Neutron-star deformation due to anisotropic momentum distribution of neutron-star matter

R. Rizaldy, A. R. Alfarasyi, A. Sulaksono, T. Sumaryada

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4 Citations (Scopus)


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-Weizäcker mass formula for nuclei can constrain the degree of anisotropy because of Fermi-surface deformation δ 0.05. The value of δ starts to affect the stiffness of the equation of state for symmetric nuclear matter and pure neutron matter when δ 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 δ. 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.

Original languageEnglish
Article number055804
JournalPhysical Review C
Issue number5
Publication statusPublished - 26 Nov 2019


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