Solar atmospheric responses to magnetic flux eruptions. I - A mechanism for coronal mass ejections. II - Slow shocks near the sun

Details Solar atmospheric responses to magnetic flux eruptions. I - A mechanism for coronal mass ejections. II - Slow shocks near the sun Solar atmospheric responses to magnetic flux eruptions. I - A mechanism for coronal mass ejections. II - Slow shocks near the sun

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991acaps..11..181h&link_type=abstract

(Acta Astrophysica Sinica, vol. 11, no. 2, 1991, p. 181-186, 188-193) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol.

Astronomy and Astrophysics

Astrophysics

Magnetic Flux, Shock Waves, Solar Atmosphere, Solar Magnetic Field, Stellar Mass Ejection, Coronal Loops, Magnetoelastic Waves, Magnetosonic Resonance, Mathematical Models, Wave Propagation

Scientific paper

A numerical simulation of the atmospheric responses to magnetic flux eruptions at the solar base coronal streamers is reported. The results show that flux eruptions may be an important mechanism in generating such events and reveal the density structure within the loop and the relevant dynamical effects and the wave phenomenon in front of the loop. Spectral analyses of a volume of type III burst groups are reported which show that periodicity is a general phenomenon among the meter wave type III burst groups. It is also shown that most of these events have multiple periods and that the periods discovered are all rather short. A study of the correlations among the periodicity, polarization, and source size shows that the type III burst groups can be divided into groups with weak polarization, wide periodicity, and large sources and a group with strong polarization, short periodicity, and single and compact sources.

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