We investigate the oscillations in active region(AR)NOAA 12891,which produces a C2.0 three-ribbon flare accompanying a jet on 2021 November 2.Using the data from the Atmospheric Imaging Assembly onboard the Solar Dyna...We investigate the oscillations in active region(AR)NOAA 12891,which produces a C2.0 three-ribbon flare accompanying a jet on 2021 November 2.Using the data from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory,the 5 minutes decayless kink oscillations of coronal loops were detected and they are independent of the solar flare.Based on the observed oscillations and seismological diagnostics,we estimate that the Alfvén speed and magnetic field in these coronal loops are around 466 kms^(-1) sand 7.6 G,respectively.Additionally,the flare-related jet shows its plasmoids with 1 minute periodicity same as the intensity fluctuation of nearby flare ribbon.The correlation between the intensity fluctuation of jet and that of flare ribbon indicates that their 1 minute oscillations should originate from the same reconnection process.展开更多
We report multi-wavelength observations of four solar flares on 2014 July 07.We firstly select these flares according to the soft X-ray(SXR)and extreme ultraviolet(EUV)emissions recorded by the Extreme Ultraviolet Var...We report multi-wavelength observations of four solar flares on 2014 July 07.We firstly select these flares according to the soft X-ray(SXR)and extreme ultraviolet(EUV)emissions recorded by the Extreme Ultraviolet Variability Experiment and Geostationary Orbiting Environmental S atellites.Then their locations and geometries are identified from the full-disk images measured by the Atmospheric Imaging Assembly(AIA),and the time delays among the light curves in different channels are identified.The electron number densities are estimated using the differential emission measure method.We find that three of four flares show strong emissions in SXR channels and high temperature(>6 MK)EUV wavelengths during the impulsive phase,i.e.,AIA 131 A and 94 A,and then they emit peak radiation subsequently in the middle temperature(~0.6-3 MK)EUV channels.Moreover,they last for a long time and have smaller electron densities,which are probably driven by the interaction of hot diffuse flare loops.Only one flare emits radiation at almost the same time in all the observed wavelengths,lasts for a relatively short time,and has a larger electron density.It is also accompanied by a typeⅢradio burst.The bright emission at the EUV channel could be corresponding to the associated erupting filament.展开更多
Small-scale, cyclic, transverse motions of plasma threads are usually seen in solar prominences, which are often interpreted as magnetohydrodynamic(MHD) waves. Here, we observed small-scale decayless transverse oscill...Small-scale, cyclic, transverse motions of plasma threads are usually seen in solar prominences, which are often interpreted as magnetohydrodynamic(MHD) waves. Here, we observed small-scale decayless transverse oscillations in a quiescent prominence, and they appear to be omnipresent. The oscillatory periods of the emission intensity and a proxy for the line-of-sight Doppler shift are about half period of the displacement oscillations. This feature agrees well with the fast kink-mode waves in a flux tube. All the moving threads oscillate transversally spatially in phase and exhibit no significant damping throughout the visible segments, indicating that the fast kink MHD waves are persistently powered and ongoing dissipating energy is transferred to the ambient plasma in the quiet corona. However, our calculations suggest that the energy taken by the fast kink MHD waves alone can not support the coronal heating on the quiet Sun.展开更多
基金funded by NSFC under Grant Nos.12073081,11973092 and 11790302CAS Strategic Pioneer Program on Space Science under Grant Nos.XDA15052200 and XDA15320301supported by Surface Project of Jiangsu No.BK20211402。
文摘We investigate the oscillations in active region(AR)NOAA 12891,which produces a C2.0 three-ribbon flare accompanying a jet on 2021 November 2.Using the data from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory,the 5 minutes decayless kink oscillations of coronal loops were detected and they are independent of the solar flare.Based on the observed oscillations and seismological diagnostics,we estimate that the Alfvén speed and magnetic field in these coronal loops are around 466 kms^(-1) sand 7.6 G,respectively.Additionally,the flare-related jet shows its plasmoids with 1 minute periodicity same as the intensity fluctuation of nearby flare ribbon.The correlation between the intensity fluctuation of jet and that of flare ribbon indicates that their 1 minute oscillations should originate from the same reconnection process.
基金supported by the National Natural Science Foundation of China(Grant Nos.11973092,11790300,11790302,11729301 and12073081)the Strategic Priority Research Program on Space Science,Chinese Academy of Sciences(Grant Nos.XDA15052200 and XDA15320301)+2 种基金supported by the Specialized Research Fund for State Key Laboratories and CAS Strategic Pioneer Program on Space Science(KLSA202003)The Laboratory No.is2010DP173032.supported by DLR(Grant No.50 QL 1701)。
文摘We report multi-wavelength observations of four solar flares on 2014 July 07.We firstly select these flares according to the soft X-ray(SXR)and extreme ultraviolet(EUV)emissions recorded by the Extreme Ultraviolet Variability Experiment and Geostationary Orbiting Environmental S atellites.Then their locations and geometries are identified from the full-disk images measured by the Atmospheric Imaging Assembly(AIA),and the time delays among the light curves in different channels are identified.The electron number densities are estimated using the differential emission measure method.We find that three of four flares show strong emissions in SXR channels and high temperature(>6 MK)EUV wavelengths during the impulsive phase,i.e.,AIA 131 A and 94 A,and then they emit peak radiation subsequently in the middle temperature(~0.6-3 MK)EUV channels.Moreover,they last for a long time and have smaller electron densities,which are probably driven by the interaction of hot diffuse flare loops.Only one flare emits radiation at almost the same time in all the observed wavelengths,lasts for a relatively short time,and has a larger electron density.It is also accompanied by a typeⅢradio burst.The bright emission at the EUV channel could be corresponding to the associated erupting filament.
基金supported by the National Natural Science Foundation of China(Grant Nos.11973092,12173012,12111530078,12073081,U1631242,11820101002,11790302,and U1731241)the CAS Strategic Priority Research Program on Space Science(Grant Nos.XDA15052200,XDA15320103,and XDA15320301)+3 种基金supported by the CAS Key Laboratory of Solar Activity(Grant No.KLSA202003)the Surface Project of Jiangsu Province(Grant No.BK20211402)supported by the Shenzhen Technology Project(Grant No.GXWD20201230155427003-20200804151658001)The Laboratory No.is 2010DP173032。
文摘Small-scale, cyclic, transverse motions of plasma threads are usually seen in solar prominences, which are often interpreted as magnetohydrodynamic(MHD) waves. Here, we observed small-scale decayless transverse oscillations in a quiescent prominence, and they appear to be omnipresent. The oscillatory periods of the emission intensity and a proxy for the line-of-sight Doppler shift are about half period of the displacement oscillations. This feature agrees well with the fast kink-mode waves in a flux tube. All the moving threads oscillate transversally spatially in phase and exhibit no significant damping throughout the visible segments, indicating that the fast kink MHD waves are persistently powered and ongoing dissipating energy is transferred to the ambient plasma in the quiet corona. However, our calculations suggest that the energy taken by the fast kink MHD waves alone can not support the coronal heating on the quiet Sun.
