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Journal Article

Maximum gravitational-wave energy emissible in magnetar flares

MPS-Authors
http://pubman.mpdl.mpg.de/cone/persons/resource/persons40530

Owen,  Benjamin J.
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

1102.3421
(Preprint), 367KB

PRD83_104014.pdf
(Any fulltext), 536KB

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There is no public supplementary material available
Citation

Corsi, A., & Owen, B. J. (2011). Maximum gravitational-wave energy emissible in magnetar flares. Physical Review D, 83(10): 104014. doi:10.1103/PhysRevD.83.104014.


Cite as: http://hdl.handle.net/11858/00-001M-0000-000F-0871-E
Abstract
Recent searches of gravitational-wave (GW) data raise the question of what maximum GW energies could be emitted during gamma-ray flares of highly magnetized neutron stars (magnetars). The highest energies (\sim 10^{49} erg) predicted so far come from a model [K. Ioka, Mon. Not. Roy. Astron. Soc. 327, 639 (2001)] in which the internal magnetic field of a magnetar experiences a global reconfiguration, changing the hydromagnetic equilibrium structure of the star and tapping the gravitational potential energy without changing the magnetic potential energy. The largest energies in this model assume very special conditions, including a large change in moment of inertia (which was observed in at most one flare), a very high internal magnetic field, and a very soft equation of state. Here we show that energies of 10^{48}-10^{49} erg are possible under more generic conditions by tapping the magnetic energy, and we note that similar energies may also be available through cracking of exotic solid cores. Current observational limits on gravitational waves from magnetar fundamental modes are just reaching these energies and will beat them in the era of advanced interferometers.