The altitude structure of the coronal magnetic field of AR 10933

被引：23

作者：

Kaltman, T. I. ^{[1
]}

Bogod, V. M. ^{[1
]}

Stupishin, A. G. ^{[2
]}

Yasnov, L. V. ^{[2
]}

机构：

[1] Russian Acad Sci, Special Astrophys Observ, St Petersburg Branch, St Petersburg 196140, Russia

[2] St Petersburg State Univ, St Petersburg, Russia

来源：

ASTRONOMY REPORTS | 2012年 / 56卷 / 10期

基金：

俄罗斯基础研究基金会;

关键词：

SOLAR ACTIVE REGIONS; VLA STEREOSCOPY; POLARIZATION; EMISSION; ATMOSPHERE; MODEL;

D O I：

10.1134/S1063772912100022

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The magnetic fields of solar active regions are analyzed using a method based on comparing the spatial structures of the reconstructed magnetic field and of the radio emission of the active region. Two approaches are used: comparing the radio size of the active region and the corresponding size calculated using the reconstructed magnetic field, and comparing the radio spectra that are observed and calculated using the reconstructed magnetic field. Overall, the calculated sizes and spectra correspond fairly well to the observational data, making it possible to estimate physical parameters of the emitting region, such as the electron density and temperature.

引用

页码：790 / 799

页数：10

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