A New Equation of State for Astrophysical Applications
نویسندگان
چکیده
The equation of state (EoS) of hot and dense matter is an essential ingredient in many astrophysical models, e.g. in supernovae and compact star calculations. The thermodynamical properties and the composition of the matter have to be known in a wide range of density (10−8 n/nsat 10), temperature (0 ≤ T 50 MeV) and proton fraction (0 ≤ Yp 0.6). Despite the large number of available EoS from various theoretical models, there are few [1, 2, 3] that are practically applied in astrophysical model calculations. Many studies focus only on certain aspects in a limited range of n, T and Yp and the relevant thermodynamical quantities are not readily available in a simple form for astrophysicists. In addition, the model parameters are not well constrained by the experimental data that are nowadays available, the description is partially not selfconsistent or too simplified. These deficiencies call for a development of an improved EoS that is practical and easy for the application in astrophysics.
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