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Related Concept Videos

Atomic Emission Spectroscopy: Overview01:20

Atomic Emission Spectroscopy: Overview

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Atomic emission spectroscopy (AES) is an analytical technique used to determine the elemental composition of a sample by analyzing the light emitted from excited atoms. In AES, atoms in a sample are excited to higher energy levels by thermal energy from high-temperature sources, such as plasma, arcs, or sparks. When these excited atoms return to lower energy states, they emit light at specific wavelengths characteristic of each element. The resulting atomic emission spectrum, which consists of...
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Nuclear Overhauser Enhancement (NOE)01:07

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Irradiation of a spin-active nucleus causes an increase or decrease in the signal intensity of neighboring nuclei that are not necessarily chemically bonded or involved in J-coupling.  This phenomenon, called the Nuclear Overhauser Enhancement (NOE), results from through-space interactions between the nuclear spins. The NOE effect decreases with increasing internuclear distance and is generally not observed beyond 4 angstroms. In NOE, dipole-dipole interactions between neighboring...
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In atomic emission spectroscopy (AES), high-temperature atomizers excite a broad range of elements and molecules that generate complex emissions from sources such as oxides, hydroxides, and flame combustion products in the flame or plasma. Several strategies can be employed to minimize spectral interferences caused by overlapping emission lines or bands. These include increasing instrument resolution, choosing alternative emission lines, optimally placing the detector in low-background regions,...
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Emission Spectra02:39

Emission Spectra

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When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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Types of Radioactivity03:23

Types of Radioactivity

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The most common types of radioactivity are α decay, β decay, γ decay, neutron emission, and electron capture.
Alpha (α) decay is the emission of an α particle from the nucleus. For example, polonium-210 undergoes α decay:
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In the AX proton spin system, proton A can sense the two spin states of a coupled proton X, resulting in a doublet NMR signal with two peaks of equal (1:1) intensity. When proton A is coupled to two equivalent protons (AX2 spin system), the spin states of each X can be aligned with or against the external field, creating three possible scenarios. This results in a 1:2:1  triplet signal, where the central peak corresponds to the chemical shift of A and is twice as large or intense as the...
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Hyperpolarized Xenon for NMR and MRI Applications
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Enhanced Supernova Axion Emission and Its Implications.

Pierluca Carenza1,2, Bryce Fore3,4, Maurizio Giannotti5

  • 1Dipartimento Interateneo di Fisica "Michelangelo Merlin," Via Amendola 173, 70126 Bari, Italy.

Physical Review Letters
|March 5, 2021
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Summary
This summary is machine-generated.

We calculated axion emission rates from thermal pions in supernovae and neutron star mergers. This process is much larger than previously thought, offering new ways to detect QCD axions.

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Area of Science:

  • Astrophysics
  • Particle Physics
  • Nuclear Physics

Background:

  • Axion emission from astrophysical events is crucial for understanding fundamental physics.
  • Nucleon-nucleon bremsstrahlung was considered the dominant axion production mechanism.

Purpose of the Study:

  • To calculate the axion emission rate from thermal pion interactions.
  • To identify unique spectral features of these axions.
  • To explore astrophysical and particle physics implications.

Main Methods:

  • Calculations of axion emission rates from pion interactions in dense matter.
  • Analysis of the resulting axion spectrum.
  • Comparison with nucleon-nucleon bremsstrahlung.

Main Results:

  • Axion emission rate from thermal pions is 2-5 times larger than nucleon-nucleon bremsstrahlung.
  • The axion spectrum is significantly harder (higher energies).

Conclusions:

  • Pion-induced axion emission is a dominant process in supernovae and neutron star mergers.
  • These findings provide a stronger constraint on the QCD axion mass.
  • Enhanced prospects for direct axion detection using neutrino detectors during supernovae.