Abstract
Numerical stellar modeling dates back since at least 45 years, when the first generation of digital computers became available. By now, we have a reasonably good qualitative understanding of what is going on in the vast majority of the cases, and we also quantitatively know many details on simple stellar structures (even if the solar neutrino problem is always a warning to be frequently reminded). In the following, a short review of the basic problems with stellar modeling will be provided, in the attempt of convincing the reader that, switching from local stellar models to non-local, turbulent ones, will be a major, generational leap, which will greatly extend the boundaries of our quantitative understanding of stellar evolution
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© 1995 Springer Verlag
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Mazzitelli, I. (1995). What is wrong with stellar modeling. In: Koester, D., Werner, K. (eds) White Dwarfs. Lecture Notes in Physics, vol 443. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-59157-5_174
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DOI: https://doi.org/10.1007/3-540-59157-5_174
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