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X-ray Crystallography02:18

X-ray Crystallography

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The size of the unit cell and the arrangement of atoms in a crystal may be determined from measurements of the diffraction of X-rays by the crystal, termed X-ray crystallography.
Diffraction
Diffraction is the change in the direction of travel experienced by an electromagnetic wave when it encounters a physical barrier whose dimensions are comparable to those of the wavelength of the light. X-rays are electromagnetic radiation with wavelengths about as long as the distance between neighboring...
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UV–Vis Spectrum01:30

UV–Vis Spectrum

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When light passes through a substance, a portion of the light is absorbed while the remaining light is reflected or transmitted. If the molecule absorbs light between the wavelengths of 180–400 nm range, the UV spectrum is obtained, and if it absorbs light in the 400–780 nm wavelength range, the visible spectrum is obtained.     
The UV–Vis spectrum of a molecule is the plot of its absorbance versus wavelength. The plot is drawn by taking molar...
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UV–Vis Spectrometers01:14

UV–Vis Spectrometers

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The absorbance of UV and visible (UV–visible) radiations is measured using a UV–visible spectrophotometer. Deuterium lamps, which emit UV radiation, and tungsten lamps, which produce radiation in the visible region, are used as light sources in UV–visible spectrophotometers. A monochromator or prism is used for diffraction grating, i.e., to split the incoming radiation into different wavelengths. A system of slits is used to focus the desired wavelength on the sample cell.
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X-ray Imaging01:24

X-ray Imaging

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German physicist Wilhelm Röntgen (1845–1923) was experimenting with electrical current when he discovered that a mysterious and invisible "ray" would pass through his flesh but leave an outline of his bones on a screen coated with a metal compound. In 1895, Röntgen made the first durable record of the internal parts of a living human: an "X-ray" image (as it came to be called) of his wife’s hand. Scientists worldwide quickly began their own experiments with...
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IR and UV–Vis Spectroscopy of Aldehydes and Ketones01:29

IR and UV–Vis Spectroscopy of Aldehydes and Ketones

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Infrared spectroscopy, also known as vibrational spectroscopy, is mainly used to determine the types of bonds and functional groups in molecules. In aldehydes and ketones, the carbonyl (C=O) bond shows an absorption around 1710 cm-1. The C=O bond vibration of an aldehyde occurs at lower frequencies than that of a ketone. In addition to the C=O absorption in an aldehyde, the aldehydic C–H bond also gives two peaks in the 2700–2800 cm-1 range. This absorption, coupled with the...
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IR and UV–Vis Spectroscopy of Carboxylic Acids01:28

IR and UV–Vis Spectroscopy of Carboxylic Acids

5.8K
In IR spectroscopy of carboxylic acids, the C=O bond shows a characteristic band between 1710 and 1760 cm⁻¹, and the O–H bond exhibits a broad band between 2500 and 3300 cm⁻¹.
However, the stretching absorptions for the C=O bond vary depending on the structure of carboxylic acids. The C=O bond of the free carboxylic acids shows a higher stretching frequency, 1760 cm−1, while H-bonded carboxylic acids (dimers) exhibit stretching absorptions at a lower frequency,...
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Solar UV and X-ray spectral diagnostics.

Giulio Del Zanna1, Helen E Mason1

  • 1DAMTP, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge, CB3 0WA UK.

Living Reviews in Solar Physics
|March 16, 2019
PubMed
Summary

This review explores X-ray and ultraviolet (XUV) spectroscopy for measuring solar plasma parameters. It details methods for analyzing optically thin emission to determine electron densities, temperatures, and abundances in the Sun's outer atmosphere.

Keywords:
Atomic dataAtomic processesLine: formationSun: abundancesSun: coronaTechniques: spectroscopic

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Area of Science:

  • Solar Physics
  • Plasma Astrophysics
  • Spectroscopy

Background:

  • Outer solar atmosphere analysis relies on X-ray and ultraviolet (UV) observations.
  • Optically thin emission at UV and X-ray (XUV) wavelengths provides key plasma diagnostics.
  • High-resolution spectroscopy is crucial for detailed measurements.

Purpose of the Study:

  • To review diagnostic methods for measuring solar plasma parameters using XUV optically thin emission.
  • To focus on electron density, electron temperature, differential emission measure (DEM), and chemical abundances.
  • To highlight techniques using single ion diagnostics and high-resolution spectroscopy.

Main Methods:

  • Analysis of optically thin emission from the solar atmosphere at UV and X-ray (XUV) wavelengths.
  • Application of high-resolution spectroscopy for detailed spectral line analysis.
  • Utilizing single ion diagnostics to determine electron densities and temperatures, minimizing ionization state complexities.

Main Results:

  • Review of diagnostic methods for electron density, electron temperature, DEM, and relative chemical abundances.
  • Summary of results for various solar regions: coronal holes, quiet Sun, active regions, and flares.
  • Emphasis on the importance of combining imaging and spectroscopic observations for comprehensive analysis.

Conclusions:

  • XUV spectroscopy is a powerful tool for characterizing solar plasma.
  • Single ion diagnostics and high-resolution spectroscopy provide reliable measurements.
  • Further advancements in atomic data and observational techniques will enhance solar atmosphere studies.