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Models of Rotating Neutron Stars in General Relativity

Published online by Cambridge University Press:  07 February 2017

S. Bonazzola  and
G. Maschio
S. Bonazzola
Affiliation:
Observatoire de Paris, 92-Meudon, France
G. Maschio
Affiliation:
Instituto di Matematica Applicata, Universita di Roma, Rome, Italy

Abstract

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We describe a numerical method of integration of Einstein's equations coupled with the hydrodynamic equations for a perfect fluid. We give, also, some preliminary results.

We point out that the analogous problem was considered by Ostriker and Mark (1968) in the Newtonian case; by Thorne (1969) in General Relativity, in the weak angular velocity approximation; by Barden and Wagoner (1969) for disk configurations in the pressure vanishing case.

Type
Session 6
Information
Symposium - International Astronomical Union , Volume 46: The Crab Nebula , 1971 , pp. 346 - 351
Copyright
Copyright © Reidel 1971 

References

Bardeen, J. M. and Wagoner, R. V.: 1969, Astrophys. J. 158, L65.CrossRefGoogle Scholar
Boyer, R. H.: 1965, Proc. Cambridge Phil. Soc. 61, 527.CrossRefGoogle Scholar
Lichnerowicz, A.: 1955, Théories de la gravitation et de l'electromagnétisme , Masson, Paris.Google Scholar
Ostriker, J. P. and Mark, J. W. K.: 1968, Astrophys. J. 151, 1075.CrossRefGoogle Scholar
Thorne, K.: 1969, Astrophys. J. 153, 807.Google Scholar