Observations of CME-related phenomena in a wide spectral range |
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| Authors: | Email author" target="_blank">V?V?GrechnevEmail author V?G?Zandanov A?M?Uralov V?P?Maksimov V?G?Rudenko V?N?Borovik G?B?Gelfreikh I?Y?Grigorieva V?G?Medar A?N?Korzhavin |
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| Institution: | (1) Institute of Solar-Terrestrial Physics, P.O. Box 4026, Lermontov Street 126, Irkutsk, 664033, Russia;(2) Main (Pulkovo) Astronomical Observatory of RAS, St. Petersburg, Russia;(3) Special Astrophysical Observatory, St. Petersburg s Branch, St. Petersburg, Russia |
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| Abstract: | We study pre-eruptive, eruptive, and post-eruptive phenomena related to a CME that occurred on November 23, 2000 by means of joint analyses of data from various spectral ranges. Almost all known CME-associated phenomena were observed during this event, i.e., a filament eruption, solar flare, dimmings, and a post-eruptive arcade formation. Following a chain of events observed in various spectral ranges, we find that the event occurred in an activity complex consisting of active regions 9231 and 9238, and that it was triggered by a magnetic flux emergence, which caused a flare in AR 9231. In turn, the flare triggered activation and eruption of the filament followed by the CME and the flare in AR 9238 in which the post-eruptive arcade was observed. We discuss some characteristics of the flare and CME and also estimate the magnetic field strength in the coronal arcade to be about 200 G from spatially resolved polarization measurements in microwaves with radio telescopes. In this particular case, the only significant emission mechanism is optically thin free-free emission, and the possible contribution of nonthermal emissions cannot change our estimate of the magnetic field strength in the corona. However, generally one should make sure that the nonthermal contribution cannot be important in similar cases; otherwise, the magnetic field can be well overestimated. Here, we specifically address the identification technique of the radio emission mechanism. |
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