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In order to eciently use the recent astronomy high angular resolution techniques (Adaptive Optics and Interferometry) to correct the perturbed wavefront arriving at the telescope pupil, it is necessary to characterize a set of astroclimatic parameters. One of these is the wavefront coherence time AO. It is an integral parameter, dening the maximum temporal correlation of the perturbed wavefront and it depends on the optical turbulence C2 N(x;y;z )a nd the wind intensityj (x;y;z)j in the whole troposphere. In this paper we use an atmospheric non-hydrostatic model (Meso-NH) conceived to simulate the classical meteorological parameters (p, T and ) and adapted to simulate the optical turbulence (C2 N) to characterize theAO in a region of some kilometers around the astronomical site of San Pedro M artir (SPM) in Baja California (Mexico). We study the seasonal variability of the wind intensity in the whole atmosphere (20 km) above the SPM site during one year. We show that, using the C2 N proles simulated by Meso-Nh initialized with ECMWF (European Center for Medium Weather Forecasts) data, we obtain typical AO values in the V band ( =0 :5 m). We calculate the seasonal variability of the AO in SPM and also some preliminary results about the seasonal variability of C2 N. Moreover, we suggest a physical explication of these variabilities. Finally we investigate the possibility of forecasting AO.

Wavefront coherence time seasonal variability and forecasting at the San Pedro Mártir site