A NEUTRON STAR COOLING CODE
This code is extremely robust, very fast (the whole cooling of an isolated neutron star from birth to freezing takes less than a minute even on a lousy laptop), and highly modular (which makes it easy to add new subroutines for new processes without major risks of screwing it up !). It can also handle “strange stars”, which have a huge density discontinuity between the quark matter and the covering thin baryonic crust.
Once given a star to cool, with all the wanted/necessary physics set up (several configuration files are provided as examples), and an initial temperature profile, the code solves the heat transport and energy balance equations, in whole GR. The result is a time sequence of temperature profiles (and, in particular, a Teff - age curve).
Several heating processes are included, and more can easily be incorporated. In particular it can evolve a star undergoing accretion with the resulting deep crustal heating, under a steady or time-variable accretion rate.
[Unpacking this archive will create a directory NSCool
with everything in it.
The subdirectory A_User_Guide contains the "User's Guide"]