Phys. Rev. D 58, 024012 (1998) [5 pages]Relativistic formalism for computation of irrotational binary stars in quasiequilibrium statesReceived 22 January 1998; published 24 June 1998 We present relativistic hydrostatic equations for obtaining irrotational binary neutron stars in quasiequilibrium states in the 3+1 formalism. The equations derived here are different from those previously given by Bonazzola, Gourgoulhon, and Marck, and have a simpler and more tractable form for computation in numerical relativity. We also present hydrostatic equations for computation of equilibrium irrotational binary stars in the first post-Newtonian order. © 1998 The American Physical Society URL:
http://link.aps.org/doi/10.1103/PhysRevD.58.024012
DOI:
10.1103/PhysRevD.58.024012
PACS:
04.25.Nx, 97.80.Gm
|
|
About | Terms and Conditions | Subscriptions | Search | Help
Use of the American Physical Society websites and journals implies that the user has read and agrees to our Terms and Conditions and any applicable Subscription Agreement. Physical Review®, Physical Review Letters®, Reviews of Modern Physics®, and Physical Review Special Topics® are trademarks of the American Physical Society.