Help Privacy Policy Disclaimer
  Advanced SearchBrowse


  Emission of solar chromospheric and transition region features related to the underlying magnetic field

Barczynski, K., Peter, H., Chitta, L. P., & Solanki, S. K. (2018). Emission of solar chromospheric and transition region features related to the underlying magnetic field. Astronomy and Astrophysics, 619: A5. doi:10.1051/0004-6361/201731650.

Item is


show Files




Barczynski, Krzysztof1, Author           
Peter, Hardi1, Author           
Chitta, L. P.1, Author           
Solanki, Sami K.1, 2, Author           
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              
2ERC Advanced Grant: Solar magnetic field and its influence on solar variability and activity (SOLMAG), Max Planck Institute for Solar System Research, Max Planck Society, ou_3164813              


Free keywords: Sun: chromosphere / Sun: transition region / Sun: magnetic fields / Sun: UV radiation / Sun: activity
 Abstract: Context. The emission of the upper atmosphere of the Sun is closely related to magnetic field concentrations at the solar surface.

Aims. It is well established that this relation between chromospheric emission and magnetic field is nonlinear. Here we investigate systematically how this relation, characterised by the exponent of a power-law fit, changes through the atmosphere, from the upper photosphere through the temperature minimum region and chromosphere to the transition region.

Methods. We used spectral maps from the Interface Region Imaging Spectrograph (IRIS) covering Mg II and its wings, C II, and Si IV together with magnetograms and UV continuum images from the Solar Dynamics Observatory. After a careful alignment of the data we performed a power-law fit for the relation between each pair of observables and determine the power-law index (or exponent) for these. This was done for different spatial resolutions and different features on the Sun.

Results. While the correlation between emission and magnetic field drops monotonically with temperature, the power-law index shows a hockey-stick-type variation: from the upper photosphere to the temperature-minimum it drops sharply and then increases through the chromosphere into the transition region. This is even seen through the features of the Mg II line, this is, from k1 to k2 and k3. It is irrespective of spatial resolution or whether we investigate active regions, plage areas, quiet Sun, or coronal holes.

Conclusions. In accordance with the general picture of flux–flux relations from the chromosphere to the corona, above the temperature minimum the sensitivity of the emission to the plasma heating increases with temperature. Below the temperature minimum a different mechanism has to govern the opposite trend of the power-law index with temperature. We suggest four possibilities, in other words, a geometric effect of expanding flux tubes filling the available chromospheric volume, the height of formation of the emitted radiation, the dependence on wavelength of the intensity-temperature relationship, and the dependence of the heating of flux tubes on the magnetic flux density.


Language(s): eng - English
 Dates: 2018
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1051/0004-6361/201731650
 Degree: -



Legal Case


Project information

show hide
Project name : ERC-2015-AdG - SOLMAG
Grant ID : 695075
Funding program : Horizon 2020 (H2020)
Funding organization : European Commission (EC)

Source 1

Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
Publ. Info: Les Ulis Cedex A France : EDP Sciences
Pages: - Volume / Issue: 619 Sequence Number: A5 Start / End Page: - Identifier: Other: 1432-0746
ISSN: 0004-6361
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1