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Magnetic field structures inside magnetars with strong toroidal field

Published online by Cambridge University Press:  07 August 2014

Kotaro Fujisawa
Kotaro Fujisawa*
Affiliation:
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902, Japan email: fujisawa@ea.c.u-tokyo.ac.jp
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Abstract

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We have analyzed the magnetized equilibrium studies with strong toroidal magnetic fields and found that the negative toroidal current density inside the star is very important for the strong toroidal magnetic fields. The strong toroidal magnetic fields require the strong poloidal current, but the strong poloidal current results in the localized strong toroidal current density in the axisymmetric system. This localized toroidal current changes the magnetic field configuration and makes the size of the toroidal magnetic field region smaller. As a result, the toroidal magnetic field energy can not become large. We need to cancel out the localized toroidal current density in order to obtain the large toroidal fields solutions. We have found and showed that the negative toroidal current cancels out the localized toroidal current density and sustain the large toroidal magnetic field energy inside the star. We can explain the magnetized equilibrium studies with strong toroidal magnetic fields systematically using the negative current density. Physical meaning of the negative current is key to the magnetar interior magnetic fields.

Keywords

Stars: interior - Stars: neutron - Stars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 423 - 426
Copyright
Copyright © International Astronomical Union 2014 

References

Braithwaite, J., 2009, MNRAS, 397, 763CrossRefGoogle Scholar
Braithwaite, J. & Spruit, H. C., 2006, A&A, 450, 1097Google Scholar
Ciolfi, R., Ferrari, V., Gualtieri, L., & Pons, J. A., 2009, MNRAS, 397, 913Google Scholar
Ciolfi, R. & Rezzolla, L., 2013, MNRAS, 435, L43Google Scholar
Duez, V. & Mathis, S., 2010, A&A, 517, A58Google Scholar
Fujisawa, K. & Eriguchi, Y., 2013, MNRAS, 432, 1245CrossRefGoogle Scholar
Fujisawa, K., Yoshida, S., & Eriguchi, Y., 2012, MNRAS, 422, 434Google Scholar
Glampedakis, K., Andersson, N., Lander, S. K., 2012, MNRAS, 420, 1263Google Scholar
Lander, S. K. & Jones, D. I., 2009, MNRAS, 395, 2162Google Scholar
Rea, N.et al., 2010, Science, 330, 944Google Scholar
Tomimura, Y. & Eriguchi, Y., 2005, MNRAS, 359, 1117Google Scholar
Yoshida, S., Kiuchi, K., & Shibata, M., 2012, Phys. Rev. D, 86, 044012Google Scholar