Gravitational wave asteroseismology for low-mass neutron stars

Abstract

The fundamental ($f$-) mode gravitational waves from cold low-mass neutron stars are systematically studied with various equations of state (EOSs) characterized by the nuclear saturation parameters, especially focusing on the phenomena of the avoided crossing with the first pressure ($p_1$-) mode. We find that the $f$-mode frequency and the average density for the neutron star at the avoided crossing can be expressed as a function of the parameter, $\eta$, which is the specific combination of the nuclear saturation parameters. Owing to these relations, we can derive the empirical formula expressing the $f$-mode frequency for a low-mass neutron star, whose central density is larger than that for the neutron star at the avoided crossing, as a function of $\eta$ and the square root of the stellar average density, $x$. On the other hand, we also derive the empirical formula expressing the $f$-mode frequency for a neutron star, whose central density is less than that for the neutron star at the avoided crossing, as a function of $x$ independently of the adopted EOS. Furthermore, adopting the empirical formula of $x$ as a function of $\eta$ and $u_c$, which is the ratio of the stellar central density to the saturation density, we can also rewrite our empirical formula for the $f$-mode frequency to a function of $\eta$ and $u_c$. So, by observing the $f$-mode gravitational wave from a low-mass neutron star, whose mass or gravitational redshift is known, one could evaluate the values of $\eta$ and $u_c$, which enables us to severely constrain the EOS for neutron star matter.

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Cited by in corpus (19)

• Neutron star asteroseismology and nuclear saturation parameter
• Neutron star mass formula with nuclear saturation parameters for asymmetric nuclear matter
• Gravitational wave asteroseismology on cooling neutron stars
• Estimating the nuclear saturation parameter via low-mass neutron star asteroseismology
• Stability of the protoneutron stars toward black hole formation
• Universality in supernova gravitational waves with proto-neutron star properties
• Long-term gravitational wave asteroseismology of supernova: from core collapse to 20 seconds postbounce
• Emergence of new oscillation modes in dark matter admixed neutron stars
• Shear and interface modes in neutron stars with pasta structures
• Shear oscillations in neutron stars and the nuclear symmetry energy
• Probing the impact of Delta-Baryons on Nuclear Matter and Non-Radial Oscillations in Neutron Stars
• Neutron star mass formula with nuclear saturation parameters
• Accuracy of one-dimensional approximation in neutron star quasi-normal modes
• Universal relation involving fundamental modes in two-fluid dark matter admixed neutron stars
• Gravitational wave asteroseismology of accreting neutron stars in a steady state
• Effects of multidimensional treatment of gravity in simulations on supernova gravitational waves
• Universal relations between the quasinormal modes of neutron stars and magnetic tidal deformability
• Universality of dual mass-scaled fundamental modes in two-fluid neutron stars with mirror dark matter
• The $g$-mode frequencies in cold neutron stars and nuclear saturation parameters