Modelling coronal electron density and temperature profiles of the Active Region NOAA 11855

The magnetic flux emergence can help understand the physical mechanism responsible for solar atmospheric phenomena. Emerging magnetic flux is frequently related to eruptive events, because when emerging they can reconnected with the ambient field and release magnetic energy. We will use a physic-bas...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2016-10, Vol.12 (S328), p.149-151
Main Authors: Gómez, J. M. Rodríguez, Vieira, L. E. Antunes, Dal Lago, A., Palacios, J., Balmaceda, L. A., Stekel, T.
Format: Article
Language:English
Subjects:
Astronomy
Atmospheric models
Atomic structure
Contributed Papers
Electron density
Emission
Energy consumption
Magnetic fields
Magnetic flux
Magnetism
Photosphere
Plasma temperature
Solar corona
Solar magnetic field
Spacecraft
Temperature profiles
Wavelengths
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Summary:The magnetic flux emergence can help understand the physical mechanism responsible for solar atmospheric phenomena. Emerging magnetic flux is frequently related to eruptive events, because when emerging they can reconnected with the ambient field and release magnetic energy. We will use a physic-based model to reconstruct the evolution of the solar emission based on the configuration of the photospheric magnetic field. The structure of the coronal magnetic field is estimated by employing force-free extrapolation NLFFF based on vector magnetic field products (SHARPS) observed by HMI instrument aboard SDO spacecraft from Sept. 29 (2013) to Oct. 07 (2013). The coronal plasma temperature and density are described and the emission is estimated using the CHIANTI atomic database 8.0. The performance of the our model is compared to the integrated emission from the AIA instrument aboard SDO spacecraft in the specific wavelengths 171Å and 304Å.
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921317003842