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For AAS measurements, samples must be introduced as clear solutions, often requiring extensive preliminary treatment to dissolve materials like soils, animal tissues, and minerals. Common methods for sample preparation include treatment with hot mineral acids, wet ashing, combustion in closed containers, high-temperature ashing, or fusion with reagents.
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The solar wind shows different element abundances than the solar corona due to the first ionization potential (FIP) effect. Intermediate elements like sulfur behave differently in solar wind, suggesting fractionation in the chromosphere.

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Area of Science:

  • Solar physics
  • Plasma physics
  • Spectroscopy

Background:

  • The solar corona and slow solar wind exhibit elemental abundances modified by the first ionization potential (FIP) effect.
  • Elements with low FIP (<10 eV) are enhanced in the corona, while high-FIP elements are relatively depleted.
  • Subtle differences exist between closed-loop solar corona and slow solar wind composition.

Purpose of the Study:

  • To investigate the distinct elemental abundances in the closed-loop solar corona and slow solar wind.
  • To understand the origin of differing FIP fractionation in these solar plasma sources.
  • To explore the role of chromospheric fractionation and wave properties in shaping solar wind composition.

Main Methods:

  • Analysis of element abundances in solar corona and solar wind.
  • Application of the ponderomotive force model for FIP fractionation in the chromosphere.
  • Consideration of wave properties (nonresonant, torsional Alfvén, shear waves) and their impact on fractionation.
  • Examination of interchange reconnection models for slow solar wind origin.

Main Results:

  • Intermediate elements (S, P, C) with FIP just above 10 eV act as high-FIP elements in closed loops but are fractionated like low-FIP elements in the solar wind.
  • Fractionation occurring low in the chromosphere, where hydrogen is neutral, enhances S, P, and C abundances.
  • Nonresonant waves and torsional Alfvén waves are more effective in this low-chromospheric fractionation process.

Conclusions:

  • The observed differences in elemental abundances likely originate from FIP fractionation low in the chromosphere.
  • The properties of waves and the location of fractionation significantly influence the composition of the slow solar wind.
  • Interchange reconnection models for slow solar wind generation need to account for the mixture of open and closed field line plasma and detailed reconnection processes.