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Maximum gravitational-wave energy emissible in magnetar flares

Alessandra Corsi

Benjamin J. Owen

  • LIGO Laboratory, California Institute of Technology, MS 100-36, Pasadena, California 91125, USA

  • Center for Gravitational Wave Physics, Institute for Gravitation and the Cosmos, Department of Physics, The Pennsylvania State University, University Park, Pennsylvania 16802, USA and Max Planck Institut für Gravitationsphysik (Albert Einstein Institut), Callinstr. 38, 30167 Hannover, Germany

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Phys. Rev. D 83, 104014 – Published 5 May, 2011

DOI: https://doi.org/10.1103/PhysRevD.83.104014

Abstract

Recent searches of gravitational-wave data raise the question of what maximum gravitational-wave energies could be emitted during gamma-ray flares of highly magnetized neutron stars (magnetars). The highest energies (∼1049  erg) predicted so far come from a model [K. Ioka, Mon. Not. R. Astron. Soc. 327, 639 (2001), http://adsabs.harvard.edu/abs/2001MNRAS.327..639I] 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 1048–1049  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.

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Phys. Rev. D 83, 104014– Published 5 May, 2011
  • Received 17 February 2011
Article part of CHORUS

© 2011 American Physical Society

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