Use of o2scl on a hyperspherical shell neutron star about o2scl HOT 5 CLOSED

Dear Andrew, I made progress.  Please correct me if I am wrong. From the paper, I understand that the energy is potential energy.  I am modeling the process where the whole Neutron Star evaporates under Zero Gravity. My suspicion is that I have to add the energy released by neutron decay as kinetic energy transferred to electrons. So, I am changing those equations to reflect the extra thermal energy: to Would that be correct?  Of course, if this energy is the potential energy, I can just write another equation for the Kinetic energy and relate that to Temperature. Later, I will related this energy to temperature by I am not clear on the meaning of this energy.  Is this the energy per nucleon at density y.I supposed that to be the case, that is how I got the y**2 on the pressure. Thanks you in advance for your attention and guidance. Thanks, Marco On Tuesday, January 21, 2020, 03:51:28 PM EST, Andrew W. Steiner <[email protected]> wrote: P=0 only at zero density, and in isospin-symmetric matter at the nuclear saturation density. Inside a neutron star, the pressure must always be positive (and must increase with decreasing radius). — You are receiving this because you authored the thread. Reply to this email directly, view it on GitHub, or unsubscribe.