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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.
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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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In a flame photometer, when a solution like potassium chloride is aspirated into the flame, the solvent evaporates, leaving behind dehydrated salt. This salt dissociates into free gaseous atoms in their ground state. Some of these atoms absorb energy from the flame, leading to their excitation. The excited atoms return to the ground state, emitting photons at characteristic wavelengths. Because only electronic transitions are involved, the resulting emission lines are very narrow. The intensity...
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The Sun: Our own backyard plasma laboratory.

Peter R Young1,2

  • 1NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.

Proceedings of the International Astronomical Union. International Astronomical Union
|December 9, 2020
PubMed
Summary

The Sun's atmosphere heats up dramatically due to magnetic fields, making it ideal for studying ionized atoms. Accurate atomic data is crucial for analyzing solar spectra, especially using the CHIANTI database.

Keywords:
Sun: UV radiationSun: X-rays, gamma raysSun: coronaatomic data

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Area of Science:

  • Solar physics
  • Atomic physics
  • Plasma astrophysics

Background:

  • The Sun's atmosphere exhibits a significant temperature increase from its surface to higher altitudes.
  • This phenomenon is primarily attributed to the complex dynamics of the Sun's magnetic field.
  • The low plasma density and extreme temperature gradients create a unique natural laboratory for atomic studies.

Purpose of the Study:

  • To emphasize the critical role of atomic data in modeling solar spectra.
  • To highlight the CHIANTI atomic database as a key resource for solar spectral analysis.
  • To discuss current challenges and future needs in atomic data for solar research.

Main Methods:

  • Analysis of atomic transitions in ultraviolet (UV) and X-ray wavelength regions.
  • Utilizing spectral line data that are not affected by optical depth or interstellar absorption.
  • Focusing on the application of the CHIANTI atomic database for solar spectral modeling.

Main Results:

  • UV and X-ray spectral lines from the solar atmosphere are generally optically thin.
  • These lines are not obscured by interstellar absorption, simplifying analysis.
  • The CHIANTI database provides essential atomic data for interpreting these spectra.

Conclusions:

  • Accurate atomic data is indispensable for understanding the physical conditions in the Sun's atmosphere.
  • The CHIANTI database is a vital tool for researchers studying solar UV and X-ray spectra.
  • Future solar missions require continued development and refinement of atomic data.