Strong magnetic fields in solar flares - Observational data and a theoretical model

Details Strong magnetic fields in solar flares - Observational data and a theoretical model Strong magnetic fields in solar flares - Observational data and a theoretical model

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991kfnt....7...40l&link_type=abstract

Kinematika i Fizika Nebesnykh Tel (ISSN 0233-7665), vol. 7, Nov.-Dec. 1991, p. 40-47. In Russian.

Physics

3

Circular Polarization, Solar Flares, Solar Magnetic Field, Solar Spectra, Spectral Line Width, Emission Spectra, Magnetic Field Configurations, Solar Atmosphere, Zeeman Effect

Scientific paper

Spectral observations of five solar flares in 1981 and 1989 performed with a circular polarization analyzer are studied. Direct measurements of the Zeeman splitting of the emission in the Fe I, Fe II, Na I, He I, and H I lines show that the strength of the longitudinal magnetic field is in the range between 10-20 and 350 mT. At the He I emission formation level, the magnetic strength is 120-180 mT. It is argued that the strong magnetic fields in flares arise owing to the magnetic tube twists in the upper layer of the solar atmosphere.

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