@Article{RodriguezGomezVieiDalLPala:2018:CoElDe,
author = "Rodriguez Gomez, Jenny Marcela and Vieira, Lu{\'{\i}}s Eduardo
Antunes and Dal Lago, Alisson and Palacios, J.",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Universidad de Alcal{\'a}}",
title = "Coronal electron density temperature and solar spectral irradiance
during solar cycles 23 and 24",
journal = "Astrophysical Journal",
year = "2018",
volume = "852",
number = "2",
pages = "e137",
month = "jan.",
keywords = "Sun: corona, Sun: magnetic fields.",
abstract = "Plasma parameters such as the electron density and temperature
play a key role in the dynamics of the solar atmosphere. These
characteristics are important in solar physics because they can
help us to understand the physics of the solar corona, the
ultimate goal being the reconstruction of the electron density and
temperature distributions in the solar corona. The relations
between emission and plasma parameters in different timescales are
studied. We present a physics-based model to reconstruct the
density, temperature, and emission in the EUV band. This model,
called COronal DEnsity and Temperature (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 are the
recovery of SSI variability in specific wavelengths in the EUV
band, as well as the variations in density and temperature during
large timescales 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 solar
cycles 23 and 24 will be presented. The emission maps were
obtained and they are in accordance with the observations.
Additionally, the density and temperature maps are related to the
variations of the magnetic field in different layers through the
solar atmosphere.",
doi = "10.3847/1538-4357/aa9f1c",
url = "http://dx.doi.org/10.3847/1538-4357/aa9f1c",
issn = "0004-637X and 1538-4357",
language = "en",
targetfile = "rodriguez_coronal.pdf",
urlaccessdate = "27 abr. 2024"
}