Fig. 3: Effect of magnetization on stellar compactness.
From: Oscillations of highly magnetized non-rotating neutron stars
Compactness M/Rcirc is plotted against the magnetic to binding energy ratio \({{{{{{{\mathscr{H}}}}}}}}/{{{{{{{\mathscr{W}}}}}}}}\) of the NS model, where M is the gravitational mass and Rcirc is the circumferential radius. M/Rcirc remains nearly unchanged for \({{{{{{{\mathscr{H}}}}}}}}/{{{{{{{\mathscr{W}}}}}}}}\lesssim 1{0}^{-2}\) but decreases dramatically for \({{{{{{{\mathscr{H}}}}}}}}/{{{{{{{\mathscr{W}}}}}}}} > 1{0}^{-1}\). This agrees with the trends of \({f}_{{{{{{{{\rm{eig}}}}}}}}}({{{{{{{\mathscr{H}}}}}}}}/{{{{{{{\mathscr{W}}}}}}}})\) shown in Fig. 2 and reveals a correlation between eigenfrequencies of oscillation modes and stellar compactness for magnetized NSs.
