Gravitational radiation from nonaxisymmetric instability in a rotating star

We present the first calculations of the gravitational radiation produced by nonaxisymmetric dynamical instability in rapidly rotating compact star. The star deforms into a bar shape, shedding ∼4% of its mass and ∼17% of its angular momentum. The gravitational radiation is calculated in the quadrupole approximation. For a mass M∼1.4${\mathit{M}}_{\mathrm{\odot }}$ and radius R∼10 km, the gravitational waves have frequency ∼4 kHz and amplitude h∼2×${10}^{\mathrm{-}22}$ at the distance of the Virgo Cluster. They carry off energy ΔE/M∼0.1% and radiate angular momentum ΔJ/J∼0.7%.