We show that magnetic fields stronger than about 1015 G are able to suppress the development of the hydrodynamical bar-mode instability in relativistic stars. The suppression is due to a change in the rest-mass density and angular velocity profiles due to the formation and to the linear growth of a toroidal component that rapidly overcomes the original poloidal one, leading to an amplification of the total magnetic energy. The study is carried out performing three-dimensional ideal-magnetohydrodynamics simulations in full general relativity, superimposing to the initial (matter) equilibrium configurations a purely poloidal magnetic field in the range 1014 -1016 G. When the seed field is a few parts in 1015 G or above, all the evolved models show the formation of a low-density envelope surrounding the star. For much weaker fields, no effect on the matter evolution is observed, while magnetic fields which are just below the suppression threshold are observed to slow down the growth-rate of the instability.

Bar-mode instability suppression in magnetized relativistic stars / Franci, Luca; DE PIETRI, Roberto; K., Dionysopoulou; L., Rezzolla. - In: JOURNAL OF PHYSICS. CONFERENCE SERIES. - ISSN 1742-6588. - 470:(2013), pp. 012008-1-012008-6. (Intervento presentato al convegno 4th Young Researcher Meeting tenutosi a Trieste; Italy nel 3 June 2013 through 4 June 2013) [10.1088/1742-6596/470/1/012008].

Bar-mode instability suppression in magnetized relativistic stars

FRANCI, Luca;DE PIETRI, Roberto;
2013-01-01

Abstract

We show that magnetic fields stronger than about 1015 G are able to suppress the development of the hydrodynamical bar-mode instability in relativistic stars. The suppression is due to a change in the rest-mass density and angular velocity profiles due to the formation and to the linear growth of a toroidal component that rapidly overcomes the original poloidal one, leading to an amplification of the total magnetic energy. The study is carried out performing three-dimensional ideal-magnetohydrodynamics simulations in full general relativity, superimposing to the initial (matter) equilibrium configurations a purely poloidal magnetic field in the range 1014 -1016 G. When the seed field is a few parts in 1015 G or above, all the evolved models show the formation of a low-density envelope surrounding the star. For much weaker fields, no effect on the matter evolution is observed, while magnetic fields which are just below the suppression threshold are observed to slow down the growth-rate of the instability.
2013
Bar-mode instability suppression in magnetized relativistic stars / Franci, Luca; DE PIETRI, Roberto; K., Dionysopoulou; L., Rezzolla. - In: JOURNAL OF PHYSICS. CONFERENCE SERIES. - ISSN 1742-6588. - 470:(2013), pp. 012008-1-012008-6. (Intervento presentato al convegno 4th Young Researcher Meeting tenutosi a Trieste; Italy nel 3 June 2013 through 4 June 2013) [10.1088/1742-6596/470/1/012008].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11381/2674865
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