A Family of Gravitational Waveforms from Rapidly Rotating Neutron Stars
Dong Lai (Cornell)
TL;DR
This paper presents fitting formulae for gravitational waveforms emitted by rapidly rotating neutron stars as they evolve from axisymmetric to triaxial shapes, aiding gravitational wave detection efforts.
Contribution
It introduces new fitting formulae for modeling gravitational waveforms from evolving rapidly rotating neutron stars, enhancing waveform prediction accuracy.
Findings
Fitting formulae accurately model neutron star gravitational waveforms.
Waveform models cover evolution from axisymmetric to triaxial configurations.
Results improve gravitational wave detection and analysis capabilities.
Abstract
This note describes fitting formulae for the gravitational waveforms generated by a rapidly rotating neutron star (e.g., newly-formed in the core collapse of a supernova) as it evolves from an initial axisymmetric configuration toward a triaxial ellipsoid.
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
Taxonomy
TopicsPulsars and Gravitational Waves Research · Geophysics and Gravity Measurements · Geophysics and Sensor Technology