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Neutron capture data on intermediate mass nuclei are of key importance tonucleosynthesis in the weak component of the slow neutron capture processes,which occurs in massive stars. The ($n,\gamma$) cross section on $^{70}$Ge,which is mainly produced in the $s$~process, was measured at the neutrontime-of-flight facility n_TOF at CERN. Resonance capture kernels weredetermined up to 40~keV neutron energy, and average cross sections up to300~keV. Stellar cross sections were calculated from $kT=5$~keV to $kT=100$ keVand are in very good agreement with a previous measurement by Walter and Beer(1985), and recent evaluations. Average cross sections are in agreement withWalter and Beer (1985) over most of the neutron energy range covered, whilebeing systematically smaller for neutron energies above 150~keV. We havecalculated isotopic abundances produced in $s$-process environments in a 25solar mass star for two initial metallicities (below solar, and close tosolar). While the low metallicity model reproduces best the solar systemgermanium isotopic abundances the close to solar model shows a good globalmatch to solar system abundances between mass numbers A=60-80.

Measurement of the $^{70}$Ge($n,\gamma$) cross section up to 300~keV at the CERN n_TOF facility