Normal and quasinormal modes of holographic multiquark star

The quadrupole normal-mode oscillation frequency fn of a multiquark star are computed for n = 1-5. At the transition from low to high density multiquark in the core region, the first two modes jump to larger values, a distinctive signature of the presence of the high-density core. When the star oscillation couples with spacetime, gravitational waves (GW) will be generated and the star will undergo damped oscillation. The quasinormal modes (QNMs) of the oscillation are computed using two methods, direct scan and WKB, for QNMs with small and large imaginary parts respectively. The small imaginary QNMs have frequencies 1.5-2.6 kHz and damping times 0.19-1.7 secs for a multiquark star with mass M = 0.6-2.1 M circle dot (solar mass). The WKB QNMs with large imaginary parts have frequencies 5.98-9.81 kHz and damping times 0.13-0.46 ms for M similar or equal to 0.3-2.1 M circle dot. They are found to be the fluid f - modes and spacetime curvature w - modes, respectively.

Automated summary

The quadrupole normal mode oscillation frequency fn of multiquark stars is calculated for n = 1-5. The transition from low to high density multiquark in the core region results in a jump in the first two modes, indicating the presence of a high-density core. When the star's oscillation couples with spacetime, gravitational waves (GW) are generated and the star undergoes damped oscillation. The computation of quasinormal modes (QNMs) using two methods, direct scan and WKB, reveals small imaginary QNMs with frequencies of 1.5-2.6 kHz and damping times of 0.19-1.7 secs, as well as large imaginary QNMs with frequencies of 5.98-9.81 kHz and damping times of 0.13-0.46 ms.