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Chandler Wobble and Free Core Nutation of Neutron Stars

  • Alexander Gusev (a1) and Irina Kitiashvili (a1)

Abstract

Extending the theory of core-mantle differential rotation of a planet, we have obtained the periods P CW and P FCN for different pulsars in the second approximation. We have investigated the dependence of these periods on the equation of state of neutron liquid, flatness of mantle and crust of the neutron star.

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Copyright

References

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Gonzalez, A-B., & Getino, J. 1997, Celest. Mech. & Dyn. Astr., 68, 139.
Gusev, A., & Kitiashvili, I. 2003, in Proc. Geon-Kazan-2003, ed. Petrova, N., Kazan Univ. Press, Vol. 3, 80.
Petrova, N., & Gusev, A. 2001, Cel. Mech & Dyn. Astr., 80, 215.
Stairs, I. H., Lyne, A. G., & Shemar, S. L. 2000, Nature, 406, 484.
Van Hoolst, T., Dehant, V., & Defraigne, P. 1998, Phys. Earth & Planetary Interiors, 117, 397.
Wolszczan, A., & Frail, D. A. 1992, Nature, 355, 145.

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Chandler Wobble and Free Core Nutation of Neutron Stars

  • Alexander Gusev (a1) and Irina Kitiashvili (a1)

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