Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock
Ying,Beili1,2,3; Feng,Li1,2,4; Lu,Lei1; Zhang,Jie5; Magdalenic,Jasmina6; Su,Yingna1,2; Su,Yang1,2; Gan,Weiqun1,2
Source PublicationThe Astrophysical Journal
AbstractAbstract Large-scale solar eruptions have been extensively explored over many years. However, the properties of small-scale events with associated shocks have rarely been investigated. We present analyses of a small-scale, short-duration event originating from a small region. The impulsive phase of the M1.9-class flare lasted only four minutes. The kinematic evolution of the CME hot channel reveals some exceptional characteristics, including a very short duration of the main acceleration phase (<2 minutes), a rather high maximal acceleration rate (~50 km s?2), and peak velocity (~1800 km s?1). The fast and impulsive kinematics subsequently results in a piston-driven shock related to a metric type II radio burst with a high starting frequency of ~320 MHz of the fundamental band. The type II source is formed at a low height of below 1.1?R⊙ less than ~2 minutes after the onset of the main acceleration phase. Through the band-split of the type II burst, the shock compression ratio decreases from 2.2 to 1.3, and the magnetic field strength of the shock upstream region decreases from 13 to 0.5 Gauss at heights of 1.1–2.3 R⊙. We find that the CME (~4 × 1030 erg) and flare (~1.6 × 1030 erg) consume similar amounts of magnetic energy. The same conclusion for large-scale eruptions implies that small- and large-scale events possibly share a similar relationship between CMEs and flares. The kinematic particularities of this event are possibly related to the small footpoint-separation distance of the associated magnetic flux rope, as predicted by the Erupting Flux Rope model.
Keywordshock waves Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares
WOS IDIOP:0004-637X-856-1-aaadaf
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210008 Nanjing, People’s Republic of China;
2.School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, People’s Republic of China
3.Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077, G?ttingen, Germany
4.State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China
5.Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030, USA
6.Solar-Terrestrial Center of Excellence–SIDC, Royal Observatory of Belgium, Av. Circulaire 3, B-1180 Brussels, Belgium
Recommended Citation
GB/T 7714
Ying,Beili,Feng,Li,Lu,Lei,et al. Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock[J]. The Astrophysical Journal,2018,856(1).
APA Ying,Beili.,Feng,Li.,Lu,Lei.,Zhang,Jie.,Magdalenic,Jasmina.,...&Gan,Weiqun.(2018).Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock.The Astrophysical Journal,856(1).
MLA Ying,Beili,et al."Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock".The Astrophysical Journal 856.1(2018).
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