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Atomic Nuclei: Nuclear Magnetic Moment00:59

Atomic Nuclei: Nuclear Magnetic Moment

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All atomic nuclei are positively charged. When they have a nonzero spin, they behave like rotating charges. As a consequence of their charge and spin, these nuclei generate a magnetic field (B). This, in turn, gives rise to a magnetic moment (μ), which is randomly oriented in the absence of an external magnetic field. When an external magnetic field (B0) is applied, the magnetic moment vectors can align with the field or against it in 2 + 1 orientations. A hydrogen nucleus, which is just a...
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Potential Due to a Magnetized Object01:24

Potential Due to a Magnetized Object

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Magnetic dipoles in magnetic materials are aligned when placed under an external magnetic field. For paramagnets and ferromagnets, dipole alignment occurs in the direction of the magnetic field. However, the dipoles align opposite to the field in the case of diamagnets. This state of magnetic polarization due to the external field is called magnetization. Magnetization is defined as the dipole moment per unit volume. It plays a similar role to polarization in electrostatics.
The vector...
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Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

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In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
690
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

1.0K
Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
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Magnetic Field due to Moving Charges01:23

Magnetic Field due to Moving Charges

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A stationary charge creates and interacts with the electric field, while a moving charge creates a magnetic field.
Consider a point charge moving with a constant velocity. Like the electric field, the magnetic field at any point is directly proportional to the magnitude of the charge and inversely proportional to the square of the distance between the source point and the field point. However, unlike the electric field, the magnetic field is always perpendicular to the plane containing the line...
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Atomic Nuclei: Magnetic Resonance01:05

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The number of nuclear spins aligned in the lower energy state is slightly greater than those in the higher energy state. In the presence of an external magnetic field, as the spins precess at the Larmor frequency, the excess population results in a net magnetization oriented along the z axis. When a pulse or a short burst of radio waves at the Larmor frequency is applied along the x axis, the coupling of frequencies causes resonance and flips the nuclear spins of the excess population from the...
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Updated: Jul 30, 2025

A 100 KW Class Applied-field Magnetoplasmadynamic Thruster
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在脉冲星二进制系统中的高度磁化环境

Dongzi Li1, Anna Bilous2, Scott Ransom3

  • 1Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA. dongzili@caltech.edu.

Nature
|May 17, 2023
PubMed
概括
此摘要是机器生成的。

像PSR B1744-24A这样的蜘蛛脉冲星具有高度磁化的环境. 证据表明这些磁场会影响脉冲星的发射,并且可能与某些快速无线电爆发 (FRB) 中发现的条件相似.

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科学领域:

  • 天文学与天体物理学
  • 脉冲星物理
  • 双星系统

背景情况:

  • 蜘蛛脉冲星是靠近低质量伴星的毫秒脉冲星.
  • 这些系统表现出像等离子体剥离,时间延迟和脉冲射线发射的日食等现象.
  • 伴星的磁场被假定会影响二进制系统的演变和日食特性.

研究的目的:

  • 为了研究蜘蛛脉冲星系统PSR B1744-24A的磁化环境.
  • 分析极化和旋转的变化,了解磁场的特性.
  • 探索蜘蛛脉冲星行为与快速无线电爆发 (FRB) 之间的潜在联系.

主要方法:

  • 在PSR B1744-24A中观察圆极化 (V) 变化.
  • 分析不同轨道阶段旋转量 (RM) 的不规则,快速变化.
  • 观察到的极化行为与已知的FRB特性进行比较.

主要成果:

  • 半正规的圆形偏振变化表明法拉第转换,将伴随磁场限制在10G以上.
  • 不规则的,快速的RM变化表明恒星风的磁场强度大于10mG.
  • 观察到的极化行为与重复的快速无线电爆发 (FRB) 有相似之处.

结论:

  • PSR B1744-24A具有高度磁化的环境,来自伴星及其恒星风的磁场显著.
  • 观察到的现象,包括法拉第转换和RM变化,为这些磁场提供了强有力的证据.
  • 与FRB的相似之处表明,FRB的一小部分可能来自像蜘蛛脉冲星这样的二进制系统.