Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions

Kotaro Fujisawa, Shota Kisaka

Research output: Chapter in Book/Report/Conference proceedingChapter

Abstract

We have calculated many Hall equilibrium states within the neutron star crust under various boundary conditions in order to investigate the influences of the boundary conditions clearly. We have found two important features of these solutions. First, the magnitude of the core magnetic fields affects the toroidal to total magnetic field energy ratio within the crust (Et /E). If the core magnetic fields are vanished, the crustal toroidal magnetic fields become weak and the typical energy ratio is only Et / E ∼0.1%. If the core magnetic fields are strong, however, the crustal toroidal magnetic fields become strong and the typical ratio reaches Et / E ∼15%. Second, the core toroidal magnetic fields and the twisted magnetosphere around the star make the size of the crustal toroidal magnetic field regions large. Therefore if the strong core magnetic fields have strong toroidal component, both strength and size of the crustal toroidal magnetic fields become large. These results show that the Hall MHD evolutions would be deeply affected by both inner and outer boundary conditions.

Original languageEnglish
Title of host publicationProceedings of the International Astronomical Union
PublisherCambridge University Press
Pages427-428
Number of pages2
Volume9
EditionS302
ISBN (Print)9781107044982
DOIs
Publication statusPublished - 2014
Externally publishedYes

Publication series

NameProceedings of the International Astronomical Union
NumberS302
Volume9
ISSN (Print)17439213
ISSN (Electronic)17439221

Fingerprint

neutron stars
crusts
boundary conditions
magnetic fields
magnetospheres
stars
energy

Keywords

  • Stars: interior - Stars: neutron - Stars: magnetic fields

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Cite this

Fujisawa, K., & Kisaka, S. (2014). Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions. In Proceedings of the International Astronomical Union (S302 ed., Vol. 9, pp. 427-428). (Proceedings of the International Astronomical Union; Vol. 9, No. S302). Cambridge University Press. https://doi.org/10.1017/S174392131400266X

Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions. / Fujisawa, Kotaro; Kisaka, Shota.

Proceedings of the International Astronomical Union. Vol. 9 S302. ed. Cambridge University Press, 2014. p. 427-428 (Proceedings of the International Astronomical Union; Vol. 9, No. S302).

Research output: Chapter in Book/Report/Conference proceedingChapter

Fujisawa, K & Kisaka, S 2014, Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions. in Proceedings of the International Astronomical Union. S302 edn, vol. 9, Proceedings of the International Astronomical Union, no. S302, vol. 9, Cambridge University Press, pp. 427-428. https://doi.org/10.1017/S174392131400266X
Fujisawa K, Kisaka S. Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions. In Proceedings of the International Astronomical Union. S302 ed. Vol. 9. Cambridge University Press. 2014. p. 427-428. (Proceedings of the International Astronomical Union; S302). https://doi.org/10.1017/S174392131400266X
Fujisawa, Kotaro ; Kisaka, Shota. / Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions. Proceedings of the International Astronomical Union. Vol. 9 S302. ed. Cambridge University Press, 2014. pp. 427-428 (Proceedings of the International Astronomical Union; S302).
@inbook{85389cf7cca2466ca0011c60937d5448,
title = "Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions",
abstract = "We have calculated many Hall equilibrium states within the neutron star crust under various boundary conditions in order to investigate the influences of the boundary conditions clearly. We have found two important features of these solutions. First, the magnitude of the core magnetic fields affects the toroidal to total magnetic field energy ratio within the crust (Et /E). If the core magnetic fields are vanished, the crustal toroidal magnetic fields become weak and the typical energy ratio is only Et / E ∼0.1{\%}. If the core magnetic fields are strong, however, the crustal toroidal magnetic fields become strong and the typical ratio reaches Et / E ∼15{\%}. Second, the core toroidal magnetic fields and the twisted magnetosphere around the star make the size of the crustal toroidal magnetic field regions large. Therefore if the strong core magnetic fields have strong toroidal component, both strength and size of the crustal toroidal magnetic fields become large. These results show that the Hall MHD evolutions would be deeply affected by both inner and outer boundary conditions.",
keywords = "Stars: interior - Stars: neutron - Stars: magnetic fields",
author = "Kotaro Fujisawa and Shota Kisaka",
year = "2014",
doi = "10.1017/S174392131400266X",
language = "English",
isbn = "9781107044982",
volume = "9",
series = "Proceedings of the International Astronomical Union",
publisher = "Cambridge University Press",
number = "S302",
pages = "427--428",
booktitle = "Proceedings of the International Astronomical Union",
edition = "S302",

}

TY - CHAP

T1 - Axisymmetric and stationary magnetic field structures in neutron star crusts under various boundary conditions

AU - Fujisawa, Kotaro

AU - Kisaka, Shota

PY - 2014

Y1 - 2014

N2 - We have calculated many Hall equilibrium states within the neutron star crust under various boundary conditions in order to investigate the influences of the boundary conditions clearly. We have found two important features of these solutions. First, the magnitude of the core magnetic fields affects the toroidal to total magnetic field energy ratio within the crust (Et /E). If the core magnetic fields are vanished, the crustal toroidal magnetic fields become weak and the typical energy ratio is only Et / E ∼0.1%. If the core magnetic fields are strong, however, the crustal toroidal magnetic fields become strong and the typical ratio reaches Et / E ∼15%. Second, the core toroidal magnetic fields and the twisted magnetosphere around the star make the size of the crustal toroidal magnetic field regions large. Therefore if the strong core magnetic fields have strong toroidal component, both strength and size of the crustal toroidal magnetic fields become large. These results show that the Hall MHD evolutions would be deeply affected by both inner and outer boundary conditions.

AB - We have calculated many Hall equilibrium states within the neutron star crust under various boundary conditions in order to investigate the influences of the boundary conditions clearly. We have found two important features of these solutions. First, the magnitude of the core magnetic fields affects the toroidal to total magnetic field energy ratio within the crust (Et /E). If the core magnetic fields are vanished, the crustal toroidal magnetic fields become weak and the typical energy ratio is only Et / E ∼0.1%. If the core magnetic fields are strong, however, the crustal toroidal magnetic fields become strong and the typical ratio reaches Et / E ∼15%. Second, the core toroidal magnetic fields and the twisted magnetosphere around the star make the size of the crustal toroidal magnetic field regions large. Therefore if the strong core magnetic fields have strong toroidal component, both strength and size of the crustal toroidal magnetic fields become large. These results show that the Hall MHD evolutions would be deeply affected by both inner and outer boundary conditions.

KW - Stars: interior - Stars: neutron - Stars: magnetic fields

UR - http://www.scopus.com/inward/record.url?scp=84905756747&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84905756747&partnerID=8YFLogxK

U2 - 10.1017/S174392131400266X

DO - 10.1017/S174392131400266X

M3 - Chapter

AN - SCOPUS:84905756747

SN - 9781107044982

VL - 9

T3 - Proceedings of the International Astronomical Union

SP - 427

EP - 428

BT - Proceedings of the International Astronomical Union

PB - Cambridge University Press

ER -