Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of (a) (magneto-)hydrodynamics, (b) energy generation due to nuclear reactions accomanying composition changes, (c) radiation transport, (d) thermodynamic properties (such as the equation of state of stellar matter).
CITATION STYLE
Thielemann, F. K., Hirschi, R., Liebendörfer, M., & Diehl, R. (2011). Massive stars and their supernovae. Lecture Notes in Physics, 812, 153–231. https://doi.org/10.1007/978-3-642-12698-7_4
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