# The tidal deformability of an anisotropic compact star: Implications of GW170817

## TL;DR

This paper investigates how pressure anisotropy in neutron stars affects their tidal deformability and uses GW170817 data to constrain the extent of anisotropy, revealing that anisotropic models can reconcile certain equations of state with observations.

## Contribution

It demonstrates that pressure anisotropy can significantly reduce neutron star tidal deformability, allowing some EOSs to be consistent with GW170817 data that were previously ruled out under isotropic assumptions.

## Key findings

- Anisotropic pressure can reduce tidal deformability by 23-46%.
- Certain EOSs become viable with anisotropy that are incompatible under isotropy.
- Star radius constraints can exclude some EOSs despite anisotropic effects.

## Abstract

We use gravitational wave (GW) and electromagnetic (EM) observations of GW170817 to constrain the extent of pressure anisotropy in it. While it is quite likely that the pressure inside a neutron star is mostly isotropic, certain physical processes or characteristics, such as phase transitions in nuclear matter or the presence of strong magnetic fields, can introduce pressure anisotropy. In this work, we show that anisotropic pressure in neutron stars can reduce their tidal deformability substantially. For the anisotropy-pressure model of Bowers and Liang and a couple of relativistic EOSs -- DDH$\delta$ and GM1 -- we demonstrate that this reduction in spherical neutron stars with masses in the range of 1 to 2 $M_\odot$ can be 23% to 46%. This suggests that certain EOSs that are ruled out by GW170817 observations, under assumptions of pressure isotropy, can become viable if the stars had a significant enough anisotropic pressure component, but do not violate causality. We also show how the inference of the star radius can be used to rule out certain EOSs (such as GM1), even for high anisotropic pressure, because their radii are larger than what the observations find.