Multiwavelength Analysis of the Kinematics of a Long Duration Flare-CME Event on 27 January 2012
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Multiwavelength Analysis of the Kinematics of a Long Duration Flare-CME Event on 27 January 2012 G. Selvarani1 · S. Prasanna Subramanian2 A. Shanmugaraju3 · K. Suresh3
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Received: 26 April 2019 / Accepted: 18 August 2020 © Springer Nature B.V. 2020
Abstract We present a detailed analysis of a long-duration flare associated with a coronal mass ejection (CME) event that occurred on 27 January 2012 in the active region (AR) 11402. We analyze the kinematics of the CME and the close relationship between the flare, radio burst, and CME. We used STEREO (Solar Terrestrial Relations Observatory)/EUVI A (Extreme Ultraviolet Imager) and white light data from STEREO (COR1 A and COR2 A) and LASCO (Large Angle and Spectrometric COronagraph) (C2/C3) coronagraphs, and X-ray data from the GOES (Geostationary Operational Environmental Satellite) spacecraft. The height of the CME is measured using the Graduated Cylindrical Shell (GCS) model. Our results show that: i) the speed of the CME (1460 km/s at 2.54 R ) is comparable to the speed of the type II radio burst (1581 km/s), ii) the height of the type II radio burst is lower than that of the CME leading edge, iii) the CME acceleration phase is found to be related to the rise time of the flare and its propagation phase is related to the decay phase of the flare, iv) the type II radio burst origin is likely to be near the CME region where a CME-streamer interaction takes place around 1.6 R , and v) the sequence of events and the CME kinematics show a close association between the CME and type II radio emissions. Keywords CME · CME-streamer interaction · LDE flare · Type II radio burst
1. Introduction Coronal mass ejections (CMEs) are eruptive phenomena in the corona that involve a large number of free electrons and an extended magnetic field from the Sun (MacQueen, 1980). They play a vital role in accelerating solar energetic particles (SEPs) and producing coronal and interplanetary shocks (Kahler, 1992). Additionally they have a severe impact on space
B G. Selvarani
[email protected]
1
Department of Physics, Sri Meenakshi Govt. Arts College for Women, Madurai-2, India
2
Radio Astronomy Centre, Ooty 634 004, India
3
Arul Anandar College, Karumathur 625 514, Madurai Dist., India
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weather. When CMEs propagate close to the Sun-Earth line, or are very wide events, they can be seen as halo CMEs. Generally, halo CMEs are faster and more energetic when compared to other CMEs (Gopalswamy et al., 2013). Three dimensional structures of CMEs have been understood thanks to the twin Solar Terrestrial Relations Observatory (STEREO) data (Howard et al., 2008), taken from much closer to the Sun up to 1 AU (Gopalswamy et al., 2009; Patsourakos, Vourlidas, and Stenborg, 2010; Harrison and Davies, 2014). These observations also help us to find the initial acceleration of CMEs (Bein et al., 2011). Many of the CMEs are related to flares (Gosling, 1990). The relationship between flares and CMEs during the initiation, impulsive acceleration, a
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