Anisotropic pressure effect on central EOS of PSR J0740+6620 in the light of dimensionless TOV equation

Abstract

It is generally agreed upon that the pressure inside a neutron star is isotropic. However, a strong magnetic field or superfluidity suggests that the pressure anisotropy may be a more realistic model. We derived the dimensionless TOV equation for anisotropic neutron stars based on two popular models, namely the BL model and the H model, to investigate the effect of anisotropy. Similar to the isotropic case, the maximum mass $M_{max}$ and its corresponding radius $R_{Mmax}$ can also be expressed linearly by a combination of radial central pressure $p_{rc}$ and central energy density ${\epsilon }_c$, which is insensitive to the equation of state (EOS). We also found that the obtained central EOS would change with different values of ${\lambda }_{BL}$ (${\lambda }_H$), which controls the magnitude of the difference between the transverse pressure and the radial pressure. Combining with observational data of PSR J0740+6620 and comparing to the extracted EOS based on isotropic neutron star, it is shown that in the BL model, for ${\lambda }_{BL}$ = 0.4, the extracted central energy density ${\epsilon }_c$ changed from 546 -- 1056 MeV/fm${}^3$ to 510 -- 1005 MeV/fm${}^3$, and the extracted radial central pressure $p_{rc}$ changed from 87 -- 310 MeV/fm${}^3$ to 76 -- 271 MeV/fm${}^3$. For ${\lambda }_{BL}$ = 2, the extracted ${\epsilon }_c$ and $p_{rc}$ changed to 412 -- 822 MeV/fm${}^3$ and 50 -- 165 MeV/fm${}^3$, respectively. In the H model, for ${\lambda }_H$ = 0.4, the extracted ${\epsilon }_c$ changed to 626 -- 1164 MeV/fm${}^3$, and the extracted $p_{rc}$ changed to 104 -- 409 MeV/fm${}^3$. For ${\lambda }_H$ = 2, the extracted ${\epsilon }_c$ decreased to 894 -- 995 MeV/fm${}^3$, and the extracted $p_{rc}$ changed to 220 -- 301 MeV/fm${}^3$.

Comments: 19 pages, 8 figures