Probing dense matter in neutron stars with axial w-modes

Abstract

We study the problem of extracting information about composition and equation of state of dense matter in neutron star interior using axial w-modes. We determine complex frequencies of axial w-modes for a set of equations of state involving hyperons as well as Bose-Einstein condensates of antikaons adopting the continued fraction method. Hyperons and antikaon condensates result in softer equations of state leading to higher frequencies of first axial w-modes than that of nuclear matter case, whereas the opposite happens in case of damping times. The presence of condensates may lead to the appearance of a new stable branch of superdense stars beyond the neutron star branch called the third family. The existence of same mass compact stars in both branches are known as neutron star twins. Further investigation of twins reveal that first axial w-mode frequencies of superdense stars in the third family are higher than those of the corresponding twins in the neutron star branch.

arXiv commentLaTeX; 23 pages including two tables and 11 figures

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Cited by in corpus (7)

• Phenomenological Relations for Axial Quasi-normal Modes of Neutron Stars with Realistic Equations of State
• Exotic matter influence on the polar quasi-normal modes of neutron stars with equations of state satisfying the $2M_{\odot }$ constraint
• Can magnetic fields stabilize or destabilize twin stars?
• Signatures of strangeness in neutron star merger remnants
• Non-radial pulsations of gravitationally coupled two-fluid neutron stars in general relativity
• Axial $w$-modes of anisotropic neutron stars
• Influence of hyperon-hyperon interaction on the properties of neutron stars