首页|Observational evidence of magnetic reconnection in a coronal bright point

Observational evidence of magnetic reconnection in a coronal bright point

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Magnetic reconnection is considered to be the fundamental process by which magnetic energy is converted into plasma or particle kinetic energy.Magnetic reconnection is a widely applied physics model to explain the solar eruption events,such as coronal bright points(CBPs).Meanwhile,it is an usual way of the solar physics research to look for the observational evidences of magnetic reconnection in the solar eruption events in order to support the model.In this paper,we have explored the evidences of magnetic reconnection in a CBP observed by the Atmospheric Imaging Assembly(AIA)onboard the Solar Dynamics Observatory(SDO)at NOAA No.11163 on 2011 March 5.Our observations show that this event is a small-scale loop system in active regions that have similar size as a traditional CBP and it might shed light on the physics of a traditional CBP.This CBP is bright in all nine AIA wavelengths and displays a flaring development with three bursts intermittently.Each burst exhibits a pair of bi-directional jets almost along a line.They originate from the same position(CBP core),then move in the opposite directions.Our findings are well consistent with the magnetic reconnection process by which the bi-directional plasma outflows are produced and radiate the bi-directional jets detected by SDO/AIA.These facts further support the conclusion that the CBP is produced by the magnetic reconnection process.

Sun:UV radiationSuncoronaSunoscillation

宁宗军、李东、张擎旻

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Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Nanjing 210033,China

This work is funded by the National Natural Science Foundation of ChinaThis work is funded by the National Natural Science Foundation of ChinaThis work is funded by the National Natural Science Foundation of ChinaThis work is funded by the National Natural Science Foundation of ChinaLaboratory

NSFC1117306211333009115730722010DP173032

2020

10.1088/1674-4527/20/9/138

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCDCSCDSCI
影响因子：0.406
ISSN：1674-4527
年,卷(期)：2020.20(9)
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