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Stockholm University, Faculty of Science, Department of Astronomy.
Number of Authors: 4
2015 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 810, no 2, 145Article in journal (Refereed) Published
Abstract [en]

Magnetic flux emergence into the outer layers of the Sun is a fundamental mechanism for releasing energy into the chromosphere and the corona. In this paper, we study the emergence of granular-sized flux concentrations and the structuring of the corresponding physical parameters and atmospheric diagnostics in the upper photosphere and in the chromosphere. We make use of a realistic 3D MHD simulation of the outer layers of the Sun to study the formation of the Ca II 8542 line. We also derive semi-empirical 3D models from non-LTE inversions of our observations. These models contain information on the line-of-sight stratifications of temperature, velocity, and the magnetic field. Our analysis explains the peculiar Ca II 8542 angstrom profiles observed in the flux emerging region. Additionally, we derive detailed temperature and velocity maps describing the ascent of a magnetic bubble from the photosphere to the chromosphere. The inversions suggest that, in active regions, granular-sized bubbles emerge up to the lower chromosphere where the existing large-scale field hinders their ascent. We report hints of heating when the field reaches the chromosphere.

Place, publisher, year, edition, pages
2015. Vol. 810, no 2, 145
Keyword [en]
line: formation, polarization, radiative transfer, Sun: chromosphere, Sun: magnetic fields
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-122127DOI: 10.1088/0004-637X/810/2/145ISI: 000362083700061OAI: diva2:865551
Available from: 2015-10-28 Created: 2015-10-26 Last updated: 2015-10-28Bibliographically approved

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de la Cruz Rodriguez, Jaime
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ReferencesLink to record
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