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Related Concept Videos

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.
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Atomic Nuclei: Larmor Precession Frequency01:11

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The earth's gravitational field produces a 'twisting force' perpendicular to the angular momentum of a spinning mass (such as a spinning top) that causes the mass to 'wobble' around the gravitational field axis in a phenomenon called precession. Similarly, the magnetic moment (μ) of a spinning nucleus precesses due to an external magnetic field directed along the z-axis. The precession of the magnetic moment vector about the magnetic field is called Larmor precession,...
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Nuclear relaxation restores the equilibrium population imbalance and can occur via spin–lattice or spin–spin mechanisms, which are first-order exponential decay processes.
In spin–lattice or longitudinal relaxation, the excited spins exchange energy with the surrounding lattice as they return to the lower energy level. Among several mechanisms that contribute to spin–lattice relaxation, magnetic dipolar interactions are significant. Here, the excited nucleus transfers...
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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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Protons and neutrons, collectively called nucleons, are packed together tightly in a nucleus. With a radius of about 10−15 meters, a nucleus is quite small compared to the radius of the entire atom, which is about 10−10 meters. Nuclei are extremely dense compared to bulk matter, averaging 1.8 × 1014 grams per cubic centimeter. If the earth’s density were equal to the average nuclear density, the earth’s radius would be only about 200 meters.
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Stability is an important concept in oscillation. If an equilibrium point is stable, a slight disturbance of an object that is initially at the stable equilibrium point will cause the object to oscillate around that point. For an unstable equilibrium point, if the object is disturbed slightly, it will not return to the equilibrium point. There are three conditions for equilibrium points—stable, unstable, and half-stable. A half-stable equilibrium point is also unstable, but is named so...
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Cooling an Optically Trapped Ultracold Fermi Gas by Periodical Driving
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Neutron-Mirror-Neutron Oscillation and Neutron Star Cooling.

Itzhak Goldman1, Rabindra N Mohapatra2, Shmuel Nussinov3

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Neutron star cooling rates may not limit neutron to mirror neutron transitions. A new effect involving mirror particle decay and scattering within neutron stars relaxes previous stringent bounds, allowing for potential discovery.

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Area of Science:

  • Astrophysics
  • Particle Physics
  • Neutron Star Physics

Background:

  • Previous studies suggested neutron star cooling rates impose stringent limits on neutron-to-mirror-neutron (n→n′) oscillation.
  • These limits were considered so restrictive as to preclude terrestrial detection of n→n′ oscillation.
  • This analysis critically re-evaluates the proposed upper limit based on neutron star cooling.

Purpose of the Study:

  • To critically analyze the proposed upper limit on n→n′ oscillation derived from neutron star cooling rates.
  • To investigate a newly identified effect in mirror models that influences the n→n′ oscillation bound.
  • To determine if the stringent upper limit on n→n′ oscillation is indeed valid.

Main Methods:

  • Analysis of nearly exact mirror models for n→n′ oscillation.
  • Inclusion of mirror beta decay (n′→p′+e′+ν̅e′) within the neutron star core.
  • Modeling of energy transfer via electron-electron (e-e′) scattering and mirror bremsstrahlung.

Main Results:

  • A new effect involving mirror particle decay creates a cloud of mirror particles (n′, p′, e′, D′) within the neutron star core.
  • Mirror electrons (e′) can extract energy from n→n′ transitions via e-e′ scattering, enabled by a millicharge on mirror particles.
  • This energy is lost via mirror bremsstrahlung, leading to a relaxation of the previously established upper limit on n→n′ oscillation.

Conclusions:

  • The stringent upper limit on n→n′ oscillation derived from neutron star cooling rates is significantly relaxed.
  • The newly considered effect of mirror particle interactions within neutron stars opens possibilities for detecting n→n′ oscillation.
  • Terrestrial searches for n→n′ oscillation may still be viable despite previous constraints.