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Related Concept Videos

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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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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Atomic Emission Spectroscopy: Lab01:29

Atomic Emission Spectroscopy: Lab

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AES is a powerful analytical technique, especially effective when used with plasma sources, producing abundant spectra in characteristic emission lines. The Inductively Coupled Plasma (ICP), in particular, yields superior quantitative analytical data due to its high stability, low noise, low background, and minimal interferences under optimal experimental conditions. However, newer air-operated microwave sources are emerging as promising alternatives that could be more cost-effective than...
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Atomic Emission Spectroscopy: Instrumentation01:22

Atomic Emission Spectroscopy: Instrumentation

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The instrumentation of atomic emission spectrometry (AES) involves various components, including atomization devices that convert samples into gas-phase atoms and ions. There are two main types of atomization devices: continuous and discrete atomizers.  Continuous atomizers, like plasmas and flames, introduce samples in a constant stream, while discrete atomizers inject individual samples using syringes or autosamplers. The most common discrete atomizer is the electrothermal atomizer.
560
Atomic Emission Spectroscopy: Interference01:30

Atomic Emission Spectroscopy: Interference

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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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Nuclear Fusion02:45

Nuclear Fusion

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The process of converting very light nuclei into heavier nuclei is also accompanied by the conversion of mass into large amounts of energy, a process called fusion. The principal source of energy in the sun is a net fusion reaction in which four hydrogen nuclei fuse and ultimately produce one helium nucleus and two positrons.
A helium nucleus has a mass that is 0.7% less than that of four hydrogen nuclei; this lost mass is converted into energy during the fusion. This reaction produces about...
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Updated: Aug 18, 2025

Measurement of Coherence Decay in GaMnAs Using Femtosecond Four-wave Mixing
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Gigaelectronvolt emission from a compact binary merger.

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A long-duration gamma-ray burst (GRB) was linked to a compact binary merger. Unexpected high-energy gamma-ray emission was observed, potentially from inverse Compton scattering with kilonova photons.

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Area of Science:

  • Astrophysics
  • High-energy astrophysics
  • Gravitational wave astronomy

Background:

  • Gamma-ray bursts (GRBs) are typically associated with massive star collapse.
  • GRB 211211A, despite its long duration, showed optical-infrared kilonova emission, suggesting a compact binary merger origin.
  • Standard afterglow models do not fully explain late-time emission from GRBs.

Purpose of the Study:

  • To investigate the origin of the high-energy gamma-ray emission from GRB 211211A.
  • To determine if the observed emission can be explained by standard afterglow models or requires alternative explanations.
  • To explore the implications of these findings for understanding compact binary mergers.

Main Methods:

  • Multi-wavelength observations of GRB 211211A, including public and dedicated data.
  • Detailed modeling of the gamma-ray emission, comparing observations with theoretical afterglow predictions.
  • Analysis of potential emission mechanisms, such as inverse Compton scattering.

Main Results:

  • Significant high-energy gamma-ray emission (above 0.1 GeV) was detected from GRB 211211A, starting 1000 seconds after the burst.
  • The observed gamma-ray flux at late times exceeded predictions from standard afterglow models.
  • Kilonova emission was identified as a potential source of seed photons for inverse Compton scattering.

Conclusions:

  • The high-energy emission from GRB 211211A is likely not solely due to standard afterglow processes.
  • Inverse Compton emission from the interaction of a late-time jet with kilonova photons offers a plausible explanation.
  • This finding provides new insights into the phenomena associated with binary neutron star mergers.