Abstract
The development of a self-consistent theoretical description of the internal structure of stars, and the consequent construction of models which trace evolutionary behaviour, represents one of the major achievements of twentieth-century astrophysics. Most studies have centred on intermediate- and high-mass stars, with little consideration of M dwarfs with masses below 0.6 M⊙. In part, this reflects the availability of more precise observational constraints, and also the greater analytic tractability in modelling higher-mass stars. Recently, however, the lower main sequence has attracted more attention, with a series of detailed models extending past the hydrogen-burning limit to the boundary between low-mass brown dwarfs and giant planets.
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Reid, I.N., Hawley, S.L. (2000). The structure, formation and evolution of low-mass stars and brown dwarfs. In: New Light on Dark Stars. Astronomy and Planetary Sciences. Springer, London. https://doi.org/10.1007/978-1-4471-3663-7_3
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