Abstract
On 27 June 2012, an eruptive solar prominence was observed in the
extreme ultraviolet (EUV) and radio wavebands. At the Aalto University
Metsähovi Radio Observatory (MRO) it was observed at 37 GHz. It was
the first time that the MRO followed a radio prominence with dense
sampling in the millimetre wavelengths. This prompted us to study the
connection of the 37 GHz event with other wavelength domains. At 37 GHz,
the prominence was tracked to a height of around 1.6 R_{⊙}, at which
the loop structure collapsed. The average velocity of the radio
prominence was 55 ± 6 km s^{-1}. The brightness temperature of
the prominence varied between 800 ± 100 K and 3200 ± 100
K. We compared our data with the Solar Dynamic Observatory (SDO)/
Atmospheric Imaging Assembly (AIA) instrument's 304 Å EUV data,
and found that the prominence behaves very similarly in both
wavelengths. The EUV data also reveal flaring activity nearby the
prominence. We present a scenario in which this flare works as a trigger
that causes the prominence to move from a stable stage to an
acceleration stage.
Original language | English |
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Article number | 84 |
Number of pages | 8 |
Journal | Solar Physics |
Volume | 292 |
Issue number | 7 |
DOIs | |
Publication status | Published - 1 Jul 2017 |
MoE publication type | A1 Journal article-refereed |
Keywords
- Prominences
- active
- Radio emission
- active regions
- Chromosphere
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Metsähovi Radio Observatory
Tammi, J. (Manager)
School of Electrical EngineeringFacility/equipment: Facility