Modelling coronal electron density and temperature profiles based on solar magnetic field observations

J. M.Rodríguez Gómez, L. E.Antunes Vieira, A. Dal Lago, J. Palacios, L. A. Balmaceda, T. Stekel

Результат исследований: Вклад в журналСтатьярецензирование

Аннотация

The density and temperature profiles in the solar corona are complex to describe, the observational diagnostics is not easy. Here we present a physics-based model to reconstruct the evolution of the electron density and temperature in the solar corona based on the configuration of the magnetic field imprinted on the solar surface. The structure of the coronal magnetic field is estimated from Potential Field Source Surface (PFSS) based on magnetic field from both observational synoptic charts and a magnetic flux transport model. We use an emission model based on the ionization equilibrium and coronal abundances from CHIANTI atomic database 8.0. The preliminary results are discussed in details.

Язык оригиналаАнглийский
Страницы (с-по)159-161
Число страниц3
ЖурналProceedings of the International Astronomical Union
Том12
DOI
СостояниеОпубликовано - 2016
Опубликовано для внешнего пользованияДа

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