Hadronic Stars Research Articles

Hadron Star Models

The properties of fully relativistic rotating hadron star models are discussed using models based on recently developed equations of state. All of these stable neutron star models are bound with binding energies as high as ∼ 25%. During hadron star formation, much of this energy will be released. The consequences, resulting from the release of this energy, are examined.

Equation of state of the perfect Fermi-gas

The equation of state of the perfect relativistic Fermi-gas is implicity given by the three Fermi- Jüttner integrals for the pressure p, the kinetic energy density u, and the number density n, respectively. A quick computer program is presented which calculates these integrals with a precision of 10-7 for the whole space of states, as necessary for astrophysical calculations on hot neutron or hadron stars.