Effects of finite sizes of atomic nuclei on shear modulus and torsional oscillations in neutron stars
arXiv:2209.05416 · doi:10.1093/mnras/stac2615
Abstract
The shear modulus of neutron star matter is one of the important properties for determining torsional oscillations in neutron stars. We take into account the effects of finite sizes of spherical nuclei on the shear modulus and examine the frequencies of crustal torsional oscillations. The shear modulus decreases owing to the finite-size effect, which in turn decreases the frequencies of torsional oscillations. In particular, the finite-size effect becomes more crucial for oscillations with a larger azimuthal quantum number and for neutron star models with a weaker density dependence of nuclear symmetry energy. In practice, when one identifies the quasi-periodic oscillations from a neutron star, where the magnetic effect is negligible, with crustal torsional oscillations, the finite-size effect can be more significant at frequencies higher than Hz.
Accepted for publication in MNRAS
References in corpus (20)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Multi-messenger Observations of a Binary Neutron Star Merger
- PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
- A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
- A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
- Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
- Torsional Oscillations of Relativistic Stars with Dipole Magnetic Fields
- Signatures of hadron-quark mixed phase in gravitational waves
- Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology
- Constraints on Neutron Star Crusts From Oscillations in Giant Flares
- Dependence of outer boundary condition on protoneutron star asteroseismology with gravitational-wave signatures
- Universal relation for supernova gravitational waves
- Probing nuclear bubble structure via neutron star asteroseismology
- Elastic properties of polycrystalline dense matter
- Determination of properties of protoneutron stars toward black hole formation via gravitational wave observations
- Neutron star asteroseismology and nuclear saturation parameter
- Probing crustal structures from neutron star compactness
- Gravitational wave asteroseismology on cooling neutron stars
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