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Related Concept Videos

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.
1.0K
Magnetic Field due to Moving Charges01:23

Magnetic Field due to Moving Charges

8.9K
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...
8.9K
Atomic Nuclei: Magnetic Resonance01:05

Atomic Nuclei: Magnetic Resonance

706
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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A 100 KW Class Applied-field Magnetoplasmadynamic Thruster
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A highly magnetized environment in a pulsar binary system.

Dongzi Li1, Anna Bilous2, Scott Ransom3

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

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|May 17, 2023
PubMed
Summary
This summary is machine-generated.

Spider pulsars, like PSR B1744-24A, exhibit highly magnetized environments. Evidence suggests these magnetic fields influence pulsar emission and may be similar to conditions found in some fast radio bursts (FRBs).

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Area of Science:

  • Astronomy and Astrophysics
  • Pulsar Physics
  • Binary Star Systems

Background:

  • Spider pulsars are millisecond pulsars in close orbits with low-mass companion stars.
  • These systems exhibit phenomena like plasma ablation, time delays, and eclipses of pulsar radio emission.
  • The companion star's magnetic field is hypothesized to influence binary system evolution and eclipse properties.

Purpose of the Study:

  • To investigate the magnetized environment of the spider pulsar system PSR B1744-24A.
  • To analyze polarization and rotation measure variations to understand magnetic field properties.
  • To explore potential connections between spider pulsar behavior and Fast Radio Bursts (FRBs).

Main Methods:

  • Observation of circular polarization (V) changes in PSR B1744-24A.
  • Analysis of irregular, fast changes in Rotation Measure (RM) at various orbital phases.
  • Comparison of observed polarization behavior with known FRB characteristics.

Main Results:

  • Semi-regular circular polarization profile changes indicate Faraday conversion, constraining the companion magnetic field to >10 G.
  • Irregular, rapid RM variations suggest a stellar wind magnetic field strength >10 mG.
  • Observed polarization behavior shows similarities to repeating Fast Radio Bursts (FRBs).

Conclusions:

  • PSR B1744-24A possesses a highly magnetized environment, with significant magnetic fields from both the companion and its stellar wind.
  • The observed phenomena, including Faraday conversion and RM variations, provide strong evidence for these magnetic fields.
  • Similarities with FRBs suggest that a fraction of FRBs may originate from binary systems like spider pulsars.