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The maximum mass of differentially rotating neutron stars

Published online by Cambridge University Press:  30 September 2008

A. Oscoz ,
E. Mediavilla ,
M. Serra-Ricart ,
M. Ansorg ,
D. Gondek-Rosińska ,
L. Villain  and
M. Bejger
M. Ansorg
Affiliation:
Max-Planck-Institut f¨ur Gravitationsphysik, Albert-Einstein-Institut, 14476 Golm, Germany
D. Gondek-Rosińska
Affiliation:
Institute of Astronomy, University of Zielona G´ora, Lubuska 2, 65-265 Zielona G´ora, Poland; e-mail: dorota.gondek@obspm.fr
L. Villain
Affiliation:
LUTH, Observatoire de Paris, Universit´e Paris 7, Place Jules Janssen, 92195 Meudon Cedex, France Departament de Fisica Aplicada, Universitat d’Alacant, Apartat de correus 99, 03080 Alacant, Spain
M. Bejger
Affiliation:
CAMK, PAN, Bartycka 18, Warsaw, Poland
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Abstract

Binary neutron star merger lead to the formation of amassive, rapidly and differentially rotating neutron star (or astrange star) or to the prompt collapse to a black hole. The maximummass of a differentially rotating remnant is crucial for distinguishingbetween these two final objects. We study the effect of differentialrotation on the maximum mass of neutron stars (strange stars). Wenumerically construct stellar models using a highly accuraterelativistic code based on a multi-domain spectral method. We findmuch larger mass increases for strange stars than for neutron starsfor the same degree of differential rotation.

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