Abstract
Herein, we present a theoretical study of how Fermi-surface distortion affects symmetric nuclear matter, pure neutron matter, and neutron-star matter. The results indicate that, for the binding energy of symmetric nuclear matter, the generally accepted value extracted from the Bethe-Weiz\acker mass formula for nuclei can constrain the degree of anisotropy because of Fermi-surface deformation $\ensuremath{\delta}\phantom{\rule{0.16em}{0ex}}\ensuremath{\lesssim}0.05$. The value of $\ensuremath{\delta}$ starts to affect the stiffness of the equation of state for symmetric nuclear matter and pure neutron matter when $\ensuremath{\delta}\phantom{\rule{0.16em}{0ex}}\ensuremath{\gtrsim}0.01$. Moreover, if the Fermi surface is distorted, the results indicate that neutron stars can be deformed into an oblate shape. This deformation depends on two factors: the stiffness of the corresponding equation of state and value of $\ensuremath{\delta}$. The corresponding deformation near the maximum neutron-star mass comes from the anisotropic pressure within these stars, which is caused by the distortion of Fermi surface predicted by the equation of state of the models.
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