Large-Amplitude Oscillation of an Erupting Filament as Seen in EUV,Hα, and Microwave Observations |
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| Authors: | H Isobe D Tripathi A Asai R Jain |
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| Institution: | (1) Department of Earth and Planetary Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan;(2) Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Wilberforce Road, Cambridge, CB3 0WA, UK;(3) Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano 384-1305, Japan;(4) Department of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK |
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| Abstract: | We present multiwavelength observations of a large-amplitude oscillation of a polar-crown filament on 15 October 2002, which
has been reported by Isobe and Tripathi (Astron. Astrophys.
449, L17, 2006). The oscillation occurred during the slow rise (≈1 km s−1) of the filament. It completed three cycles before sudden acceleration and eruption. The oscillation and following eruption
were clearly seen in observations recorded by the Extreme-Ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO). The oscillation was seen only in a part of the filament, and it appears to be a standing oscillation rather than
a propagating wave. The amplitudes of velocity and spatial displacement of the oscillation in the plane of the sky were about
5 km s−1 and 15 000 km, respectively. The period of oscillation was about two hours and did not change significantly during the oscillation.
The oscillation was also observed in Hα by the Flare Monitoring Telescope at the Hida Observatory. We determine the three-dimensional
motion of the oscillation from the Hα wing images. The maximum line-of-sight velocity was estimated to be a few tens of kilometers
per second, although the uncertainty is large owing to the lack of line-profile information. Furthermore, we also identified
the spatial displacement of the oscillation in 17-GHz microwave images from Nobeyama Radio Heliograph (NoRH). The filament
oscillation seems to be triggered by magnetic reconnection between a filament barb and nearby emerging magnetic flux as was
evident from the MDI magnetogram observations. No flare was observed to be associated with the onset of the oscillation. We
also discuss possible implications of the oscillation as a diagnostic tool for the eruption mechanisms. We suggest that in
the early phase of eruption a part of the filament lost its equilibrium first, while the remaining part was still in an equilibrium
and oscillated. |
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| Keywords: | Prominences: dynamics Oscillations Coronal seismology |
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