L. De, . De-corot-dans-une-base-de-données-texte, X. Html, and C. , MySQL 23 spécifiquement dessinée pour les résultats de notre algorithme qui peutêtrepeutêtre consultée avec des routines PHP 24 programmées pour l'occasion. CoRoT génère un grand nombre de courbes (de l'ordre de 10000 par run) qui occupent une quantité importante d'espace de disque dur (80 GB pour un long run) ; des chiffres peu confortables. La base de données permet un accès rapide et fiablè a tous les paramètres d'un candidat ainsi que leur rangement en fonction des différents critères et la sortie de l'information dans plusieurs formats

. La-base-de-données-nécessite-quelque-développement-informatique, mais elle fait gagnerénormementgagnerénormement de temps et simplifie le traitement de l'information . L'expérience acquise dans l'´ elaboration de ces outils informatiques peut s'appliqueràappliquerà l'adaptation du catalogue de naines froides (Ultracool Dwarf Catalog, Martín et al. 2005) aux conditions de l'Observatoire Virtuel

&. Jordán and . Dvorak, LeséchellesLeséchelles de temps y impliquées sont trop longues pour les mesurer avec le satellite CoRoT, qui au maximum fournit jusqu'` a 150 jours d'observations ininterrompues . Néanmoins, ils existent encore des perturbationsàperturbationsà plus court terme, comme celles produites par les corps placés dans des orbites troyennes (Laughlin & Chambers, Agol et al. 2005) ou les effets dusàdusà la propagation du signaì a la vitesse de lalumì ere. 4.8.1 Les troyens Dans le système solaire ils existent les astero¨?desastero¨?des troyens, un ensemble de corps de faible masse dans les points de Lagrange L4 et L5 de l'orbite de Jupiter. Mais dans le domaine des exoplanètes on considère la formation et la stabilité de corps de masse planétaire dans les mêmes orbites (lire Ford & Gaudi 2006 et Dvorak et al. 2004 ainsi que les références y incluses). On peut estimer les perturbations que ces corps produiront sur le temps d'arrivée du, 2002.

. Irwin, offrent une excellente exposition du traitement de la mesure de ces différences, mais Scott (1940) offre un point de vue plus pratique. C'est la même idée que Woltjer (1922) a utilisé pour ressoudre le probì eme (posé par Hertzsprung 1922) d'analyser les signaux comme celles mesurés par Chandler (1892) On utilise toujours cette méthode pourétudierpourétudier les binaires, même si pour elles les périodes typiques sont plus grandes que dans le cas des planètes et si il faut considerer d'autres sources de perturbations, 1952.

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