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Spectropolarimetric capabilities of Ca II 8542 angstrom line
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi.
Vise andre og tillknytning
Rekke forfattare: 7
2016 (engelsk)Inngår i: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 459, nr 3, 3363-3376 s.Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

The next generation of space-and ground-based solar missions aim to study the magnetic properties of the solar chromosphere using the infrared Ca II lines and the He I 10830 angstrom line. The former seem to be the best candidates to study the stratification of magnetic fields in the solar chromosphere and their relation to the other thermodynamical properties underlying the chromospheric plasma. The purpose of this work is to provide a detailed analysis of the diagnostic capabilities of the Ca II 8542 angstrom line, anticipating forthcoming observational facilities. We study the sensitivity of the Ca II 8542 angstrom line to perturbations applied to the physical parameters of reference semi-empirical 1D model atmospheres using response functions and we make use of 3D magnetohydrodynamics simulations to examine the expected polarization signals for moderate magnetic field strengths. Our results indicate that the Ca II 8542 angstrom line is mostly sensitive to the layers enclosed in the range log tau = [0, -5.5], under the physical conditions that are present in our model atmospheres. In addition, the simulated magnetic flux tube generates strong longitudinal signals in its centre and moderate transversal signals, due to the vertical expansion of magnetic field lines, in its edge. Thus, observing the Ca II 8542 angstrom line we will be able to infer the 3D geometry of moderate magnetic field regions.

sted, utgiver, år, opplag, sider
2016. Vol. 459, nr 3, 3363-3376 s.
Emneord [en]
techniques: polarimetric, Sun: chromosphere, Sun: magnetic fields
HSV kategori
Identifikatorer
URN: urn:nbn:se:su:diva-133240DOI: 10.1093/mnras/stw867ISI: 000379840900082OAI: oai:DiVA.org:su-133240DiVA: diva2:957950
Tilgjengelig fra: 2016-09-05 Laget: 2016-09-05 Sist oppdatert: 2016-09-05bibliografisk kontrollert

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