Sunspots, Starspots, and Elemental Abundances

Element abundances in the solar photosphere, chromosphere, transition region, and corona are key parameters for investigating sources of the solar wind and for estimating radiative losses in the quiet corona and in dynamical events such as solar flares. Abundances in the solar corona and photosphere...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2017-07, Vol.844 (1), p.52
Main Authors: Doschek, G. A., Warren, H. P.
Format: Article
Language:English
Subjects:
Abundance
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHROMOSPHERE
Corona
ELEMENT ABUNDANCE
EXTREME ULTRAVIOLET RADIATION
First ionization potential
Ionization
IONIZATION POTENTIAL
PHOTOSPHERE
Shutdowns
SOLAR CORONA
SOLAR FLARES
SOLAR WIND
SPACE VEHICLES
Spacecraft
SPECTROMETERS
Starspots
SUN
Sun: activity
Sun: corona
Sun: flares
Sun: UV radiation
SUNSPOTS
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:Element abundances in the solar photosphere, chromosphere, transition region, and corona are key parameters for investigating sources of the solar wind and for estimating radiative losses in the quiet corona and in dynamical events such as solar flares. Abundances in the solar corona and photosphere differ from each other depending on the first ionization potential (FIP) of the element. Normally, abundances with FIP values less than about 10 eV are about 3-4 times more abundant in the corona than in the photosphere. However, recently, an inverse FIP effect was found in small regions near sunspots where elements with FIP less than 10 eV are less abundant relative to high FIP elements ( eV) than they are in the photosphere. This is similar to fully convective stars with large starspots. The inverse FIP effect is predicted to occur in the vicinity of sunspots/starspots. Up to now, the solar anomalous abundances have only been found in very spatially small areas. In this paper, we show that in the vicinity of sunspots there can be substantially larger areas with abundances that are between coronal and photospheric abundances and sometimes just photospheric abundances. In some cases, the FIP effect tends to shut down near sunspots. We examine several active regions with relatively large sunspots that were observed with the Extreme-ultraviolet Imaging Spectrometer on the Hinode spacecraft in cycle 24.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa7bea