2019/01/31 by Sebastian H. Völkel, Sebastian H Völkel, Kostas D. Kokkotas +1 · 15 citations
Engineering · Physics and Astronomy · #Asteroseismology #Astrophysical Phenomena and Observations #Compact star #Coordinate system #Geophysics and Sensor Technology #Inverse #Inverse problem #Metric (unit) #Neutron star #Pulsars and Gravitational Waves Research #Spectrum (functional analysis) #WKB approximation #gr-qc
paper · pdf · doi:10.1088/1361-6382/ab186e
published in Classical and Quantum Gravity 36(11), 115002 (IOP Publishing)
arxiv created 2019/01/31 · openalex created_date 2019/02/21 · openalex publication_date 2019/04/11 · arxiv updated 2019/05/22 · openalex updated_date 2026/08/05
Abstract In this work we revisit axial perturbations of spherically symmetric and non-rotating neutron stars. Although it has been object of many studies, it still offers new insights that are of potential interest for more realistic scenarios or in the study exotic compact objects, which have drawn much attention recently. By using WKB theory, we first derive a new Bohr–Sommerfeld rule that allows to investigate the quasi-normal mode spectrum and address the inverse spectrum problem. The pure analytical treatment of the wave equation is rather involved, because it requires the solution of the TOV equations and the non-trivial tortoise coordinate transformation depending on the underlying space-time. Therefore we provide an easy way to construct potentials that simplifies the analytical treatment, but still captures the relevant physics. The approximated potential can be used for calculations of the axial perturbation spectrum. These results are also useful in the treatment of the inverse problem. We demonstrate this by reconstructing the time–time component of the metric throughout the star and constraining the equation of state in the central region. Our method also provides an analytical explanation of the empirically known asteroseismology relation that connects the fundamental QNM and radius of a neutron star with its compactness.