Models of the Solar Chromosphere and Transition Region from SUMER and HRTS Observations: Formation of the Extreme-Ultraviolet Spectrum of Hydrogen, Carbon, and Oxygen

364 citations recorded by the source corpus.

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

SEMIEMPIRICAL MODELS OF THE SOLAR ATMOSPHERE. III. SET OF NON-LTE MODELS FOR FAR-ULTRAVIOLET/EXTREME-ULTRAVIOLET IRRADIANCE COMPUTATION (2009, methodology): “The upper chromosphere for all models was assumed to consist of an almost constant temperature plateau as was proposed by Avrett & Loeser (2008).”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “(2013) use somewhat unrealistic chromospheric models, in that the degree of hydrogen ionization for a given density is lower than that in Avrett and Loeser (2008), at least for the models which come closest to matching observed abundance anomalies. Although the Avrett and Loeser (2008) model is quas”
Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle (2009, background): “Additionally, Avrett and Loeser (2008) have updated 1D atmosphere models for the averaged quiet Sun.”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, result): “This estimate agrees with the temperature profile recovered from observations of chromospheric lines (see, e.g., Fig.2 and Fig.8 in Avrett and Loeser (2008)).”