A non-local mixing-length theory able to compute core overshooting

机译：一种能够计算核心过冲的非局部混合长度理论

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Turbulent convection is certainly one of the most important and thorny issuesin stellar physics. Our deficient knowledge of this crucial physical processintroduces a fairly large uncertainty concerning the internal structure andevolution of stars. A striking example is overshoot at the edge of convectivecores. Indeed, nearly all stellar evolutionary codes treat the overshootingzones in a very approximative way that considers both its extent and theprofile of the temperature gradient as free parameters. There are only a fewsophisticated theories of stellar convection such as Reynolds stressapproaches, but they also require the adjustment of a non-negligible number offree parameters. We present here a theory, based on the plume theory as well ason the mean-field equations, but without relying on the usual Taylor's closurehypothesis. It leads us to a set of eight differential equations plus a fewalgebraic ones. Our theory is essentially a non-mixing length theory. Itenables us to compute the temperature gradient in a shrinking convective coreand its overshooting zone. The case of an expanding convective core is alsodiscussed, though more briefly. Numerical simulations have quickly improvedduring recent years and enabling us to foresee that they will probably soonprovide a model of convection adapted to the computation of 1D stellar models.

机译：湍流对流无疑是恒星物理中最重要和棘手的问题之一。我们对这一关键物理过程的认识不足，给恒星的内部结构和演化带来了相当大的不确定性。一个明显的例子是对流核心边缘的超调。实际上，几乎所有的恒星演化代码都以非常近似的方式对待过冲带，将其范围和温度梯度的分布都视为自由参数。只有少数复杂的恒星对流理论，例如雷诺应力法，但它们也需要调整大量自由参数。我们在此提出一种基于羽状理论以及平均场方程的理论，但不依赖于通常的泰勒闭合假设。它导致我们得到一组八个微分方程和几个代数方程。我们的理论本质上是非混合长度理论。使我们能够计算收缩对流岩心及其超调带中的温度梯度。还讨论了对流核心扩大的情况，尽管更简短。近年来，数值模拟已迅速改善，使我们可以预见，它们可能很快会提供一种适用于一维恒星模型计算的对流模型。

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Gabriel, M.; Belkacem, K.;
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A non-local mixing-length theory able to compute core overshooting

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