Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. This page will automatically redirect to the new ADS interface at that point.

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic On-line Article (HTML)
· Table of Contents
· References in the Article
· Reads History
·
· Translate This Page
Title:
Modelling coronal electron density and temperature profiles based on solar magnetic field observations
Authors:
Rodríguez Gómez, J. M.; Antunes Vieira, L. E.; Dal Lago, A.; Palacios, J.; Balmaceda, L. A.; Stekel, T.
Affiliation:
AA(National Institute for Space Research (INPE), Avenida dos Astronautas-12227-010, São José dos Campos-SP, Brazil ), AB(National Institute for Space Research (INPE), Avenida dos Astronautas-12227-010, São José dos Campos-SP, Brazil),AC(National Institute for Space Research (INPE), Avenida dos Astronautas-12227-010, São José dos Campos-SP, Brazil), AD(Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain), AE(Instituto de Ciencias Astronómicas de la Tierra y el Espacio, ICATE-CONICET, Avda. de España Sur 1512, J5402DSP, San Juan, Argentina.), AF(National Institute for Space Research (INPE), Avenida dos Astronautas-12227-010, São José dos Campos-SP, Brazil)
Publication:
Living Around Active Stars, Proceedings of the International Astronomical Union, IAU Symposium, Volume 328, pp. 159-161
Publication Date:
10/2017
Origin:
CUP
Keywords:
Sun: magnetic fields, corona,
Abstract Copyright:
(c) 2017: Copyright © International Astronomical Union 2017
DOI:
10.1017/S1743921317003799
Bibliographic Code:
2017IAUS..328..159R

Abstract

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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints