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Homologous large-amplitude Nonlinear fast-mode Magnetosonic Waves Driven by Recurrent Coronal Jets  

Yuandeng Shen   Submitted: 2018-06-07 06:25

The detailed observational analysis of a homologous Extreme-ultraviolet (EUV) wave event is presented to study the driving mechanism and the physical property of the EUV waves, combining high resolution data taken by the Solar Dynamics Observatory and the Solar TErrestrial RElations Observatory. It is observed that four homologous EUV waves originated from the same active region AR11476 within about one hour, and the time separations between consecutive waves were of 8 - 20 minutes. The waves showed narrow arc-shaped wavefronts and propagated in the same direction along a large-scale transequatorial loop system at a speed of 648 - 712 km s-1 and a deceleration of 0.985 - 1.219 km s-12. The EUV waves were accompanied by weak flares, coronal jets, and radio type III bursts, in which the EUV waves were delayed with respect to the start times of the radio type III bursts and coronal jets about 2 - 13 and 4 - 9 minutes, respectively. Different to previous studies of homologous EUV waves, no coronal mass ejections were found in the present event. Based on the observational results and the close temporal the spatial relationship between the EUV waves and the coronal jets, for the first time, we propose that the observed homologous EUV waves were large-amplitude nonlinear fast-mode magnetosonic waves or shocks driven by the associated recurrent coronal jets, resemble the generation mechanism of a piston shock in a tube. In addition, it is found that the recurrent jets were tightly associated with the alternating flux cancellation and emergence in the eruption source region and radio type III bursts.

Authors: Yuandeng Shen; Yu Liu; Ying D. Liu; Jiangtao Su; Zehao Tang; Yuhu Miao
Projects: SDO-AIA

Publication Status: accepted by apj
Last Modified: 2018-06-07 12:34
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EUV Waves Driven by Sudden Expansion of Transequatorial Loops Caused by Solar Coronal Jets  

Yuandeng Shen   Submitted: 2018-06-07 06:23

We present two events to study the driving mechanism of extreme-ultraviolet (EUV) waves that are not associated with coronal mass ejections (CMEs), by using high resolution observations taken by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory. Observational results indicate that the observed EUV waves were accompanied by ares and coronal jets, but without CMEs that were regarded as the driver of most EUV waves in previous studies. In the first case, it is observed that a coronal jet ejected along a transequatorial loop system at a plane-of-the-sky (POS) speed of 335 ± 22 km s-1, in the meantime, an arc-shaped EUV wave appeared on the eastern side of the loop system. In addition, the EUV wave further interacted with another interconnecting loop system and launched a fast propagating (QFP) magnetosonic wave along the loop system, which had a period of 200 s and a speed of 388 ± 65 km s-1, respectively. In the second case, we also observed a coronal jet ejected at a POS speed of 282 ± 44 km s-1 along a transequatorial loop system and the generation of bright EUV wave on the eastern side of the loop system. Based on the observational results, we propose that the observed EUV waves on the eastern side of the transequatorial loop systems are fast-mode magnetosonic waves, and they were driven by the sudden lateral expansion of the transequatorial loop systems due to the direct impingement of the associated coronal jets, while the QFP wave in the first case formed due to the dispersive evolution of the disturbance caused by the interaction between the EUV wave and the interconnecting coronal loops. It is noted that EUV waves driven by sudden loop expansions have shorter lifetimes than those driven by CMEs.

Authors: Yuandeng Shen; Zehao Tang; Yuhu Miao; Jiangtao Su; Yu Liu
Projects: SDO-AIA

Publication Status: accepted by apj
Last Modified: 2018-06-07 12:35
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Dispersively formed quasi-periodic fast magnetosonic wavefronts due to the eruption of a nearby mini-filament  

Yuandeng Shen   Submitted: 2018-06-07 06:20

Observational analysis is performed to study the excitation mechanism and propagation properties of a quasi-periodic fast-propagating (QFP) magnetosonic wave. The QFP wave was associated with the eruption of a nearby mini-filament and a small B4 Geostationary Operational Environmental Satellite (GOES) flare, which may indicate that the generation of a QFP wave does not require much flare energy. The propagation of the QFP wave was along a bundle of funnel-shaped open loops with a speed of about 1100 ? 78 km s-1 and an acceleration of -2.2 ? 1.1 km s-2. Periodicity analysis indicates that the periods of the QFP wave are 43-6 and 79 ? 18 s. For the first time, we find that the periods of the QFP wave and the accompanying flare are inconsistent, which is different from the findings reported in previous studies. We propose that the present QFP wave was possibly caused by the mechanism of dispersive evolution of the initially broad-band disturbance resulting from the nearby mini-filament eruption.

Authors: Yuandeng Shen; Tengfei Song; Yu Liu
Projects: SDO-AIA

Publication Status: Published in MNRAS Letters
Last Modified: 2018-06-07 12:35
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A quasi-periodic fast-propagating magnetosonic wave associated with the eruption of a magnetic flux rope  

Yuandeng Shen   Submitted: 2017-12-27 18:19

Using high temporal and high spatial resolution observations taken by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we present the detailed observational analysis of a high quality quasi-periodic fast- propagating (QFP) magnetosonic wave that was associated with the eruption of a magnetic flux rope and a GOES C5.0 flare. For the first time, we find that the QFP wave lasted during the entire flare lifetime rather than only the rising phase of the accompanying flare as reported in previous studies. In addition, the propagation of the different parts of the wave train showed different kinematics and morphologies. For the southern (northern) part, the speed, duration, intensity variation are about 875 ± 29 (1485 ± 233) km s-1, 45 (60) minutes, and 4% (2%), and the pronounced periods of them are 106 ± 12 and 160 ± 18 (75 ± 10 and 120 ± 16) seconds, respectively. It is interesting that the northern part of the wave train showed obvious refraction effect when they pass through a region of strong magnetic field. Periodicity analysis result indicates that all the periods of the QFP wave can be found in the period spectrum of the accompanying flare, suggesting their common physical origin. We propose that the quasi-periodic nonlinear magnetohydrodynamics process in the magnetic reconnection that produces the accompanying flare should be important for exciting of QFP wave, and the different magnetic distribution along different paths can account for the different speeds and morphology evolution of the wave fronts.

Authors: Yuandeng Shen; Yu Liu; Tengfei Song; Zhanjun Tian
Projects: SDO-AIA

Publication Status: accept for publication in ApJ
Last Modified: 2018-01-03 11:40
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On a small-scale EUV wave: the driving mechanism and the associated oscillating filament  

Yuandeng Shen   Submitted: 2017-11-15 18:21

We present observations of a small-scale Extreme-ultraviolet (EUV) wave that was associated with a mini-filament eruption and a GOES B1.9 micro-fare in the quiet Sun region. The initiation of the event was due to the photospheric magnetic emergence and cancellation in the eruption source region, which first caused the ejection of a small plasma ejecta, then the ejecta impacted on a nearby mini-filament and thereby led to the filament's eruption and the associated fare. During the filament eruption, an EUV wave at a speed of 182 - 317 km s-1 was formed ahead of an expanding coronal loop, which propagated faster than the expanding loop and showed obvious deceleration and refection during the propagation. In addition, the EUV wave further resulted in the transverse oscillation of a remote filament whose period and damping time are 15 and 60 minutes, respectively. Based on the observational results, we propose that the small-scale EUV wave should be a fast-mode magnetosonic wave that was driven by the the expanding coronal loop. Moreover, with the application of filament seismology, it is estimated that the radial magnetic field strength is about 7 Gauss. The observations also suggest that small-scale EUV waves associated with miniature solar eruptions share similar driving mechanism and observational characteristics with their large-scale counterparts.

Authors: Yuandeng Shen, Yu Liu, Zhanjun Tian, Zhining Qu
Projects: SDO-AIA

Publication Status: Accepted by ApJ
Last Modified: 2017-11-17 14:24
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On a solar blowout jet: driven mechanism and the formation of cool and hot components  

Yuandeng Shen   Submitted: 2017-11-12 02:45

We present the observations of a blowout jet that experienced two distinct ejection stages. The first stage started from the emergence of a small positive magnetic polarity, which cancelled with the nearby negative magnetic field and caused the rising of a mini-filament and its confining loops. This further resulted in a small jet due to the magnetic reconnection between the rising confining loops and the overlying open field. The second ejection stage was mainly due to the successive removal of the confining field by the reconnection. Thus that the filament erupted and the erupting cool filament material directly combined with the hot jet originated form the reconnection region and therefore formed the cool and hot components of the blowout jet. During the two ejection stages, cool Hα jets are also observed cospatial with their coronal counterparts, but their appearance times are earlier than the hot coronal jets a few minutes. Therefore, the hot coronal jets are possibly caused by the heating of the cool Hα jets, or the rising of the reconnection height from chromosphere to the corona. The scenario that magnetic reconnection occurred between the confining loops and the overlying open loops are supported by many observational facts, including the bright patches on the both sides of the mini-filament, hot plasma blobs along the jet body, and periodic metric radio type III bursts at the very beginnings of the two stages. The evolution and characteristics of these features manifest the detailed non-linear process in the magnetic reconnection.

Authors: Shen, Yuandeng; Liu, Ying D.; Su, Jiangtao; Qu, Zhining; Tian, Zhanjun
Projects: SDO-AIA

Publication Status: accepted by ApJ
Last Modified: 2017-11-15 12:19
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Successive Two-sided loop Jets Caused by Magnetic Reconnection between Two adjacent Filamentary Threads  

Yuandeng Shen   Submitted: 2017-07-16 18:18

We present observational analysis of two successive two-sided loop jets observed by the ground-based New Vacuum Solar Telescope (NVST) and the space-borne Solar Dynamics Observatory ( SDO). The two successive two-sided loop jets manifested similar evolution process and both were associated with the interaction of two small-scale adjacent filamentary threads, magnetic emerging and cancellation processes at the jet's source region. High temporal and high spatial resolution observations reveal that the two adjacent ends of the two filamentary threads are rooted in opposite magnetic polarities within the source region. The two threads approached to each other, and then an obvious brightening patch is observed at the interaction position. Subsequently, a pair of hot plasma ejections are observed heading to opposite directions along the paths of the two filamentary threads, and with a typical speed of two-sided loop jets of the order 150 km s-1. Close to the end of the second jet, we report the formation of a bright hot loop structure at the source region, which suggests the formation of new loops during the interaction. Based on the observational results, we propose that the observed two-sided loop jets are caused by the magnetic reconnection between the two adjacent filamentary threads, largely different from the previous scenario that a two-sided loop jet is generated by magnetic reconnection between an emerging bipole and the overlying horizontal magnetic fields.

Authors: Zhanjun Tian, Yu Liu, Yuandeng Shen, Abouazza Elmhamdi, Jiangtao Su, Ying D. Liu, and Ayman. S. Kordi
Projects: SDO-AIA

Publication Status: accepted by APJ
Last Modified: 2017-07-17 10:17
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Simultaneous Transverse Oscillations of a Prominence and a Filament and Longitudinal Oscillation of another Filament Induced by a Single Shock Wave  

Yuandeng Shen   Submitted: 2014-09-05 01:00

We present the first stereoscopic and Doppler observations of simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament launched by a single shock wave. Using Hα Doppler observations, we derive the three-dimensional oscillation velocities at different heights along the prominence axis. The results indicate that the prominence has a larger oscillation amplitude and damping time at higher altitude, but the periods at different heights are the same (i.e., 13.5 minutes). This suggests that the prominence oscillates like a linear vertical rigid body with one end anchored on the Sun. One of the filaments shows weak transverse oscillation after the passing of the shock, which is possibly due to the low altitude of the filament and the weakening (due to reflection) of the shock wave before the interaction. Large amplitude longitudinal oscillation is observed in the other filament after the passing of the shock wave. The velocity amplitude and period are about 26.8 km s-1 and 80.3 minutes, respectively. We propose that the orientation of a filament or prominence relative to the normal vector of the incoming shock should be an important factor for launching transverse or longitudinal filament oscillations. In addition, the restoring forces of the transverse prominence are most likely due to the coupling of gravity and magnetic tension of the supporting magnetic field, while that for the longitudinal filament oscillation is probably the resultant force of gravity and magnetic pressure.

Authors: Yuandeng Shen, Ying D. Liu, P. F. Chen, and Kiyoshi Ichimoto
Projects: SDO-AIA

Publication Status: accepted by ApJ
Last Modified: 2014-09-05 10:14
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A Chain of Winking (Oscillating) Filaments Triggered by an Invisible Extreme-Ultraviolet Wave  

Yuandeng Shen   Submitted: 2014-04-04 01:57

Winking (oscillating) filaments have been observed for many years. However, observations of successive winking filaments in one event have not been reported yet. In this paper, we present the observations of a chain of winking filaments and a subsequent jet that are observed right after the X2.1 are in AR11283. The event also produced an Extreme-ultraviolet (EUV) wave that has two components: upward dome-like wave (850 km s-1) and lateral surface wave (554 km s-1) which was very weak (or invisible) in imaging observations. By analyzing the temporal and spatial relationships between the oscillating filaments and the EUV waves, we propose that all the winking filaments and the jet were triggered by the weak (or invisible) lateral surface EUV wave. The oscillation of the filaments last for two or three cycles, and their periods, Doppler velocity amplitudes, and damping times are 11 - 22 minutes, 6 - 14 km s-1, and 25 - 60 minutes, respectively. We further estimate the radial component magnetic field and the maximum kinetic energy of the filaments, and they are 5 - 10 Gauss and ~ 1019 J, respectively. The estimated maximum kinetic energy is comparable to the minimum energy of ordinary EUV waves, suggesting that EUV waves can efficiently launch filament oscillations on their path. Based on our analysis results, we conclude that the EUV wave is a good agent for triggering and connecting successive but separated solar activities in the solar atmosphere, and it is also important for producing solar sympathetic eruptions.

Authors: Yuandeng Shen, Kiyoshi Ichimoto, Takako T. Ishii, Zhanjun Tian, Ruijuan Zhao, Kazunari Shibata
Projects: Other

Publication Status: accepted by APJ
Last Modified: 2014-04-07 10:55
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Kinematics and Fine Structure of an Unwinding Polar Jet Observed by the SDO/AIA  

Yuandeng Shen   Submitted: 2013-07-31 19:23

We present an observational study of the kinematics and fine structure of an unwinding polar jet, with high temporal and spatial observations taken by the Atmospheric Imaging Assembly on board the Solar Dynamic Observatory and the Solar Magnetic Activity Research Telescope. During the rising period, the shape of the jet resembled a cylinder with helical structures on the surface, while the mass of the jet was mainly distributed on the cylinder's shell. In the radial direction, the jet expanded successively at its western side and underwent three distinct phases: the gradually expanding phase, the fast expanding phase, and the steady phase. Each phase lasted for about 12 minutes. The angular speed of the unwinding motion of the jet and the twist transferred into the outer corona during the eruption are estimated to be 11.1 ? 10-3 rad s-1 (period = 564 s) and 1.17-2.55 turns (or 2.34-5.1π), respectively. On the other hand, by calculating the azimuthal component of the magnetic field in the jet and comparing the free energy stored in the non-potential magnetic field with the jet's total energy, we find that the non-potential magnetic field in the jet is enough to supply the energy for the ejection. These new observational results strongly support the scenario that the jets are driven by the magnetic twist, which is stored in the twisted closed field of a small bipole, and released through magnetic reconnection between the bipole and its ambient open field.

Authors: Shen, Yuandeng; Liu, Yu; Su, Jiangtao; Ibrahim, Ahmed
Projects: SDO-AIA

Publication Status: published by APJ Letters
Last Modified: 2013-08-01 11:16
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A time series of filament eruptions observed by three eyes from space: from failed to successful eruptions  

Yuandeng Shen   Submitted: 2013-07-31 19:20

We present stereoscopic observations of six sequential eruptions of a filament in the active region NOAA 11045 on 2010 Feb 8, with the advantage of the STEREO twin viewpoints in combination with Earth's viewpoint from SOHO instruments and ground-based telescopes. The last one of the six eruptions is a coronal mass ejection, but the others are not. The flare in this successful one is more intense than in the others. Moreover, the velocity of filament material in the successful one is also the largest among them. Interestingly, all the filament velocities are found to be proportional to the power of their flares. We calculate magnetic field intensity at low altitude, the decay indexes of the external field above the filament, and the asymmetry properties of the overlying fields before and after the failed eruptions and find little difference between them, indicating the same coronal confinement exists for both the failed and successful eruptions. The results suggest that, besides the confinement of the coronal magnetic field, the energy released in the low corona should be another crucial element affecting a failed or successful filament eruption. That is, a coronal mass ejection can only be launched if the energy released exceeds some critical value, given the same initial coronal conditions.

Authors: Yuandeng Shen, Yu Liu, and Rui Liu
Projects: STEREO

Publication Status: published by RAA
Last Modified: 2013-08-01 11:16
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Observations of a Quasi-Periodic Fast Propagating Magnetosonic Wave in Multi-Wavelength and Its Interaction with Other Magnetic Structures  

Yuandeng Shen   Submitted: 2013-07-31 19:11

We present an observational study of a quasi-periodic fast propagating (QFP) magnetosonic wave on 2012, April 23. The multiple wave trains were observed along an active region open loop system which has a divergence geometry. The wave trains were first observed in 171 Å observations at a distance of 150 Mm from the footpoint of the guiding loop system and with a speed of 689 km s-1, then they appeared in 193 Å observations after their interaction with a perpendicular underlaying loop system on the path, in the meantime, the wave speed decelerated to 343 km s-1 quickly within a short timescale. The sudden deceleration of the wave trains and their appearance in 193 Å observations caused by the interaction are interpreted through geometric effect and the density increase of the guiding loop system, respectively. On the other hand, with Wavelet and Fourier analysis methods we find that the wave trains has a common period of 80 s with the associated flare. In addition, a few low frequencies are also identified in the QFP wave. We propose that the generation of the period of 80 s was caused by the periodic releasing of energy busts through some nonlinear processes in magnetic reconnection or the so-called oscillatory reconnection mechanism, while the low frequencies detected in the QFP wave were possibly the manifestations of the leakage of pressure-driven oscillations from the photosphere or chromosphere, which could be an important source for driving QFP waves in the low corona. Our observational results also indicate that the properties of the guiding magnetic structure such as the distributions of magnetic field and density as well as geometry are crucial for modulating the propagation behaviors of QFP waves. Therefore, QFP waves could be used for remote diagnostics of the local physical properties of the solar corona.

Authors: Shen, Yuandeng; Liu, Yu.; Su, Jiangtao.; Li, Hui.; Zhang, Xuefei; Tian, Zhanjun; Zhao, Ruijuan; Elmhamdi, Abouazza
Projects: SDO-AIA

Publication Status: Accepted by Solar Physics
Last Modified: 2013-08-01 11:16
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Diffraction, Refraction, and Reflection of An Extreme-Ultraviolet Wave Observed during Its Interactions with Remote Active Regions  

Yuandeng Shen   Submitted: 2013-07-31 19:06

We present observations of the diffraction, refraction, and reflection of a global extreme-ultraviolet (EUV) wave propagating in the solar corona. These intriguing phenomena are observed when the wave interacts with two remote active regions, and they together exhibit the wave property of this EUV wave. When the wave approached AR11465, it became weaker and finally disappeared in the active region, but a few minutes latter a new wavefront appeared behind the active region, and it was not concentric with the incoming wave. In addition, a reflected wave was also observed simultaneously on the wave incoming side. When the wave approached AR11459, it transmitted through the active region directly and without reflection. The formation of the new wavefront and the transmission could be explained with diffraction and refraction effects, respectively. We propose that the different behaviors observed during the interactions may caused by different speed gradients at the boundaries of the two active regions. For the origin of the EUV wave, we find that it formed ahead of a group of expanding loops a few minutes after the start of the loops' expansion, which represents the initiation of the associated coronal mass ejection (CME). Based on these results, we conclude that the EUV wave should be a nonlinear magnetosonic wave or shock driven by the associated CME, which propagated faster than the ambient fast-mode speed and gradually slowed down to an ordinary linear wave. Our observations support the hybrid model that includes both fast wave and slow non-wave components.

Authors: Shen, Yuandeng; Liu, Yu; Su, Jiangtao; Li, Hui; Zhao, Ruijuan; Tian, Zhanjun; Ichimoto, Kiyoshi; Shibata, Kazunari
Projects: SDO-AIA

Publication Status: accepted by APJ letters
Last Modified: 2013-08-01 11:16
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Evidence for the Wave Nature of an Extreme Ultraviolet Wave Observed by the Atmospheric Imaging Assembly Onboard the Solar Dynamics Observatory  

Yuandeng Shen   Submitted: 2012-05-17 05:22

Extreme Ultraviolet (EUV) waves have been found for about 15 years. However, significant controversy remains over their physical natures and origins. In this paper, we report an EUV wave that was accompanied by an X1.9 flare and a partial halo coronal mass ejection. Using high temporal and spatial resolution observations taken by the {em Solar Dynamics Observatory} and the Solar-TErrestrial RElations Observatory, we are able to investigate the detailed kinematics of the EUV wave. We find several arguments that support the fast-mode wave scenario: (1) The speed of the EUV wave (570 km s-1) is higher than the sound speed of quiet-Sun corona. (2) Significant deceleration of the EUV wave (-130 m/s2) is found during its propagation. (3) The EUV wave resulted in the oscillations of a loop and a filament along its propagation path, and a reflected wave from the polar coronal hole is also detected. (4) Refraction or reflection effect is observed when the EUV wave was passing through two coronal bright points. (5) The dimming region behind the wavefront stopped to expand when the wavefront started to become diffuse. (6) The profiles of the wavefront exhibited a dispersive nature, and the magnetosonic Mach number of the EUV wave derived from the highest intensity jump is about 1.4. In addition, triangulation indicates that the EUV wave propagated within a height range of about 60-100 Mm above the photosphere. We propose that the EUV wave observed should be a nonlinear fast-mode magnetosonic wave that propagated freely in the corona after it was driven by the CME expanding flanks during the initial period.

Authors: Yuandeng Shen, Yu Liu
Projects: SDO-AIA

Publication Status: Accepted for publication in ApJ
Last Modified: 2012-05-17 12:39
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Simultaneous Observations of a Large-Scale Wave Event in the Solar Atmosphere: From Photosphere to Corona  

Yuandeng Shen   Submitted: 2012-05-17 05:20

For the first time, we report a large-scale wave that was observed simultaneously in the photosphere, chromosphere, transition region and low corona layers of the solar atmosphere. Using the high temporal and high spatial resolution observations taken by the Solar Magnetic Activity Research Telescope at Hida Observatory and the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamic Observatory, we find that the wave evolved synchronously at different heights of the solar atmosphere, and it propagated at a speed of 605 km s-1 and showed a significant deceleration (-424 m/s2) in the extreme-ultraviolet (EUV) observations. During the initial stage, the wave speed in the EUV observations was 1000 km s-1, similar to those measured from the AIA 1700 Å (967 km s-1) and 1600 Å (893 km s-1) observations. The wave was reflected by a remote region with open fields, and a slower wave-like feature at a speed of 220 km s-1 was also identified following the primary fast wave. In addition, a type-II radio burst was observed to be associated with the wave. We conclude that this wave should be a fast magnetosonic shock wave, which was firstly driven by the associated coronal mass ejection and then propagated freely in the corona. As the shock wave propagated, its legs swept the solar surface and thereby resulted in the wave signatures observed in the lower layers of the solar atmosphere. The slower wave-like structure following the primary wave was probably caused by the reconfiguration of the low coronal magnetic fields, as predicted in the field-line stretching model.

Authors: Yuandeng Shen, Yu Liu
Projects: SDO-AIA

Publication Status: Accepted for publication in ApJL
Last Modified: 2012-05-17 12:39
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On a Coronal Blowout Jet: The First Observation of a Simultaneously Produced Bubble-like CME and a Jet-like CME in a Solar Event  

Yuandeng Shen   Submitted: 2012-05-01 20:06

The coronal blowout jet is a peculiar category among various jet phenomena, in which the sheared base arch, often carrying a small filament, experiences a miniature version of blowout eruption that produces large-scale coronal mass ejection (CME). In this paper, we report such a coronal blowout jet with high-resolution multi-wavelength and multi-angle observations taken from Solar Dynamics Observatory, Solar Terrestrial Relations Observatory, and Big Bear Solar Observatory. For the first time, we find that simultaneous bubble-like and jet-like CMEs were dynamically related to the blowout jet that showed cool and hot components next to each other. Our observational results indicate that (1) the cool component resulted from the eruption of the filament contained within the jet's base arch, and it further caused the bubble-like CME; (2) the jet-like CME was associated with the hot component, which was the outward moving heated plasma generated by the reconnection of the base arch and its ambient open field lines. On the other hand, bifurcation of the jet's cool component was also observed, which resulted from the uncoupling of the erupting filament's two legs that were highly twisted at the very beginning. Based on these results, we propose a model to interpret the coronal blowout jet, in which the external reconnection not only produces the jet-like CME, but also leads to the rising of the filament. Subsequently, internal reconnection starts underneath the rising filament and thereby causes the bubble-like CME.

Authors: Yuandeng Shen, Yu Liu, Jiangtao Su, and Yuanyong Deng
Projects: SDO-AIA

Publication Status: It has been published by ApJ (2012, ApJ, 745, 164).
Last Modified: 2012-05-02 11:15
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Sympathetic Partial and Full Filament Eruptions Observed in One Solar Breakout Event  

Yuandeng Shen   Submitted: 2012-05-01 20:03

We report two sympathetic solar eruptions including a partial and a full flux rope eruption in a quadrupolar magnetic region where a large and a small filament resided above the middle and the east neutral lines, respectively. The large filament first rose slowly at a speed of 8 km s-1 for 23 minutes; it then accelerated to 102 km s-1. Finally, this filament erupted successfully and caused a coronal mass ejection. During the slow rising phase, various evidence for breakout-like external reconnection has been identified at high and low temperature lines. The eruption of the small filament started around the end of the large filament's slow rising. This filament erupted partially, and no associated coronal mass ejection could be detected. Based on a potential field extrapolation, we find that the topology of the three-dimensional coronal field above the source region is composed of three low-lying lobes and a large overlying flux system, and a null point located between the middle lobe and the overlying antiparallel flux system. We propose a possible mechanism within the framework of the magnetic breakout model to interpret the sympathetic filament eruptions, in which the magnetic implosion mechanism is thought to be a possible link between the sympathetic eruptions, and the external reconnection at the null point transfers field lines from the middle lobe to the lateral lobes and thereby leads to the full (partial) eruption of the observed large (small) filament. Other possible mechanisms are also discussed briefly. We conclude that the structural properties of coronal fields are important for producing sympathetic eruptions.

Authors: Yuandeng Shen, Yu Liu, Jiangtao Su
Projects: SDO-AIA

Publication Status: it has been published by ApJ (2012, ApJ, 750, 12)
Last Modified: 2012-05-02 11:16
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Observational Study Of the Quasi-Periodic Fast Propagating Magnetosonic Waves and the Associated Flare on 2011 May 30  

Yuandeng Shen   Submitted: 2012-05-01 19:31

On 2011 May 30, quasi-periodic fast propagating (QFP) magnetosonic waves accompanied by a C2.8 flare were directly imaged by the Atomospheric Imaging Assembly instrument on board the Solar Dynamics Observatory. The QFP waves successively emanated from the flare kernel, they propagated along a cluster of open coronal loops with a phase speed of 834 km s-1 during the flare's rising phase, and the multiple arc-shaped wave trains can be fitted with a series of concentric circles. We generate the k-omega diagram of the Fourier power and find a straight ridge that represents the dispersion relation of the waves. Along the ridge, we find a lot of prominent nodes which represent the available frequencies of the QFP waves. On the other hand, the frequencies of the flare are also obtained by analyzing the flare light curves using the wavelet technique. The results indicate that almost all the main frequencies of the flare are consistent with those of the QFP waves. This suggests that the flare and the QFP waves were possibly excited by a common physical origin. On the other hand, a few low frequencies revealed by the k-omega diagram can not be found in the accompanying flare. We propose that these low frequencies were possibly due to the leakage of the pressure-driven p-mode oscillations from the photosphere into the low corona, which should be a noticeable mechanism for driving the QFP waves observed in the corona.

Authors: Yuandeng Shen, Yu Liu
Projects: SDO-AIA

Publication Status: accepted by ApJ
Last Modified: 2012-05-02 11:16
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Abstracts by Author
Homologous large-amplitude Nonlinear fast-mode Magnetosonic Waves Driven by Recurrent Coronal Jets
EUV Waves Driven by Sudden Expansion of Transequatorial Loops Caused by Solar Coronal Jets
Dispersively formed quasi-periodic fast magnetosonic wavefronts due to the eruption of a nearby mini-filament
A quasi-periodic fast-propagating magnetosonic wave associated with the eruption of a magnetic flux rope
On a small-scale EUV wave: the driving mechanism and the associated oscillating filament
On a solar blowout jet: driven mechanism and the formation of cool and hot components
Successive Two-sided loop Jets Caused by Magnetic Reconnection between Two adjacent Filamentary Threads
Simultaneous Transverse Oscillations of a Prominence and a Filament and Longitudinal Oscillation of another Filament Induced by a Single Shock Wave
A Chain of Winking (Oscillating) Filaments Triggered by an Invisible Extreme-Ultraviolet Wave
Kinematics and Fine Structure of an Unwinding Polar Jet Observed by the SDO/AIA
A time series of filament eruptions observed by three eyes from space: from failed to successful eruptions
Observations of a Quasi-Periodic Fast Propagating Magnetosonic Wave in Multi-Wavelength and Its Interaction with Other Magnetic Structures
Diffraction, Refraction, and Reflection of An Extreme-Ultraviolet Wave Observed during Its Interactions with Remote Active Regions
Evidence for the Wave Nature of an Extreme Ultraviolet Wave Observed by the Atmospheric Imaging Assembly Onboard the Solar Dynamics Observatory
Simultaneous Observations of a Large-Scale Wave Event in the Solar Atmosphere: From Photosphere to Corona
On a Coronal Blowout Jet: The First Observation of a Simultaneously Produced Bubble-like CME and a Jet-like CME in a Solar Event
Sympathetic Partial and Full Filament Eruptions Observed in One Solar Breakout Event
Observational Study Of the Quasi-Periodic Fast Propagating Magnetosonic Waves and the Associated Flare on 2011 May 30

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2003 Solar Physics Group - Montana State University