The energy of waves in the photosphere and lower chromosphere IV. Inversion results of Ca II H spectra

Most semi-empirical static one-dimensional (1D) models of the solar atmosphere in the magnetically quiet Sun (QS) predict an increase in temperature at chromospheric layers. Numerical simulations of the solar chromosphere with a variable degree of sophistication, i.e. from 1D to three-dimensional (3...

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Published inAstronomy and astrophysics (Berlin) Vol. 553; pp. 1 - 17
Main Authors Beck, C, Rezaei, R, Puschmann, K G
Format Journal Article
LanguageEnglish
Published 01.05.2013
Subjects
Astronomy
Chromosphere
Computer simulation
Inversions
Mathematical models
Solar atmosphere
Spectra
Three dimensional
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Summary:Most semi-empirical static one-dimensional (1D) models of the solar atmosphere in the magnetically quiet Sun (QS) predict an increase in temperature at chromospheric layers. Numerical simulations of the solar chromosphere with a variable degree of sophistication, i.e. from 1D to three-dimensional (3D) simulations; assuming local thermal equilibrium (LTE) or non-LTE (NLTE), on the other hand, only yielded an increase in the brightness temperature without any stationary increase in the gas temperature. We investigate the thermal structure in the solar chromosphere as derived from an LTE inversion of observed Ca ii H spectra in QS and active regions (Ars). The temperature fluctuations in QS derived by the LTE inversion do not suffice on average to maintain a stationary chromospheric temperature rise. The spatially and vertically resolved information on the temperature structure allows one to investigate in detail the topology and evolution of the thermal structure in the lower solar atmosphere.
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ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201220463