Hostname: page-component-848d4c4894-pjpqr Total loading time: 0 Render date: 2024-07-01T05:34:56.304Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Get access

Abstract

Binary neutron star merger lead to the formation of a massive, rapidly and differentially rotating neutron star (or a strange star) or to the prompt collapse to a black hole. The maximum mass of a differentially rotating remnant is crucial for distinguishing between these two final objects. We study the effect of differential rotation on the maximum mass of neutron stars (strange stars). We numerically construct stellar models using a highly accurate relativistic code based on a multi-domain spectral method. We find much larger mass increases for strange stars than for neutron stars for the same degree of differential rotation.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 30: Spanish Relativity Meeting - Encuentros Relativistas Españoles , ERE2007: Relativistic Astrophysics and Cosmology , 2008 , pp. 373 - 376
Copyright
© EAS, EDP Sciences, 2008

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Alcock, C., Farhi, E., & Olinto, A., 1986, ApJ, 310, 261 CrossRef
Ansorg, M., Gondek-Rosińska, D., & Villain, L., 2008, in preparation
Ansorg, M., 2005, Phys. Rev. D, 72, 024018 CrossRef
Ansorg, M., & Petroff, D., 2005, Phys. Rev. D, 72, 024019 CrossRef
Ansorg, M., Kleinwächter, A., & Meinel, R., 2003, A&A, 405, 711
Baumgarte, T.W., Shapiro, S.L., & Shibata, M., 2000, ApJ, 528, L29 CrossRef
Cook, G.B., Shapiro, S.L., & Teukolsky, S.A., 1994, ApJ, 422, 227 CrossRef
Fahri, E., & Jaffe, R.L., 1984, Phys. Rev. D, 30, 2379
Gourgoulhon, E., Haensel, P., Livine, R., et al., 1999, A&A, 349, 851
Gondek-Rosińska, D., Bulik, T., Zdunik, J.L., et al., 2000, A&A, 363, 1005
Gondek-Rosinska, D., Haensel, P., Zdunik, J.L., & Gourgoulhon, E., 2000, Proceedings of the 177th Colloquium of the IAU held in Bonn, Germany, 1999 (San Francisco: ASP), ed. M. Kramer, N. Wex, and N. Wielebinski, ASP Conf. Ser., 202, 661
Gondek-Rosińska, D., Gourgoulhon, E., & Haensel, P., 2003, A&A, 412, 777
Haensel, P., Zdunik, J.L., & Schaeffer, R., 1986, A&A, 160, 121
Komatsu, H., Eriguchi, Y., & Hachisu, I., 1989, MNRAS, 237, 355 CrossRef
Lasota, J.P., Haensel, P., & Abramowicz, M.A., 1996, ApJ, 456, 300 CrossRef
Madsen, J., 1999, Lect. Notes Phys., 516, 162 CrossRef
Morrison, I.A., Baumgarte, T.W., & Shapiro, S.L., 2004, ApJ, 610, 941 CrossRef
Shibata, M., & Uryu, K., 2002, Prog. Theor. Phys., 107, 265 CrossRef
Schöbel, K., & Ansorg, M., 2003, A&A, 405, 405
Villain, L., Pons, J.A., Cerda-Duran, P., & Gourgoulhon, E., 2004, A&A, 418, 283
Weber, F., 2004, Prog. Part. Nucl. Phys., 54, 193 CrossRef
Zdunik, J.L., 2000, A&A, 359, 311