2011/02/28 by Kazumi Kashiyama, Kunihito Ioka · 31 citations
Earth and Planetary Sciences · Physics and Astronomy · #Asteroseismology #Astronomy #Astrophysics #Einstein Telescope #Gamma-ray bursts and supernovae #Gravitational wave #Gravitational-wave observatory #High-pressure geophysics and materials #LIGO #Magnetar #Neutron star #Observatory #Physics #Pulsar #Pulsars and Gravitational Waves Research #Stars #astro-ph.HE #gr-qc
paper · pdf · doi:10.1103/physrevd.83.081302
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 83(8), 81302 (American Physical Society) · 4 pages, 3 figures, accepted for publication in PRD rapid communications
arxiv created 2011/03/28 · openalex publication_date 2011/04/13 · arxiv updated 2015/04/23 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Magnetic flares and induced oscillations of magnetars (supermagnetized neutron stars) are promising sources of gravitational waves (GWs). We suggest that the GW emission, if any, would last longer than the observed x-ray quasiperiodic oscillations (X-QPOs), calling for longer-term GW analyses lasting a day to months, compared to current searches' durations. Like the pulsar timing, the oscillation frequency would also evolve with time because of the decay or reconfiguration of the magnetic field, which is crucial for the GW detection. With the observed GW frequency and its time-derivatives, we can probe the interior magnetic field strength of \ensuremath∼1016 G and its evolution to open a new GW asteroseismology with the next generation interferometers like the advanced laser interferometer gravitational wave observatory, the advanced Virgo gravitational wave detector at the European Gravitational Observatory, the Large-scale cryogenic gravitational wave telescope, and the Einstein telescope.