Rotating neutron star models with a toroidal magnetic field - SFB/TR7

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Conclusion 17 • First fully relativistic models of rotating stars with a toroidal magnetic field: ⋆ Only slight prolate deformation of the apparent shape. ⋆ Noticeable impact on matter distribution inside the star. ⋆ Magnetic field leads to an overall growth of the star. ⋆ For astrophysically relevant range of rotation frequency and magnetic field strength perturbative treatment justified. ⋆ General relativistic effects attenuate the magnetic distortion. ⋆ Influence of realistic EOS dominated by impact on actual radius. ⋆ Magnetic and rotational deformation parameters given by Cutler (2002) significantly too large. • Further directions to explore: ⋆ Global study of neutron star models with a toroidal magnetic field. ⋆ Implement differential rotation. ⋆ Implement mixed magnetic fields (poloidal and toroidal). ⋆ Investigate instability of magnetized models. Joachim Frieben Golm, June 18, 2007
References 18 P. B. Jones, Astrophys. Space Sci., 33, 215 (1975) A. Oron, Phys. Rev. D 66, 023006 (2002) http://www.lorene.obspm.fr N. K. Sinha, Aust. J. Phys., 21, 283 (1968) J. C. Wheeler, I. Yi, P. Höflich, and L. Wang, Astrophys. J., 537, 810 (2000) S. Bonazzola and E. Gourgoulhon, Astron. Astrophys. 312, 675 (1996) C. Cutler, Phys. Rev. D 66, 084025 (2002) Golm, June 18, 2007
Page 1 and 2: Rotating neutron star models with a
Page 3 and 4: Motivation 2 Quest for astrophysica
Page 5 and 6: Theoretical formulation 4 Electroma
Page 7 and 8: Results for an n=1 polytropic equat
Page 13 and 14: 12 Results for an n=1 polytropic eq
Page 15 and 16: Results for realistic equations of
Page 17: Results for realistic equations of

Rotating neutron star models with a toroidal magnetic field - SFB/TR7

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