Research Article
Magnetic Dipole and Quadrupole Interaction Fields of Neutron Star
Gemechu Muleta Kumssa*
,
Legesse Wetro Kebede
Issue:
Volume 11, Issue 4, December 2024
Pages:
92-105
Received:
26 July 2024
Accepted:
3 September 2024
Published:
31 October 2024
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.
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 cycle...
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Research Article
Calculation of the Initial 53Mn/55Mn in Calcium-Aluminum Rich Inclusions in the Solar Wind Implantation Model
Glynn Bricker*
Issue:
Volume 11, Issue 4, December 2024
Pages:
106-112
Received:
17 October 2024
Accepted:
12 November 2024
Published:
29 November 2024
DOI:
10.11648/j.ajaa.20241104.12
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Abstract: Studies indicate that short-lived radionuclides (SLRs), including 53Mn, were incorporated into Calcium-Aluminum Rich inclusions (CAIs) in ancient undisturbed primitive meteorites at the time the solar system was forming. In this study, the potential incorporation of 53Mn into CAIs in accordance with the Solar Wind Implantation Model (SWIM) is investigated. In the SWIM model, radiogenic nuclei are made through solar energetic particle (SEP) nuclear reactions with target material in the proto-stellar atmospheres of proto-stars are whilst the proto-stars are in the accretion phase. The newly produced daughter nuclei are subsequently trapped in the magnetic field lines associated with the proto-stars. The radiogenic nuclei are then funneled into the X-region, and some fraction of these nascent nuclei are implanted into refractory matter which accretes towards the proto-star. Production rates daughter nuclei scale with ancient X-ray luminosities, which have been measured to be 100,000 times contemporary levels in T Tauri stars, yielding daughter nuclei produced at ~105 over contemporary levels. From the ancient enhanced SEP fluxes and refractory mass inflow rate found in the SWIM, we found the initial 53Mn/55Mn isotopic ratio ranged from 4 x 10-5 to 6 x 10-4, when taking into account spectral flare variability.
Abstract: Studies indicate that short-lived radionuclides (SLRs), including 53Mn, were incorporated into Calcium-Aluminum Rich inclusions (CAIs) in ancient undisturbed primitive meteorites at the time the solar system was forming. In this study, the potential incorporation of 53Mn into CAIs in accordance with the Solar Wind Implantation Model (SWIM) is inves...
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