint statistical and normalization fit option

The method from D’Agostini DAg94 has been used, in particular, by Serpico et al. Ser04 for BBN reaction rate evaluations, Cyburt and Davids Cyb08a , and Schürmann et al. Sch12 , for the He(Be, and C(O, reactions respectively. In addition to the parameters of the theoretical model (a single one, , in our case), scale factors, , with associated errors, , affect all data sets. Note that the , for each experiment, are not always available. In that case, Serpico et al. Ser04 write ”Whenever only a total error determination is available for a certain experiment, that error is used instead of , and an upper limit on the scale error is estimated as max[].” The to be minimized has the form:

(16) |

Hence, the experimental values are scaled by factors that are constrained by the experimental uncertainty on normalization while the theoretical function is also scaled by the factor we want to determine. The minimization procedure is no longer trivial and we have to perform it numerically with the use of MINUIT MINUIT94 . It is no longer possible to give an analytical expression of the uncertainty. The uncertainty adopted by Serpico et al. Ser04 is more empirical: ”The overall scale error used in the analysis was chosen to be equal to the lowest experimentally determined for that reaction. …..It was added in quadrature to the statistical error in the fits….”. Cyburt and Davids Cyb08a used the Markov Chain Monte Carlo technique to calculate the uncertainties. Note that in our case, the situation is simpler since, we do not fit the shape of the –factor, which comes from theory, but only the normalization factor, and we use the error on the parameter [Eq. (16)] provided by MINUIT MINUIT94 .

### a.3 Our method

From an other point of view, the recommended normalization factor can be given by the weighted average of the obtained by Eqs. (12) and (13) from different experiments (labelled )

(17) |

Working out the algebra, starting from Eqs. (12) and (13), one finds that this equation is just a re–phrasing of Eq. (14) when no extra normalization error, , has to be introduced. On the contrary, it is easily introduced in Eq. (17) by the change

(18) |

The error on would normally be given by

(19) |

We considered the possibility of applying the Cyburt et al. rescaling Cyb01 ; Cyb04 by to Eq. (19), together with an extra , in order to obtain a weighted empirical variance

(20) |

(Apart from the N/N-1 factor, this is just Eq. (21) of Cyburt Cyb04 .) This has the advantage of converging to the empirical variance [] when the ’s are all equal or favoring the contributions of the terms with lower ’s if it is not the case. If systematics are negligible, the central values would be the same, but Eq. (15) would give a larger uncertainty. However, we found that, after introducing the normalization error with Eq. (18), the reduced chi–square was always close to unity. Accordingly, we found unnecessary to inflate the uncertainty by a factor.

## Appendix B The D(p,He data

The –factor is related to the total cross section by

(21) |

(MeV and barn units). In the following, we detail the experimental data that we considered in this evaluation, in general taken from published tables, but when scanned from a figure, we provide here tables of the extracted numerical values.

The Casella et al. (LUNA) data Cas02 comes from their Table I where “only accidental errors are reported: the systematic uncertainties ranged from 3.6% (E = 21.23 keV, highest measured energy) to 5.3% (E = 2.52 keV, lowest measured energy) and are negligible in comparison with the accidental errors”. We hence adopt = 0.045 as an average systematic uncertainty.

It was found, that NACRE overlooked the overall scaling factor of 1.37 Sch96 missing in the Schmidt et al. Sch95 data. Here, we follow DAACV and use instead (multiplied by ) from Table II in Schmidt et al. Sch97 . The uncertainties reported in their Table I are statistical only. The systematic error is evaluated in their § II.H to be = 0.09 and is used in their Fig. 13. In our Table 4 we present the –factor used in our work.

(MeV) | (nb) | (eV.b) |
---|---|---|

0.0100 | 7.300.38 | 0.2425 0.0125 |

0.0167 | 30.79 0.84 | 0.2740 0.0075 |

0.0233 | 73.26 1.38 | 0.3452 0.0065 |

0.0300 | 122.8 1.9 | 0.3974 0.0061 |

0.0367 | 176.0 2.3 | 0.4452 0.0057 |

0.0433 | 222.4 3.4 | 0.4738 0.0072 |

0.0500 | 252.6 3.4 | 0.4744 0.0064 |

### b.1 The Ma et al. data

(MeV) | (eV.b) |
---|---|

0.075 | 0.685 0.070 |

0.107 | 0.708 0.068 |

0.133 | 0.956 0.084 |

0.173 | 1.26 0.10 |

The systematic uncertainty is estimated to be = 0.09, but may be already included in the error bars of their Fig. 9.

NACRE used data form Wölfli et al. Wol67 (in German), presumably scanned from their Fig. 6 or from Fig. 1 in Ref. Wol66 which is a comparison with theory. The lowest energy data point reported by NACRE at is probably an error since the experiment explored the = 2.–12. MeV range. Only three data points are found below = 2. MeV, the limit of the theoretical calculation. In addition, the evaluation of the systematic uncertainty is difficult from the publications.

NACRE, NACRE–II NACRE2 and Serpico et al. Ser04 use the data from Geller et al. Gel67 . However, as shown in their Fig. 2 Gel67 , and text, all data are normalized to the Gunn–Irving theoretical cross section Gun51 at = 3.07 MeV. Therefore, we do not use these data for normalization.

NACRE used cross–section data for photodisintegration, scanned from Fig. 2 in Warren et al War63 , and applied detailed balance theorem to obtain the following d(p,He cross section:

(MeV) | (b) | (eV.b) |
---|---|---|

0.637 | 3.2 0.3 | 5.7 0.5 |

1.465 | 5.3 0.9 | 15. 2. |

1.575 | 5.2 0.6 | 16. 2. |

There is no information on systematic uncertainty.

NACRE used experimental data from Griffith et al Gri62 ; Gri63 , presented here in Table 7 . The low energy –factor was obtained by scanning Fig. 6 in Ref. Gri63 while the high energy cross section is taken from Table I in Ref. Gri62 . Data between parenthesis are relative measurements and are not used in the fits.

(MeV) | (b) | (eV.b) |
---|---|---|

0.015 | 0.039 0.008 | 0.43 0.09 |

0.016 | 0.044 0.011 | 0.42 0.10 |

0.018 | 0.052 0.009 | 0.39 0.07 |

0.020 | 0.063 0.014 | 0.38 0.09 |

0.022 | 0.077 0.011 | 0.39 0.06 |

0.023 | 0.086 0.011 | 0.41 0.05 |

0.024 | 0.092 0.016 | 0.41 0.07 |

0.026 | 0.12 0.02 | 0.47 0.07 |

0.027 | 0.12 0.02 | 0.44 0.06 |

0.028 | 0.12 0.2 | 0.44 0.07 |

0.031 | 0.15 0.02 | 0.47 0.06 |

0.032 | 0.14 0.02 | 0.41 0.07 |

0.183 | 0.97 0.11 | 1.18 0.13 |

0.387 | (2.20 0.25) | (3.13 0.36) |

0.503 | 2.71 0.13 | 4.28 0.21 |

0.657 | 3.50 0.38 | 6.25 0.68 |

1.167 | (4.92 0.50) | (12.16 1.24) |

DAACV quote the data from Bailey et al. Bai70 . Table 8 displays our own scanned data from Fig. 1 of that Bailey et al. article Bai70 . These data have nothing in common with the presumably erroneous data displayed in Fig. 1.a of DAACV.

(MeV) | (b) | (eV.b) |
---|---|---|

0.067 | 0.43 0.06 | 0.66 0.09 |

0.092 | 0.67 0.07 | 0.88 0.09 |

0.260 | 1.55 0.11 | 1.98 0.14 |

0.311 | 1.77 0.12 | 2.36 0.15 |

0.342 | 2.01 0.11 | 2.75 0.14 |

0.411 | 2.26 0.11 | 3.29 0.16 |

0.432 | 2.34 0.08 | 3.47 0.12 |

0.462 | 2.46 0.10 | 3.75 0.15 |

0.528 | 2.69 0.12 | 4.34 0.19 |

0.660 | 3.31 0.19 | 5.93 0.33 |

0.727 | 3.43 0.190 | 6.45 0.35 |

NACRE–II used the data from Table 3 in Bystritsky et al. Bys08b (copied in Table 9); the systematic uncertainty, is less than 8%.

(keV) | (eV.b) |
---|---|

8.07 0.27 | 0.237 0.071 |

9.27 0.33 | 0.277 0.064 |

9.87 0.40 | 0.298 0.065 |

### b.2 Miscellaneous

Unlike DAACV, we do not use the Skopik et al. Sko79 data because the energies are well above the limits of our adopted theoretical model.

## Appendix C The D(d,n)He and D(d,p)H data

In the range of energy we are interested in, all experiments have measured both of these reaction cross sections. This allows us to perform a test to evaluate the coherence of the data because the ratio of these cross section is essentially governed by the Coulomb interaction, and as such is weakly dependent of the nuclear model. We take as reference the recent ab initio calculation of Arai et al. Ara11 . As mentioned before, the theoretical energy dependence is more accurate than the normalization. Therefore the ratio of both cross sections is expected to be quite reliable, and offers a good test of the various experimental data.

The curve in Fig. 15 represents the ratio of theoretical cross sections compared with the data sets to be discussed below. Confidence in this theoretical shape is reinforced by fact that the most recent directly measured Leo06 and higher energy Sch72 experimental data sets follow precisely (except for a few data points) this curve. This can hardly be accidental: even though the model, because of limitations on angular momentum, underestimates the high energy absolute cross–sections, the ratio is well reproduced, suggesting that it is indeed independent of the nuclear matrix elements. Obviously, this comparison is of no use to identify systematic errors in normalization which would affect both reactions in the same way. However, deviations from the theoretical ratio may indicate normalization errors in at least one of the reaction.

The –factor is related to the total cross section by:

(22) |

In the following subsections, we detail the experimental data that we considered in this evaluation.

NACRE and DAACV used the –factor and uncertainties from Schulte et al. Sch72 , but the theoretical model does not reach their energy range, and we have to put it aside. This is unfortunate since the ratio of cross sections follow the theoretical ratio (Coulomb only) in Fig. 15, suggesting that the normalizations are correct, or at least differ by the same constant factor.

We considered the Trojan Horse data Tum14 , but the evolution of the ratio of cross sections (Fig. 15) is completely different from the theoretical one. We are not able to tell whether this discrepancy is experimental or is due to the theoretical model used to extract the two-body cross section from the three-body experimental data. However, we note that the discrepancies seen in Fig. 15, and between Figs. 6 and 7 are of the order of 10%. It is not acceptable for the precision required here, but it would be excellent, compared with other indirect methods.

The Leonard et al. Leo06 data are taken from their Table III, while their Table V provides the error matrix and quote a 2%1% scale error, and are reported here in Table 10

d(d,n)He | d(d,p)H | |||
---|---|---|---|---|

(MeV) | (mb) | (keV.b) | (mb) | (keV.b) |

0.0561 | 21.07 0.92 | 78.18 3.41 | 19.77 0.85 | 73.36 3.15 |

0.0864 | 33.03 1.01 | 83.63 2.56 | 29.55 0.88 | 74.82 2.23 |

0.1164 | 43.13 0.96 | 92.17 2.05 | 37.65 0.82 | 80.46 1.75 |

0.1573 | 56.01 1.33 | 107.69 2.56 | 45.77 1.06 | 88.00 2.04 |

0.1896 | 62.60 1.12 | 116.06 2.08 | 53.09 0.94 | 98.43 1.74 |

0.2351 | 69.55 1.04 | 126.72 1.89 | 58.47 0.80 | 106.53 1.46 |

0.2786 | 80.22 1.18 | 146.62 2.16 | 68.02 0.96 | 124.32 1.75 |

0.3231 | 84.34 1.59 | 156.29 2.95 | 74.55 1.07 | 138.15 1.98 |

Table 4 in Greife et al. Gre95 provides –factors for the d(d,p)H reaction below 15 keV, however, their Fig. 1.a shows an important screening effect. Consequently, we do not use 15 keV data for this reaction. We only use the –factor (Table 11) calculated from the cross sections found in their Table 2 Gre95 whose uncertainties include systematics (solid angles (3%), gas pressure (1%), and calorimetric measurements (1%) [caption of Table 2]). Since they dominate over statistical errors, we adopt = 0.033.

d(d,n)He | d(d,p)H | |||
---|---|---|---|---|

(keV) | (mb) | (keV.b) | (mb) | (keV.b) |

14.85 | 1.21 0.05 | 62.08 2.57 | 1.21 0.07 | 62.08 3.59 |

24.66 | 5.00 0.20 | 68.67 2.75 | 4.70 0.20 | 64.55 2.75 |

39.62 | 12.60 0.50 | 73.21 2.91 | 11.80 0.50 | 68.56 2.91 |

41.00 | 13.20 0.50 | 72.92 2.76 | 12.70 0.60 | 70.16 3.31 |

50.00 | 17.90 0.70 | 75.89 2.97 | 16.30 0.60 | 69.10 2.54 |

52.00 | 18.10 0.70 | 73.21 2.83 | 16.70 0.60 | 67.55 2.43 |

76.00 | 29.80 1.00 | 83.01 2.79 | 26.60 0.90 | 74.10 2.51 |

102.00 | 39.40 1.40 | 89.99 3.20 | 34.40 1.20 | 78.57 2.74 |

128.00 | 49.00 1.70 | 100.61 3.49 | 42.20 1.60 | 86.64 3.29 |

The Krauss et al. Kra87 experiments took place in Münster ( keV) and at Bochum ( keV). We exclude the 15 keV data, because of screening (see above). Table 2 in Krauss et al. Kra87 provides –factors and statistical uncertainties. A normalization error of 6.4% comes from an absolute d(d,p)H cross section measurement at = 49.67 keV, to which a 5% error due to variations in the alignment of beam and jet target profiles has to be added for the the Münster data. NACRE added quadratically all these errors. Hence, we use = 0.064 for the Bochum data and, following the authors, = 0.082 for the Münster data.

NACRE used the –factor and uncertainties (0.4–4%) from Brown & Jarmie 1990 Bro90 Table II. However, NACRE did not take into account the 1.3% ”scale error”, dominated by the uncertainty in the p +d elastic calibration leading to = 0.013.

The article from the “The First Research Group, The First Research Division” first , written in chinese, reports on the d(d,p)H and d(d,n)He cross section data, from = 15 to 150 keV, which are available in exfor and have been used in Refs. Ser04 ; Tum14 . The ratio of cross sections, shown in Fig. 15, follows closely and scatters evenly around the theoretical curve. However, because of our inability to understand the core of the article, and in particular the error budget, we considered these results in our evaluation, but did not use them in our fit.

Preston et al. Pre54 , measured the d(d,p)H and d(d,n)He cross sections, from = 156 to 466 keV. The ratio of cross section is in good agreement with theory (Fig. 15).

We list here data which may have been used in other evaluations but that we put aside in our evaluation. Bystritsky et al. Bys08a quoted in NACRE-II are not considered as they explore a range of energy where screening is important; its study being the goal. The same ( keV) applies to Belov et al. Bel90 data obtained from exfor . Hofstee et al. (a conference proceeding) Hof01 , also quoted in NACRE-II is not considered either (two data points with large () uncertainty). Davidenko et al. Dav57 quote a 20% uncertainty on d(d,n)He. Data from Ganeev et al. Gan57 can be obtained from exfor . There is an overlap in energy range for the d(d,n)He and d(d,p)H cross section measurements but the energy steps are different. Hence, we plotted in Fig. 15 the ratio between interpolated experimental values and experimental values. The resulting values show a large scatter (8%) w.r.t. the theoretical curve. In McNeill and Keyser McN51 , it is stated (p. 605) that “In addition, errors in calibration and measurement, amounting to a maximum possible value of 20 percent, must be considered.”, we do not include these data in our fit. Arnold et al. Arn54 , provide d(d,n)He and d(d,p)H cross section data from = 13. to 113. keV with a detailed error analysis. Unfortunately, as can be seen in Fig. 15, their ratio is too small by 7%. This is apparently due to an systematic error in the d(d,n)He data (Fig. 4).

## Appendix D Tabulated reaction rates

d(p,He | d(d,n)He | d(d,p)H | ||||

T (GK) | rec. rate | rec. rate | rec. rate | |||

0.001 | 4.815 | 1.038 | 1.142 | 1.011 | 1.173 | 1.011 |

0.002 | 6.409 | 1.038 | 5.470 | 1.011 | 5.609 | 1.011 |

0.003 | 4.525 | 1.038 | 3.021 | 1.011 | 3.092 | 1.011 |

0.004 | 4.896 | 1.038 | 3.732 | 1.011 | 3.814 | 1.011 |

0.005 | 2.444 | 1.038 | 2.212 | 1.011 | 2.257 | 1.011 |

0.006 | 8.086 | 1.038 | 8.546 | 1.011 | 8.707 | 1.011 |

0.007 | 2.078 | 1.038 | 2.505 | 1.011 | 2.549 | 1.011 |

0.008 | 4.499 | 1.038 | 6.066 | 1.011 | 6.164 | 1.011 |

0.009 | 8.619 | 1.038 | 1.278 | 1.011 | 1.297 | 1.011 |

0.010 | 1.506 | 1.038 | 2.424 | 1.011 | 2.458 | 1.011 |

0.011 | 2.450 | 1.038 | 4.237 | 1.011 | 4.290 | 1.011 |

0.012 | 3.767 | 1.038 | 6.936 | 1.011 | 7.016 | 1.011 |

0.013 | 5.531 | 1.038 | 1.077 | 1.011 | 1.088 | 1.011 |

0.014 | 7.816 | 1.038 | 1.600 | 1.011 | 1.615 | 1.011 |

0.015 | 1.070 | 1.038 | 2.291 | 1.011 | 2.310 | 1.011 |

0.016 | 1.425 | 1.038 | 3.179 | 1.011 | 3.202 | 1.011 |

0.018 | 2.366 | 1.038 | 5.667 | 1.011 | 5.698 | 1.011 |

0.020 | 3.659 | 1.038 | 9.310 | 1.011 | 9.343 | 1.011 |

0.025 | 8.753 | 1.038 | 2.504 | 1.011 | 2.502 | 1.011 |

0.030 | 1.701 | 1.038 | 5.301 | 1.011 | 5.276 | 1.011 |

0.040 | 4.476 | 1.038 | 1.568 | 1.011 | 1.549 | 1.011 |

0.050 | 8.915 | 1.038 | 3.369 | 1.011 | 3.307 | 1.011 |

0.060 | 1.510 | 1.038 | 6.013 | 1.011 | 5.868 | 1.011 |

0.070 | 2.302 | 1.038 | 9.527 | 1.011 | 9.246 | 1.011 |

0.080 | 3.265 | 1.038 | 1.390 | 1.011 | 1.343 | 1.011 |

0.090 | 4.392 | 1.038 | 1.912 | 1.011 | 1.837 | 1.011 |

0.100 | 5.676 | 1.038 | 2.513 | 1.011 | 2.404 | 1.011 |

0.110 | 7.109 | 1.038 | 3.190 | 1.011 | 3.039 | 1.011 |

0.120 | 8.685 | 1.038 | 3.938 | 1.011 | 3.737 | 1.011 |

0.130 | 1.040 | 1.038 | 4.753 | 1.011 | 4.493 | 1.011 |

0.140 | 1.224 | 1.038 | 5.631 | 1.011 | 5.304 | 1.011 |

0.150 | 1.420 | 1.038 | 6.568 | 1.011 | 6.165 | 1.011 |

0.160 | 1.628 | 1.038 | 7.559 | 1.011 | 7.072 | 1.011 |

0.180 | 2.076 | 1.038 | 9.691 | 1.011 | 9.011 | 1.011 |

0.200 | 2.565 | 1.038 | 1.200 | 1.011 | 1.110 | 1.011 |

0.250 | 3.941 | 1.038 | 1.842 | 1.011 | 1.682 | 1.011 |

0.300 | 5.505 | 1.038 | 2.555 | 1.011 | 2.309 | 1.011 |

0.350 | 7.225 | 1.038 | 3.318 | 1.011 | 2.974 | 1.011 |

0.400 | 9.076 | 1.038 | 4.119 | 1.011 | 3.663 | 1.011 |

0.450 | 1.104 | 1.038 | 4.946 | 1.011 | 4.371 | 1.011 |

0.500 | 1.310 | 1.038 | 5.792 | 1.011 | 5.089 | 1.011 |

0.600 | 1.748 | 1.038 | 7.517 | 1.011 | 6.543 | 1.011 |

0.700 | 2.212 | 1.038 | 9.260 | 1.011 | 8.001 | 1.011 |

0.800 | 2.700 | 1.038 | 1.100 | 1.011 | 9.448 | 1.011 |

0.900 | 3.207 | 1.038 | 1.272 | 1.011 | 1.087 | 1.011 |

1.000 | 3.729 | 1.038 | 1.442 | 1.011 | 1.228 | 1.011 |

1.250 | 5.093 | 1.038 | 1.850 | 1.011 | 1.565 | 1.011 |

1.500 | 6.522 | 1.038 | 2.235 | 1.011 | 1.882 | 1.011 |

1.750 | 8.000 | 1.038 | 2.595 | 1.012 | 2.181 | 1.012 |

2.000 | 9.517 | 1.038 | 2.932 | 1.012 | 2.461 | 1.012 |

2.500 | 1.265 | 1.038 | 3.546 | 1.013 | 2.976 | 1.013 |

3.000 | 1.587 | 1.038 | 4.093 |