Coronal Density and Temperature Profiles Calculated by Forward Modeling EUV Emission Observed by SDO/AIA

We present a model for the intensity of optically thin extreme ultraviolet (EUV) emission for a plasma atmosphere. We apply our model to the solar corona as observed using the six optically thin EUV channels of the Solar Dynamics Observatory/Atmospheric Imaging Assembly instrument. The emissivity of...

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Bibliographic Details
Published in:The Astrophysical journal 2019-10, Vol.884 (1), p.43
Main Authors: Pascoe, D. J., Smyrli, A., Van Doorsselaere, T.
Format: Article
Language:English
Subjects:
Astrophysics
Atmospheric models
Corona
Coronal density
Coronal holes
Density
Emission
Emission measurements
Emissivity
Field strength
Inversions
Magnetic fields
Magnetic properties
Plasma
Seismology
Solar activity
Solar corona
Solar observatories
Sun: atmosphere
Sun: corona
Sun: magnetic fields
Sun: UV radiation
Temperature
Temperature profiles
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Summary:We present a model for the intensity of optically thin extreme ultraviolet (EUV) emission for a plasma atmosphere. We apply our model to the solar corona as observed using the six optically thin EUV channels of the Solar Dynamics Observatory/Atmospheric Imaging Assembly instrument. The emissivity of the plasma is calculated from the density and temperature using CHIANTI tables and the intensity is then determined by integration along the line of sight. We consider several different profiles for the radial density and temperature profiles, each of which are constrained by the observational data alone with no further physical assumptions. We demonstrate the method first by applying it to a quiet region of the corona, and then use it as the background component of a model including coronal holes, allowing the plasma densities and temperatures inside and outside the hole to be estimated. We compare our results with differential emission measure inversions. More accurate estimates for the coronal density and temperature profiles have the potential to help constrain plasma properties such as the magnetic field strength when used in combination with methods such as seismology.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ab3e39