The energy of waves in the photosphere and lower chromosphere

2013/02/27 by C. Beck, R. Rezaei, K. G. Puschmann
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Atmosphere (unit) #Atmospheric sciences #Chromosphere #Meteorology #Optics #Photosphere #Physics #Radiative equilibrium #Radiative transfer #Solar and Space Plasma Dynamics #Spectral line #Stellar, planetary, and galactic studies #astro-ph.SR

paper · pdf · doi:10.1051/0004-6361/201220463

published as Astronomy and Astrophysics, Vol. 553, A73, 2013 · 16 pages, 16 figures + 1 page Appendix, accepted by A&A

arxiv created 2013/02/27 · openalex publication_date 2013/03/27 · arxiv updated 2013/05/08 · openalex created_date 2022/10/02 · openalex updated_date 2026/06/11

Abstract

Context. 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.

Citations

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