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  Dynamical bar-mode instability in rotating and magnetized relativistic stars

Franci, L., De Pietri, R., Dionysopoulou, K., & Rezzolla, L. (2013). Dynamical bar-mode instability in rotating and magnetized relativistic stars. Physical Review D, 88(10): 104028. doi:10.1103/PhysRevD.88.104028.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0014-F703-0 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0014-F704-E
Genre: Journal Article

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 Creators:
Franci, Luca, Author
De Pietri, Roberto, Author
Dionysopoulou, Kyriaki, Author
Rezzolla, Luciano1, Author              
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: We present three-dimensional simulations of the dynamical bar-mode instability in magnetized and differentially rotating stars in full general relativity. Our focus is on the effects that magnetic fields have on the dynamics and the onset of the instability. In particular, we perform ideal-magnetohydrodynamics simulations of neutron stars that are known to be either stable or unstable against the purely hydrodynamical instability, but to which a poloidal magnetic field in the range of $10^{14}$--$10^{16}$ G is superimposed initially. As expected, the differential rotation is responsible for the shearing of the poloidal field and the consequent linear growth in time of the toroidal magnetic field. The latter rapidly exceeds in strength the original poloidal one, leading to a magnetic-field amplification in the the stars. Weak initial magnetic fields, i.e. $ \lesssim 10^{15}$ G, have negligible effects on the development of the dynamical bar-mode instability, simply braking the stellar configuration via magnetic-field shearing, and over a timescale for which we derived a simple algebraic expression. On the other hand, strong magnetic fields, i.e. $\gtrsim 10^{16}$ G, can suppress the instability completely, with the precise threshold being dependent also on the amount of rotation. As a result, it is unlikely that very highly magnetized neutron stars can be considered as sources of gravitational waves via the dynamical bar-mode instability.

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 Dates: 2013-08-192013
 Publication Status: Published in print
 Pages: 18 pages, 13 figures
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1308.3989
DOI: 10.1103/PhysRevD.88.104028
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 88 (10) Sequence Number: 104028 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258