اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدAstrophysical S factor and rate of $^{7}{rm Be}(p, gamma)^{8}{rm B}$ direct capture reaction in a potential model
58
0
0.0
(
0
)
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
The astrophysical $^7{rm Be}(p, gamma)^8{rm B}$ direct capture process is studied in the framework of a two-body single-channel model with potentials of the Gaussian form. A modified potential is constructed to reproduce the new experimental value of the $S$-wave scattering length and the known astrophysical $S$ factor at the Gamow energy, extracted from the solar neutrino flux. The resulting potential is consistent with the theory developed by Baye [Phys. Rev. C {bf 62} (2000) 065803] according to which the $S$-wave scattering length and the astrophysical $S$ factor at zero energy divided by the square of ANC are related. The obtained results for the astrophysical $S$ factor at intermediate energies are in good agreement with the two data sets of Hammache {it et al.} [Phys. Rev. Lett. {bf 86}, 3985 (2001); {it ibid.} {bf 80}, 928 (1998)]. Linear extrapolation to zero energy yields $ S_{17}(0) approx (20.5 pm 0.5) , rm eV , b $, consistent with the Solar Fusion II estimate. The calculated reaction rates are substantially lower than the results of the NACRE II collaboration.
قيم البحث
اقرأ أيضاً
The astrophysical $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$ and $^{3}{rm H}(alpha, gamma)^{7}{rm Li}$ direct capture processes are studied in the framework of the two-body model with the potentials of a simple Gaussian form, which describe correctly the
phase-shifts in the s-, p-, d-, and f-waves, as well as the binding energy and the asymptotic normalization constant of the ground $p_{3/2}$ and the first excited $p_{1/2}$ bound states. It is shown that the E1-transition from the initial s-wave to the final p-waves is strongly dominant in both capture reactions. On this basis the s-wave potential parameters are adjusted to reproduce the new data of the LUNA collaboration around 100 keV and the newest data at the Gamov peak estimated with the help of the observed neutrino fluxes from the Sun, $S_{34}$(23$^{+6}_{-5}$ keV)=0.548$pm$0.054 keV b for the astrophysical S-factor of the capture process $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$. The resulting model describes well the astrophysical S-factor in low-energy Big Bang nucleosynthesis region of 180-400 keV, however has a tendency to underestimate the data above 0.5 MeV. Two-body potentials, adjusted on the properties of the $^7$Be nucleus, $^3{rm He}+alpha$ elastic scattering data and the astrophysical S-factor of the $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$ direct capture reaction, are able to reproduce the properties of the $^7$Li nucleus, the binding energies of the ground 3/2$^-$ and first excited 1/2$^-$ states, and phase shifts of the $^3 {rm H}+alpha$ elastic scattering in partial waves. Most importantly, these potential models can successfully describe both absolute value and energy dependence of the existing experimental data for the mirror astrophysical $^{3}{rm H}(alpha, gamma)^{7}{rm Li}$ capture reaction without any additional adjustment of the parameters.
Astrophysical $S$ factors and reaction rates of the direct radiative capture processes $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$ and $^{3}{rm H}(alpha,gamma)^{7}{rm Li}$, as well as the primordial abundance of the $^{7}{rm Li}$ element, are estimated in
the framework of a modified two-body potential model. It is shown that suitable modification of phase-equivalent $alpha-^{3}{rm He}$ potentials in the $d$ waves can improve the description of the astrophysical $S$ factor for the direct $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$ radiative capture reaction at energies above 0.5 MeV. An estimated $^{7}{rm Li/H}$ abundance ratio of $(4.89pm 0.18 )times 10^{-10}$ is in very good agreement with the recent measurement of $(5.0pm 0.3) times 10^{-10}$ by the LUNA collaboration.
The ${^3{rm He}}(alpha,gamma){^7{rm Be}}$ and ${^3{rm H}}(alpha,gamma){^7{rm Li}}$ astrophysical $S$ factors are calculated within the no-core shell model with continuum using a renormalized chiral nucleon-nucleon interaction. The ${^3{rm He}}(alpha,
gamma){^7{rm Be}}$ astrophysical $S$ factors agree reasonably well with the experimental data while the ${^3{rm H}}(alpha,gamma){^7{rm Li}}$ ones are overestimated. The seven-nucleon bound and resonance states and the $alpha+{^3{rm He}}/{^3{rm H}}$ elastic scattering are also studied and compared with experiment. The low-lying resonance properties are rather well reproduced by our approach. At low energies, the $s$-wave phase shift, which is non-resonant, is overestimated.
The reaction rates of the direct astrophysical capture processes $^{3}{rm He}(alpha, gamma)^{7}{rm Be}$ and $^{3}{rm H}(alpha,gamma)^{7}{rm Li}$, as well as the abundance of the $^{7}{rm Li}$ element are estimated in the framework of a two-body poten
tial model. The estimated $^{7}{rm Li/H}$ abundance ratio of $^{7}{rm Li/H}=(5.07pm 0.14 )times 10^{-10}$ is in a very good agreement with the recent measurement $^{7}{rm Li/H}=(5.0pm 0.3) times 10^{-10}$ of the LUNA collaboration.
At the long-wavelength approximation, electric dipole transitions are forbidden between isospin-zero states. In an $alpha+n+p$ model with $T = 1$ contributions, the $alpha(d,gamma)^6$Li astrophysical $S$-factor is in agreement with the experimental d
ata of the LUNA collaboration, without adjustable parameter. The exact-masses prescription used to avoid the disappearance of $E1$ transitions in potential models is not founded at the microscopic level.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
