English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Bar-mode instability suppression in magnetized relativistic stars

Franci, L., De Pietri, R., Dionysopoulou, K., & Rezzolla, L. (2013). Bar-mode instability suppression in magnetized relativistic stars. Journal of Physics: Conference Series, 470: 012008. doi:10.1088/1742-6596/470/1/012008.

Item is

Files

show Files
hide Files
:
1309.6549.pdf (Preprint), 7MB
Name:
1309.6549.pdf
Description:
File downloaded from arXiv at 2016-07-12 09:18
OA-Status:
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
:
jpconf13_470_012008.pdf (Any fulltext), 7MB
Name:
jpconf13_470_012008.pdf
Description:
-
OA-Status:
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 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              

Content

show
hide
Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: We show that magnetic fields stronger than about $10^{15}$ 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 $10^{14}-10^{16}$ G. When the seed field is a few parts in $10^{15}$ 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.

Details

show
hide
Language(s):
 Dates: 2013-09-252013
 Publication Status: Issued
 Pages: 6 pages, 4 figures, to appear on the proceedings of the 4th YRM (Trieste 2013)
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Journal of Physics: Conference Series
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 470 Sequence Number: 012008 Start / End Page: - Identifier: -