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Coronal electron density, temperature and solar spectral irradiance during the solar cycle 23 and 24
Solar and Stellar Astrophysics · Submitted 11 Apr 2018
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The most important results of the current work that the recovery of SSI variability in specific wavelengths in the EUV band, also the variations in density and temperature in large time scale through the solar atmosphere, with the CODET model.
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The abstract, sentence by sentence
The plasma parameters such as the electron density and temperature plays a key role in the dynamics of the solar atmosphere. These characteristics are important in solar physics, because they can help to understand the physics in the solar corona. The goal is to reconstruct the electron density and temperature distributions in the solar corona. The relations between emission and plasma parameters in different time scales are studied. We present a physics-based model to reconstruct the density, temperature and emission in the EUV band. This model called CODET is composed of a flux transport model, an extrapolation model, an emission model and an optimization algorithm. The CODET model parameters were constrained by comparing the model's output to the TIMED/SEE record instead of direct observations because it covers a longer time interval than the direct solar observations currently available. The most important results of the current work that the recovery of SSI variability in specific wavelengths in the EUV band, also the variations in density and temperature in large time scale through the solar atmosphere, with the CODET model. The evolution of the electron density and temperature profiles through the solar corona in different layers during the solar cycle 23 and 24, will be presented. The emission maps were obtained and they are in accordance to the observations. Also, the density and temperature maps are related to the variations of the magnetic field in different layers through the solar atmosphere.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The plasma parameters such as the electron density and temperature plays a key role in the dynamics of the solar atmosphere. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | These characteristics are important in solar physics, because they can help to understand the physics in the solar corona. | background 1.00 | 0.04 | 0.02 | asserted 0.78 |
| s2 | The goal is to reconstruct the electron density and temperature distributions in the solar corona. | contribution 0.65 | 0.24 | 0.05 | asserted 0.84 |
| s3 | The relations between emission and plasma parameters in different time scales are studied. | contribution 0.63 | 0.69 | 0.03 | asserted 0.91 |
| s4 | We present a physics-based model to reconstruct the density, temperature and emission in the EUV band. | method 0.57 | 0.91 | 0.07 | asserted 1.00 |
| s5 | This model called CODET is composed of a flux transport model, an extrapolation model, an emission model and an optimization algorithm. | method 0.98 | 0.78 | 0.04 | asserted 1.00 |
| s6 | The CODET model parameters were constrained by comparing the model's output to the TIMED/SEE record instead of direct observations because it covers a longer time interval than the direct solar observations currently available. | method 0.98 | 0.81 | 0.04 | asserted 1.00 |
| s7 | The most important results of the current work that the recovery of SSI variability in specific wavelengths in the EUV band, also the variations in density and temperature in large time scale through the solar atmosphere, with the CODET model. | result 0.98 | 0.93 | 0.78 | asserted 0.96 |
| s8 | The evolution of the electron density and temperature profiles through the solar corona in different layers during the solar cycle 23 and 24, will be presented. | contribution 0.64 | 0.80 | 0.15 | asserted 0.89 |
| s9 | The emission maps were obtained and they are in accordance to the observations. | result 0.98 | 0.91 | 0.10 | asserted 0.96 |
| s10 | Also, the density and temperature maps are related to the variations of the magnetic field in different layers through the solar atmosphere. | result 0.85 | 0.81 | 0.11 | asserted 1.00 |
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The paper
Original abstract
The plasma parameters such as the electron density and temperature plays a key role in the dynamics of the solar atmosphere. These characteristics are important in solar physics, because they can help to understand the physics in the solar corona. The goal is to reconstruct the electron density and temperature distributions in the solar corona. The relations between emission and plasma parameters in different time scales are studied. We present a physics-based model to reconstruct the density, temperature and emission in the EUV band. This model called CODET is composed of a flux transport model, an extrapolation model, an emission model and an optimization algorithm. The CODET model parameters were constrained by comparing the model's output to the TIMED/SEE record instead of direct observations because it covers a longer time interval than the direct solar observations currently available. The most important results of the current work that the recovery of SSI variability in specific wavelengths in the EUV band, also the variations in density and temperature in large time scale through the solar atmosphere, with the CODET model. The evolution of the electron density and temperature profiles through the solar corona in different layers during the solar cycle 23 and 24, will be presented. The emission maps were obtained and they are in accordance to the observations. Also, the density and temperature maps are related to the variations of the magnetic field in different layers through the solar atmosphere.
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