The superflares of soft Gamma-ray repeatres: giant quakes in solid quark stars?

R. X. Xu; D. J. Tao; Y. Yang

doi:10.1111/j.1745-3933.2006.00248.x

paper

The superflares of soft Gamma-ray repeatres: giant quakes in solid quark stars?

arXiv:astro-ph/0607106 · doi:10.1111/j.1745-3933.2006.00248.x

Abstract

Three times of supergiant flares from soft $γ$ -ray repeatres are observed, with typical released energy of $\sim 1 0^{44 - 47}$ erg. A conventional model (i.e., the magnetar model) for such events is catastrophic magnetism-powered instability through magnetohydrodynamic process, in which a significant part of short-hard $γ$ -ray bursts could also be the results of magnetars. Based on various observational features (e.g., precession, glitch, thermal photon emission) and the underlying theory of strong interaction (quantum chromodynamics, QCD), it could not be ruled out yet that pulsar-like stars might be actually solid quark stars. Strain energy develops during a solid star's life, and starquakes could occur when stellar stresses reach a critical value, with huge energy released. An alternative model for supergiant flares of soft $γ$ -ray repeatres is presented, in which energy release during a star quake of solid quark stars is calculated. Numerical results for spherically asymmetric solid stars show that the released gravitational energy during a giant quake could be as high as $1 0^{48}$ erg if the tangential pressure is slightly higher than the radial one. Difficulties in magnetar models may be overcome if AXPs/SGRs are accreting solid quark stars with mass $\sim (1 - 2) M_{⊙}$ .

Extensive discussions are presented, with a new figure added to show the change of mass and radius of accreting quark stars

The superflares of soft Gamma-ray repeatres: giant quakes in solid quark stars?

Abstract

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