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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Probing neutron star structure via f-mode oscillations and damping in dynamical spacetime models

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Rosofsky, Shawn G. [1, 2] ; Gold, Roman [3, 4, 5, 6] ; Chirenti, Cecilia [7] ; Huerta, E. A. [2, 8] ; Miller, M. Coleman [9, 3]
Total Authors: 5
[1] Univ Illinois, Dept Phys, Urbana, IL 61801 - USA
[2] Univ Illinois, NCSA, Urbana, IL 61801 - USA
[3] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 - USA
[4] Univ Maryland, Dept Phys, College Pk, MD 20742 - USA
[5] Goethe Univ Frankfurt, Inst Theoret Phys, Max von Laue Str 1, D-60438 Frankfurt - Germany
[6] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5 - Canada
[7] Univ Fed ABC, Ctr Math Computat & Cognit, BR-09210580 Santo Andre, SP - Brazil
[8] Univ Illinois, Dept Astron, Urbana, IL 61801 - USA
[9] Univ Maryland, Dept Astron, College Pk, MD 20742 - USA
Total Affiliations: 9
Document type: Journal article
Source: Physical Review D; v. 99, n. 8 APR 15 2019.
Web of Science Citations: 3

Gravitational wave and electromagnetic observations can provide new insights into the nature of matter at supranuclear densities inside neutron stars. Improvements in electromagnetic and gravitational wave sensing instruments continue to enhance the accuracy with which they can measure the masses, radii, and tidal deformability of neutron stars. These better measurements place tighter constraints on the equation of state of cold matter above nuclear density. In this article, we discuss a complementary approach to get insights into the structure of neutron stars by providing a model prediction for nonlinear fundamental eigenmodes (f modes) and their decay over time, which are thought to be induced by time-dependent tides in neutron star binaries. Building on pioneering studies that relate the properties of f modes to the structure of neutron stars, we systematically study this link in the nonperturbative regime using models that utilize numerical relativity. Using a suite of fully relativistic numerical relativity simulations of oscillating Tolman-Oppenheimer-Volkof stars, we establish blueprints for the numerical accuracy needed to accurately compute the frequency and damping times of f-mode oscillations, which we expect to be a good guide for the requirements in the binary case. We show that the resulting f-mode frequencies match established results from linear perturbation theory, but the damping times within numerical errors depart from linear predictions. This work lays the foundation for upcoming studies aimed at a comparison of theoretical models of f-mode signatures in gravitational waves, and their uncertainties with actual gravitational wave data, searching for neutron star binaries on highly eccentric orbits, and probing neutron star structure at high densities. (AU)

FAPESP's process: 15/50421-8 - Gravitational waves and neutron star oscillations
Grantee:Cecilia Bertoni Martha Hadler Chirenti
Support type: Regular Research Grants