Coronal Heating and Solar Wind Formation in Quiet Sun and Coronal Holes: A Unified Scenario

Coronal holes (CHs) are darker than the quiet Sun (QS) when observed in coronal channels. This study aims to understand the similarities and differences between CHs and QS in the transition region using the Si iv  1394 Å line, recorded by the Interface Region Imaging Spectrograph, by considering the...

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Bibliographic Details
Published in:The Astrophysical journal 2021-02, Vol.908 (1), p.28
Main Authors: Tripathi, Durgesh, Nived, V. N., Solanki, Sami K
Format: Article
Language:English
Subjects:
Astrophysics
Corona
Coronal heating
Coronal holes
Fast solar wind
Fluctuations
Flux density
Heating
Magnetic fields
Magnetic flux
Magnetism
Quiet Sun
Slow solar wind
Solar activity
Solar corona
Solar coronal heating
Solar coronal holes
Solar magnetic fields
Solar observatories
Solar transition region
Solar wind
Sun
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Summary:Coronal holes (CHs) are darker than the quiet Sun (QS) when observed in coronal channels. This study aims to understand the similarities and differences between CHs and QS in the transition region using the Si iv  1394 Å line, recorded by the Interface Region Imaging Spectrograph, by considering the distribution of magnetic field measured by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. We find that Si iv intensities obtained in CHs are lower than those obtained in QS for regions with identical magnetic flux densities. Moreover, the difference in intensities between CHs and QS increases with increasing magnetic flux. For the regions with equal magnetic flux density, QS line profiles are more redshifted than those measured in CHs. Moreover, the blueshifts measured in CHs show an increase with increasing magnetic flux density unlike in the QS. The non-thermal velocities in QS, as well as in CHs, show an increase with increasing magnetic flux. However, no significant difference was observed in QS and CHs, albeit a small deviation at small flux densities. Using these results, we propose a unified model for the heating of the corona in the QS and in CHs and the formation of solar wind.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abcc6b