Context : The analysis of solar-like oscillations for stars belonging to a binary system provides a unique opportunity to probe the internal stellar structure and to test our knowledge of stellar physics .
Such oscillations have been recently observed and characterized for the A component of the 70Â Ophiuchi system .

Aims : We determined the global parameters of 70Â Ophiuchi AB using the new asteroseismic measurements now available for 70~Oph~A and tested the input physics introduced in stellar evolution codes .

Methods : Three different stellar evolution codes and two different calibration methods were used to perform a comprehensive analysis of the 70Â Ophiuchi system .

Results : A model of 70Â Ophiuchi AB that correctly reproduces all observational constraints available for both stars is determined .
An age of 6.2 \pm 1.0 Gyr is found with an initial helium mass fraction Y _ { \mathrm { i } } = 0.266 \pm 0.015 and an initial metallicity ( Z / X ) _ { \mathrm { i } } = 0.0300 \pm 0.0025 when atomic diffusion is included and a solar value of the mixing-length parameter assumed .
A precise and independent determination of the value of the mixing-length parameter needed to model 70~Oph~A requires accurate measurement of the mean small separation , which is not available yet .
Current asteroseismic observations , however , suggest that the value of the mixing-length parameter of 70~Oph~A is lower or equal to the solar calibrated value .
The effects of atomic diffusion and of the choice of the adopted solar mixture were also studied .
We finally found that the different evolution codes and calibration methods we used led to perfectly coherent results .

Conclusions :