Deutsch
 
Hilfe Datenschutzhinweis Impressum
  DetailsucheBrowse

Datensatz

 
 
DownloadE-Mail
  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

Dateien

einblenden: Dateien
ausblenden: Dateien
:
1309.6549.pdf (Preprint), 7MB
Name:
1309.6549.pdf
Beschreibung:
File downloaded from arXiv at 2016-07-12 09:18
OA-Status:
Sichtbarkeit:
Öffentlich
MIME-Typ / Prüfsumme:
application/pdf / [MD5]
Technische Metadaten:
Copyright Datum:
-
Copyright Info:
-
:
jpconf13_470_012008.pdf (beliebiger Volltext), 7MB
Name:
jpconf13_470_012008.pdf
Beschreibung:
-
OA-Status:
Sichtbarkeit:
Öffentlich
MIME-Typ / Prüfsumme:
application/pdf / [MD5]
Technische Metadaten:
Copyright Datum:
-
Copyright Info:
-
Lizenz:
-

Externe Referenzen

einblenden:

Urheber

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

Inhalt

einblenden:
ausblenden:
Schlagwörter: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Zusammenfassung: 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

einblenden:
ausblenden:
Sprache(n):
 Datum: 2013-09-252013
 Publikationsstatus: Erschienen
 Seiten: 6 pages, 4 figures, to appear on the proceedings of the 4th YRM (Trieste 2013)
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Art des Abschluß: -

Veranstaltung

einblenden:

Entscheidung

einblenden:

Projektinformation

einblenden:

Quelle 1

einblenden:
ausblenden:
Titel: Journal of Physics: Conference Series
Genre der Quelle: Zeitschrift
 Urheber:
Affiliations:
Ort, Verlag, Ausgabe: -
Seiten: - Band / Heft: 470 Artikelnummer: 012008 Start- / Endseite: - Identifikator: -