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, hydrogène en fusion, lorsque l'on s'approche du point d'inversion entre les zones en contraction et en dilatation où la variation du moment d'inertie est nulle. Ainsi, pour un modèle donné, le taux d'extraction du moment cinétique en fonction du temps dans les régions en contraction est dominé par les régions

, Pour un modèle d'une masse donnée, la variation locale du moment d'inertie est de plus en plus importante au cours de l'évolution dans les régions qui sont progressivement accrétées dans le coeur d'hélium inerte, et un gradient de variation temporelle du moment d'inertie se met en place entre le centre et les régions nouvellement accrétées au cours de l'évolution sur la branche des géantes rouges (Fig 8.3). Cela signifie que le taux de moment cinétique à extraire en fonction du temps pour conserver un profil de rotation

, Les modèles mettent en avant une différence de comportement de l'évolution de la variation locale du moment d'inertie entre les modèles de M < 2.2 M ? et M ? 2.2 M ? : la variation temporelle du moment d'inertie des régions situées dans le coeur d'hélium inerte augmente d'environ un ordre de grandeur le long de la branche des géantes rouges pour les étoiles de M < 2.2 M ? , alors qu'elle diminue d'environ un ordre de grandeur dans ces régions pour les

, On observe également que la différence de variation du moment d'inertie entre la zone autour de la couche d'hydrogène en fusion et le coeur d'hélium augmente au cours de l'évolution mais diminue avec la masse. Pour le premier modèle sur la branche des géantes rouges, cette différence passe de trois ordres de grandeur pour une étoile de 1 M ? à un ordre de grandeur pour une étoile de 2.5 M ? ; pour le dernier modèle, elle passe de huit ordres de grandeur pour une étoile de 1 M ? à trois ordre de grandeur pour une étoile de 2.5 M ? (Fig 8.3). Cela signifie que, Cela signifie qu'en supposant un profil de rotation constant dans le coeur en fonction du temps, le taux d'extraction du moment cinétique en fonction du temps augmente dans le coeur d'hélium inerte de manière comparable au cours de l'évolution sur la branche des géantes rouges pour les étoiles de M < 2

, Pour les modèles de masses comprises entre 1 et 2.2 M ? , on remarque qu'à un moment de l'évolution la variation temporelle du moment d'inertie devient moins importante au niveau de la base de la couche d'hydrogène en fusion, avant de recommencer à augmenter (Fig. 8.3). Cette inversion dans l'évolution de la variation du moment d'inertie de la base de la couche d'hydrogène en fusion n'est pas visible pour une étoile de 2.5 M ? . Elle survient entre le troisième et le quatrième modèle, On peut noter une caractéristique intéressante au cours de l'évolution sur la branche des géantes rouges

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