SMS Γ=4/3

Detail

In this case, the supermassive star is seeded with a poloidal dipole magnetic field that extends from the interior into the exterior. The stellar model is described by a polytropic equation of state (EOS) with $\Gamma=4/3$, corresponding to pure thermal radiation pressure support. This EOS is most appropriate for stars with mass $M \gtrsim 10^6 M_\odot$.