1994/02/28 by J. L. Houser, Janet Houser, Scott C. Smith +2 · 1 citation
Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Classical mechanics #Gamma-ray bursts and supernovae #Gravitation #Gravitational collapse #Gravitational instability #Gravitational wave #Instability #Mechanics #Optics #Physics #Pulsars and Gravitational Waves Research #Radiation #Star (game theory) #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevlett.72.1314
published as Phys.Rev.Lett.72:1314-1317,1994 · 16 pages, LaTeX with REVTEX macros, reprints available - send mailing address to [email protected]. Published: PRL 72, 1314 (1994)
openalex publication_date 1994/02/28 · arxiv created 1994/09/27 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 \ensuremath∼4% of its mass and \ensuremath∼17% of its angular momentum. The gravitational radiation is calculated in the quadrupole approximation. For a mass M\ensuremath∼1.4M_\mathrm\ensuremath\bigodot and radius R\ensuremath∼10 km, the gravitational waves have frequency \ensuremath∼4 kHz and amplitude h\ensuremath∼2\ifmmode×\else\texttimes\fi10^\mathrm\ensuremath-22 at the distance of the Virgo Cluster. They carry off energy \ensuremathΔE/M\ensuremath∼0.1% and radiate angular momentum \ensuremathΔJ/J\ensuremath∼0.7%.