Quadrupole Moments of Rotating Neutron Stars

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© 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation William G. Laarakkers and Eric Poisson 1999 ApJ 512 282 DOI 10.1086/306732

0004-637X/512/1/282

Abstract

Numerical models of rotating neutron stars are constructed for four equations of state using the computer code RNS written by Stergioulas. For five selected values of the star's gravitational mass (in the interval between 1.0 and 1.8 solar masses) and for each equation of state, the star's angular momentum is varied from J=0 to the Keplerian limit J=Jmax. For each neutron star configuration, we compute Q, the quadrupole moment of the mass distribution. We show that for given values of M and J, |Q| increases with the stiffness of the equation of state. For fixed mass and equation of state, the dependence on J is well reproduced with a simple quadratic fit, Q≃ -aJ2/Mc2, where c is the speed of light and a is a parameter of order unity depending on the mass and the equation of state.

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10.1086/306732