Abstract
In this chapter the equations of stellar structure are introduced. Up-to-date descriptions of the most relevant microphysics needed to build reliable stellar configurations are also provided. These include the equation of state, nuclear reactions, opacities, and other less frequently discussed physical processes, such as diffusion and radiative levitation. The necessary numerical techniques currently employed to build evolutionary stellar models as well as the otherwise necessary boundary conditions needed to integrate the equations of stellar structure are also addressed. Finally, an overview of the current state-of-the-art modeling is given.
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Acknowledgements
This work was partially supported by AGAUR, by MCINN grant AYA2008–04211–C02–01, by the European Union FEDER funds, by the ESF EUROGENESIS project (grant EUI2009-04167), by AGENCIA: Programa de Modernización Tecnológica BID 1728/OC-AR, and by PIP 2008-00940 from CONICET.
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Garcı́a–Berro, E., Althaus, G.L. (2013). Stellar Structure. In: Oswalt, T.D., Barstow, M.A. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5615-1_1
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