Change search
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf
Comparison of Solar Fine Structure Observed Simultaneously in Ly alpha and MgII h
Stockholm University, Faculty of Science, Department of Astronomy. University of Oslo, Norway.
Show others and affiliations
Number of Authors: 132017 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 847, no 2, article id 141Article in journal (Refereed) Published
Abstract [en]

The Chromospheric Lyman Alpha Spectropolarimeter (CLASP) observed the Sun in H I Ly alpha during a suborbital rocket flight on 2015 September 3. The Interface Region Imaging Telescope (IRIS) coordinated with the CLASP observations and recorded nearly simultaneous and co-spatial observations in the Mg II h and k lines. The Mg II h and Lya lines are important transitions, energetically and diagnostically, in the chromosphere. The canonical solar atmosphere model predicts that these lines form in close proximity to each other and so we expect that the line profiles will exhibit similar variability. In this analysis, we present these coordinated observations and discuss how the two profiles compare over a region of quiet Sun at viewing angles that approach the limb. In addition to the observations, we synthesize both line profiles using a 3D radiation-MHD simulation. In the observations, we find that the peak width and the peak intensities are well correlated between the lines. For the simulation, we do not find the same relationship. We have attempted to mitigate the instrumental differences between IRIS and CLASP and to reproduce the instrumental factors in the synthetic profiles. The model indicates that formation heights of the lines differ in a somewhat regular fashion related to magnetic geometry. This variation explains to some degree the lack of correlation, observed and synthesized, between Mg II and Lya. Our analysis will aid in the definition of future observatories that aim to link dynamics in the chromosphere and transition region.

Place, publisher, year, edition, pages
2017. Vol. 847, no 2, article id 141
Keywords [en]
Sun: chromosphere, Sun: transition region, Sun: UV radiation
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-148867DOI: 10.3847/1538-4357/aa890bISI: 000412267900011OAI: oai:DiVA.org:su-148867DiVA, id: diva2:1159244
Available from: 2017-11-22 Created: 2017-11-22 Last updated: 2017-11-22Bibliographically approved

Open Access in DiVA

No full text in DiVA

Other links

Publisher's full text
By organisation
Department of Astronomy
In the same journal
Astrophysical Journal
Physical Sciences

Search outside of DiVA

GoogleGoogle Scholar

doi
urn-nbn

Altmetric score

doi
urn-nbn
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf