<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi>Li</mml:mi><mml:mprescripts/><mml:none/><mml:mn>6</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo>)</mml:mo><mml:mmultiscripts><mml:mi>Be</mml:mi><mml:mprescripts/><mml:none/><mml:mn>7</mml:mn></mml:mmultiscripts></mml:mrow></mml:math>reaction rate in the light of the new data of the Laboratory for Underground Nuclear Astrophysics

We present new calculations of the astrophysical $S$ factor and reaction rate for the $^{6}\mathrm{Li}(p,\ensuremath{\gamma})^{7}\mathrm{Be}$ reaction at energies of 10 keV to 5 MeV in the framework of a modified potential cluster model with forbidden states, including low lying resonances. The astrophysical $S(E)$ factor is compared with the available experimental data and calculations done within different models. The results for the $S$ factor are in good agreement with the data set (for $E&lt;0.3$ MeV) and calculations (for $E&lt;0.6$ MeV) of the LUNA Collaboration [Phys. Rev. C 102, 052802(R) (2020)]. The recommended extrapolated zero value $S(0)$ turned out to be 101 eV b. Using the theoretical total cross sections, the $^{6}\mathrm{Li}(p,\ensuremath{\gamma})^{7}\mathrm{Be}$ capture reaction rate is calculated at temperatures ranging from $0.01{T}_{9}$ to $10{T}_{9}$ and compared with NACRE and NACRE II. Analytical expressions for the $S$ factor and reaction rate are given, and the effect of low-lying resonances on the reaction rate is estimated. We suggest updating the NACRE and NACRE II databases in light of the new LUNA data and present calculations.

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