Oscillatory properties of strange quark stars described by the vector MIT bag model
arXiv:2412.05752 · doi:10.1140/epjc/s10052-025-14224-8
Abstract
We investigated the radial and non-radial fundamental () mode oscillations of self-bound (quark) stars obtained after employing the Vector MIT (vMIT) bag model. Within this model, we computed the equation of state for strange quark matter satisfying thermodynamic consistency. This allowed us to obtain the corresponding behavior of the speed of sound, mass-radius relation, and gravitational redshift. In particular, our choice of = 0.30 fm produces masses and radii in agreement with recent astronomical data (e.g. from NICER and HESS J1731). In fact, we tested that variations of the remaining vMIT parameters slightly modify this conclusion. Then, we proceeded to compute the radial oscillation frequencies of the -mode, which is tightly connected to the dynamical stability of these compact stars. We found that increments of the parameter have a stabilizing property around the maximal-mass stars for a given stellar family. We also calculated the gravitational-wave frequencies of the non-radial -mode. Our results show that they are restricted to be in the range (1.6 - 1.8) kHz for high-mass stars and to (1.5 - 1.6) kHz for low-mass stars. Finally, we propose a universal relation between these frequencies and the square root of the average density. All these last results are important in distinguishing strange stars from ordinary neutron stars in future gravitational-wave detections coming from compact sources with activated non-radial modes.
arXiv comment6 Figures, 10 pages,
References in corpus (30)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- 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
- Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
- A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
- Towards gravitational-wave asteroseismology
- Science with the Einstein Telescope: a comparison of different designs
- A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437$\unicode{x2013}$4715
- Gravitational Wave asteroseismology revisited
- On the Sound Speed in Neutron Stars
- Phase transition effects on the dynamical stability of hybrid neutron stars
- Fundamental oscillation modes of neutron stars: validity of universal relations
- Equilibrium, radial stability and non-adiabatic gravitational collapse of anisotropic neutron stars
- General relativistic treatment of -mode oscillations of hyperonic stars
- Constraining color flavor locked strange stars in the gravitational wave era
- Constraining strangeness in dense matter with GW170817
- Modified MIT bag Models -- part I: Thermodynamic consistency, stability windows and symmetry group
- Radial oscillations of color superconducting self-bound quark stars
- Vacuum Nucleon Loops and Naturalness
- Modified MIT Bag Models -- part II: QCD phase diagram and hot quark stars
- Effects of the quark-hadron phase transition on highly magnetized neutron stars
- Effects of Dark Matter on -mode oscillations of Neutron Stars
- Gravitational Wave Signatures of Highly Magnetized Neutron Stars
- Can magnetic fields stabilize or destabilize twin stars?
- Could a slow stable hybrid star explain the central compact object in HESS~J1731-347?
- A Bayesian study of quark models in view of recent astrophysical constraints
- Imprints of the nuclear symmetry energy slope in gravitational wave signals emanating from neutron stars
- Extra dimensions' influence on the equilibrium and radial stability of strange quark stars
- The neutron star inner crust: an empirical essay
- QCD Phase Diagrams via QHD and MIT-Based Models