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Atomic Nuclei: Nuclear Relaxation Processes01:23

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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.
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An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
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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.
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Scattering And Absorption of Light in Planetary Regoliths
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Cosmic rays and random magnetic traps.

Devika Tharakkal1, Andrew P Snodin1, Graeme R Sarson1

  • 1School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne, NE1 7RU, United Kingdom.

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Summary
This summary is machine-generated.

Cosmic ray (CR) distribution in the interstellar medium (ISM) is affected by magnetic fields. Simulations show source variations and energy losses create persistent CR clumps, impacting astrophysical interpretations.

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Area of Science:

  • Astrophysics
  • Radio Astronomy

Background:

  • Cosmic ray (CR) distribution in the interstellar medium (ISM) is crucial for radio astronomy and theoretical astrophysics.
  • Local magnetic field variations influence CR particle dynamics and diffusivity.
  • Magnetic traps can create persistent features in CR spatial distribution.

Purpose of the Study:

  • To investigate the spatial distribution of cosmic ray particles in various magnetic field configurations.
  • To understand the impact of magnetic field structures on CR particle behavior.
  • To analyze the influence of CR source inhomogeneity and energy losses on their distribution.

Main Methods:

  • Utilized test particle simulations.
  • Studied ensembles of both protons and electrons.
  • Employed diverse magnetic field configurations, from idealized traps to random fields.

Main Results:

  • Demonstrated that CR source inhomogeneity and energy losses lead to persistent local CR distribution inhomogeneities.
  • Showcased distinct spatial distributions for protons and electrons.
  • Highlighted the role of magnetic traps in shaping CR distribution.

Conclusions:

  • CR spatial distribution is significantly influenced by magnetic field structures and particle properties.
  • Findings have implications for interpreting synchrotron emission and its fluctuations.
  • The study provides insights into the complex interplay between CRs and the ISM.