Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star

Gemechu Muleta Kumssa; Legesse Wetro Kebede

doi:doi:10.11648/j.ajaa.20241104.11

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Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star

Gemechu Muleta Kumssa^*

, Legesse Wetro Kebede

Published in American Journal of Astronomy and Astrophysics (Volume 11, Issue 4)

Received: 26 July 2024 Accepted: 3 September 2024 Published: 31 October 2024

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Abstract

Neutron stars (NSs) are rapidly rotating entities, spinning at approximately 10⁴ Hz, and possess extremely strong magnetic fields, ranging from 10¹³ to 10¹⁴ Gauss. These compact objects, characterized by a radius of about 10 kilometers and a density of 10¹³⁻¹⁴, gcm⁻³ are formed as a result of supernova explosions that mark the end of the life cycles of massive stars. Observations of electromagnetic emissions associated with curvature radiation from well-known pulsars, such as the Crab and Vela pulsars, provide compelling evidence that the magnetic field configuration near the surfaces of these neutron stars deviates significantly from the traditionally anticipated pure dipole structure. Researchers now propose that the inclusion of non-dipolar components in the magnetic field may address this longstanding discrepancy. Furthermore, the arrangement of magnetic field lines plays a crucial role in determining the characteristics and geometry of accretion discs surrounding neutron stars in binary systems. This study has focused on elucidating the geometry of the combined dipole and quadrupole magnetic field lines. In idealized scenarios, the magnetic field lines in proximity to these compact objects are typically closed; however, they may become open at greater distances due to interactions with external magnetic fields or the stress energy generated by other sources, including the accretion discs.

Published in	American Journal of Astronomy and Astrophysics (Volume 11, Issue 4)
DOI	10.11648/j.ajaa.20241104.11
Page(s)	92-105
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2024. Published by Science Publishing Group

Keywords

Pulsar, Neutron Star, Magnetic Field, Dipole, Quadrupole, Supernova, Magnetar

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APA Style

Kumssa, G. M., Kebede, L. W. (2024). Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. American Journal of Astronomy and Astrophysics, 11(4), 92-105. https://doi.org/10.11648/j.ajaa.20241104.11

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ACS Style

Kumssa, G. M.; Kebede, L. W. Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. Am. J. Astron. Astrophys. 2024, 11(4), 92-105. doi: 10.11648/j.ajaa.20241104.11

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AMA Style

Kumssa GM, Kebede LW. Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. Am J Astron Astrophys. 2024;11(4):92-105. doi: 10.11648/j.ajaa.20241104.11

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@article{10.11648/j.ajaa.20241104.11,
  author = {Gemechu Muleta Kumssa and Legesse Wetro Kebede},
  title = {Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {11},
  number = {4},
  pages = {92-105},
  doi = {10.11648/j.ajaa.20241104.11},
  url = {https://doi.org/10.11648/j.ajaa.20241104.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20241104.11},
  abstract = {Neutron stars (NSs) are rapidly rotating entities, spinning at approximately 104 Hz, and possess extremely strong magnetic fields, ranging from 1013 to 1014 Gauss. These compact objects, characterized by a radius of about 10 kilometers and a density of 1013−14, gcm−3 are formed as a result of supernova explosions that mark the end of the life cycles of massive stars. Observations of electromagnetic emissions associated with curvature radiation from well-known pulsars, such as the Crab and Vela pulsars, provide compelling evidence that the magnetic field configuration near the surfaces of these neutron stars deviates significantly from the traditionally anticipated pure dipole structure. Researchers now propose that the inclusion of non-dipolar components in the magnetic field may address this longstanding discrepancy. Furthermore, the arrangement of magnetic field lines plays a crucial role in determining the characteristics and geometry of accretion discs surrounding neutron stars in binary systems. This study has focused on elucidating the geometry of the combined dipole and quadrupole magnetic field lines. In idealized scenarios, the magnetic field lines in proximity to these compact objects are typically closed; however, they may become open at greater distances due to interactions with external magnetic fields or the stress energy generated by other sources, including the accretion discs.},
 year = {2024}
}

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TY  - JOUR
T1  - Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star
AU  - Gemechu Muleta Kumssa
AU  - Legesse Wetro Kebede
Y1  - 2024/10/31
PY  - 2024
N1  - https://doi.org/10.11648/j.ajaa.20241104.11
DO  - 10.11648/j.ajaa.20241104.11
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 92
EP  - 105
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20241104.11
AB  - Neutron stars (NSs) are rapidly rotating entities, spinning at approximately 104 Hz, and possess extremely strong magnetic fields, ranging from 1013 to 1014 Gauss. These compact objects, characterized by a radius of about 10 kilometers and a density of 1013−14, gcm−3 are formed as a result of supernova explosions that mark the end of the life cycles of massive stars. Observations of electromagnetic emissions associated with curvature radiation from well-known pulsars, such as the Crab and Vela pulsars, provide compelling evidence that the magnetic field configuration near the surfaces of these neutron stars deviates significantly from the traditionally anticipated pure dipole structure. Researchers now propose that the inclusion of non-dipolar components in the magnetic field may address this longstanding discrepancy. Furthermore, the arrangement of magnetic field lines plays a crucial role in determining the characteristics and geometry of accretion discs surrounding neutron stars in binary systems. This study has focused on elucidating the geometry of the combined dipole and quadrupole magnetic field lines. In idealized scenarios, the magnetic field lines in proximity to these compact objects are typically closed; however, they may become open at greater distances due to interactions with external magnetic fields or the stress energy generated by other sources, including the accretion discs.
VL  - 11
IS  - 4
ER  -

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Author Information

Gemechu Muleta Kumssa

Department of Physics, Addis Ababa University, Addis Ababa, Ethiopia; Astronomy and Astrophysics Department, Space Science and Geospatial Institute (SSGI), Entoto Observatory and Research Center (EORC), Addis Ababa, Ethiopia; Department of Physics, Jimma University, Jimma, Ethiopia

Contact Email

http://orcid.org/0000-0002-9043-3779
Legesse Wetro Kebede

Astronomy and Astrophysics Department, Space Science and Geospatial Institute (SSGI), Entoto Observatory and Research Center (EORC), Addis Ababa, Ethiopia

Contact Email

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Sections

Plain Text BibTeX RIS

APA Style

Kumssa, G. M., Kebede, L. W. (2024). Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. American Journal of Astronomy and Astrophysics, 11(4), 92-105. https://doi.org/10.11648/j.ajaa.20241104.11

Copy | Download

ACS Style

Kumssa, G. M.; Kebede, L. W. Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. Am. J. Astron. Astrophys. 2024, 11(4), 92-105. doi: 10.11648/j.ajaa.20241104.11

Copy | Download

AMA Style

Kumssa GM, Kebede LW. Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star. Am J Astron Astrophys. 2024;11(4):92-105. doi: 10.11648/j.ajaa.20241104.11

Copy | Download

@article{10.11648/j.ajaa.20241104.11,
  author = {Gemechu Muleta Kumssa and Legesse Wetro Kebede},
  title = {Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {11},
  number = {4},
  pages = {92-105},
  doi = {10.11648/j.ajaa.20241104.11},
  url = {https://doi.org/10.11648/j.ajaa.20241104.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20241104.11},
  abstract = {Neutron stars (NSs) are rapidly rotating entities, spinning at approximately 104 Hz, and possess extremely strong magnetic fields, ranging from 1013 to 1014 Gauss. These compact objects, characterized by a radius of about 10 kilometers and a density of 1013−14, gcm−3 are formed as a result of supernova explosions that mark the end of the life cycles of massive stars. Observations of electromagnetic emissions associated with curvature radiation from well-known pulsars, such as the Crab and Vela pulsars, provide compelling evidence that the magnetic field configuration near the surfaces of these neutron stars deviates significantly from the traditionally anticipated pure dipole structure. Researchers now propose that the inclusion of non-dipolar components in the magnetic field may address this longstanding discrepancy. Furthermore, the arrangement of magnetic field lines plays a crucial role in determining the characteristics and geometry of accretion discs surrounding neutron stars in binary systems. This study has focused on elucidating the geometry of the combined dipole and quadrupole magnetic field lines. In idealized scenarios, the magnetic field lines in proximity to these compact objects are typically closed; however, they may become open at greater distances due to interactions with external magnetic fields or the stress energy generated by other sources, including the accretion discs.},
 year = {2024}
}

Copy | Download

TY  - JOUR
T1  - Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star
AU  - Gemechu Muleta Kumssa
AU  - Legesse Wetro Kebede
Y1  - 2024/10/31
PY  - 2024
N1  - https://doi.org/10.11648/j.ajaa.20241104.11
DO  - 10.11648/j.ajaa.20241104.11
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 92
EP  - 105
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20241104.11
AB  - Neutron stars (NSs) are rapidly rotating entities, spinning at approximately 104 Hz, and possess extremely strong magnetic fields, ranging from 1013 to 1014 Gauss. These compact objects, characterized by a radius of about 10 kilometers and a density of 1013−14, gcm−3 are formed as a result of supernova explosions that mark the end of the life cycles of massive stars. Observations of electromagnetic emissions associated with curvature radiation from well-known pulsars, such as the Crab and Vela pulsars, provide compelling evidence that the magnetic field configuration near the surfaces of these neutron stars deviates significantly from the traditionally anticipated pure dipole structure. Researchers now propose that the inclusion of non-dipolar components in the magnetic field may address this longstanding discrepancy. Furthermore, the arrangement of magnetic field lines plays a crucial role in determining the characteristics and geometry of accretion discs surrounding neutron stars in binary systems. This study has focused on elucidating the geometry of the combined dipole and quadrupole magnetic field lines. In idealized scenarios, the magnetic field lines in proximity to these compact objects are typically closed; however, they may become open at greater distances due to interactions with external magnetic fields or the stress energy generated by other sources, including the accretion discs.
VL  - 11
IS  - 4
ER  -

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