Role of dense matter in tidal deformations of inspiralling neutron stars and in gravitational waveforms with unified equations of state

The role of dense-matter properties in the tidal deformability of a cold nonaccreted neutron star is further investigated. Using the set of Brussels-Montreal unified equations of state, we have computed the gravitoelectric Love numbers $k_{\ell }$ and the gravitomagnetic Love numbers $j_{\ell }$ up to $\ell =5$. Their relative importance and their sensitivity to the symmetry energy and the neutron-matter stiffness are numerically assessed. Their impact on the phase of the gravitational-wave signal emitted by binary neutron star inspirals is also discussed.

Figure 1

Gravitoelectric Love number $k_3$ as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 2

Gravitoelectric Love number $k_4$ as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 3

Gravitoelectric Love number $k_5$ as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 4

Gravitomagnetic Love number $j_2$ for a static fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 5

Gravitomagnetic Love number $j_3$ for a static fluid as a function of NS mass computed with the Brussels-Montreal unified EoSs.

Figure 6

Gravitomagnetic Love number $j_4$ for a static fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 7

Gravitomagnetic Love number $j_5$ for a static fluid as a function of NS mass computed with the Brussels-Montreal unified EoSs.

Figure 8

Gravitomagnetic Love number $j_2$ for an irrotational fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 9

Gravitomagnetic Love number $j_3$ for an irrotational fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 10

Gravitomagnetic Love number $j_4$ for an irrotational fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 11

Gravitomagnetic Love number $j_5$ for an irrotational fluid as a function of NS mass computed with Brussels-Montreal unified EoSs.

Figure 12

Gravitoelectric Love numbers $k_{\ell }$ as a function of the gravitational mass $M$ for a NS with and without crust. Calculations were performed using the Brussels-Montreal nuclear energy-density functional BSk24.

Figure 13

Gravitomagnetic Love numbers $j_{\ell }$ as a function of the gravitational mass $M$ for a NS (irrotational fluid) with and without crust. Calculations were performed using the Brussels-Montreal nuclear energy-density functional BSk24.

Figure 14

Contribution from the gravitoelectric Love number $k_2$ to the phase (20) of the gravitational-wave signal from a binary NS inspiral as a function of the frequency $f$ for different EoSs. Calculations were performed for NSs with equal masses of 1.4 $M_{\odot }$.

Figure 15

Same as Fig. 14 for the gravitoelectric Love number $k_3$.

Figure 16

Same as Fig. 14 for the gravitoelectric Love number $k_4$.

Figure 17

Same as Fig. 14 for the gravitoelectric Love number $k_5$.

Figure 18

Contribution from the gravitomagnetic Love number $j_2$ to the phase (21) of the gravitational-wave signal from a binary NS inspiral as a function of the frequency $f$ for different EoSs. Calculations were performed for an irrotational fluid and NSs with equal masses of 1.4 $M_{\odot }$.

Figure 19

Contribution from the gravitoelectric Love number $k_2$ to the phase (20) of the gravitational-wave signal from a binary NS inspiral as a function of the frequency $f$ for different NS masses. Calculations were performed using the unified EoS BSk24.

Figure 20

Same as Fig. 19 for the gravitoelectric Love number $k_3$.

Figure 21

Same as Fig. 19 for the gravitoelectric Love number $k_4$.

Figure 22

Same as Fig. 19 for the gravitoelectric Love number $k_5$.

Figure 23

Contribution from the gravitomagnetic Love number $j_2$ to the phase (21) of the gravitational-wave signal from a binary NS inspiral as a function of the frequency $f$ for different NS masses. Calculations were performed using the unified EoS BSk24 for an irrotational fluid.

Figure 24

Dimensionless gravitoelectric tidal deformability coefficients as a function of the gravitational mass $M$ of a NS. Results obtained without crust are indistinguishable from those with crust. Calculations were performed using the Brussels-Montreal nuclear energy-density functional BSk24.

Figure 25

Dimensionless gravitomagnetic tidal deformability coefficients as a function of the gravitational mass $M$ of a NS (irrotational fluid). Results obtained without crust are indistinguishable from those with crust. Calculations were performed using the Brussels-Montreal nuclear energy-density functional BSk24.