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La question de l'ajustement au mieux du modèle auto-régressif sur un modèle d'évolution de type Taylor pourrait alors être traitée de façon pertinente. A plus long terme, la démarche présentée dans ce mémoire -un formalisme d'état et un filtrage de Kalman -pour estimer la phase turbulente pourra être avantageusement mise en pratique dans au moins deux champs d'application : l'Optique Adaptative Haut Strehl et l'OAMC. L'OA Haut Strehl (Extreme AO ou XAO) s'insère dans une démarche de détection d'exoplanètes depuis le sol [MLB + 02]. On peut par coronographie éteindre une étoile pour laisser apparaître la planète qui gravite autour. Cela nécessite une grande efficacité du coronographe, ce qui signifie que le front d'onde qui lui arrive dessus doit être de variance spatiale la plus faible possible. Il s'agit d'utiliser pour cela une Optique Adaptative Classique optimisée le plus possible, c'està-dire dans laquelle on a minimisé tous les termes d'erreur. L'étoile de référence sera pour ce genre de systèmes relativement brillante, afin de limiter le bruit de photons. Cela signifie donc qu'il faudra, pour rester limité par ce bruit de photon et équilibrer le budget d'erreur, être beaucoup plus exigeant sur toutes les autres sources d'erreur et notamment prendre en compte le retard entre mesure et commande pour limiter l'erreur temporelle mais aussi l'aliasing, la scintillation, Le filtrage de Kalman tel qu ,
il faudra utiliser une commande optimale du type de celle que l'on propose dans ce mémoire, de même que pour les très grands télescopes (depuis les télescopes de 20 m jusqu'au télescope OWL de 100 m de l'ESO) à l'étude actuellement ,
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