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The connection between solar coronal abundances and the underlying lower atmospheric properties
Paola Testa1, Juan Martinez-Sykora2,3,4,5, Bart De Pontieu3,4,5
1Harvard-Smithsonian Center for Astrophysics , Cambridge, MA, USA.
Summary
The solar corona and wind show different elemental abundances than the photosphere, with low first ionization potential (FIP) elements often enhanced. This FIP effect likely originates in the chromosphere due to ionization differences.
Area of Science:
- Solar physics
- Plasma astrophysics
- Planetary science
Background:
- Solar corona and solar wind elemental abundances differ from photospheric values.
- A common observation is the enhancement of low first ionization potential (FIP) elements, known as the FIP effect.
- This fractionation is linked to chemical processes in the solar atmosphere.
Purpose of the Study:
- Investigate the connection between chemical fractionation and the FIP effect.
- Explore the chromospheric origin of the FIP effect.
- Examine observational evidence for coronal abundance anomalies in the lower solar atmosphere.
Main Methods:
- Review recent observational studies on solar atmospheric abundances.
- Analyze data linking coronal abundance anomalies to lower atmospheric conditions.
- Discuss the role of ionization states of elements in the chromosphere.
Main Results:
- Observational evidence suggests the FIP effect originates in the chromosphere.
- Low-FIP elements are preferentially ionized and fractionated compared to high-FIP elements.
- Coronal abundance anomalies may have a footprint in the lower solar atmosphere.
Conclusions:
- The chromosphere is a likely site for the mechanisms causing the FIP effect.
- Further observations are needed to fully understand the FIP effect and its lower atmospheric signatures.
- Addressing this open issue in solar physics requires continued research and advanced observational techniques.
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