Multiple Plasma Ejections and Intermittent Nature of Magnetic Reconnection in Solar Chromospheric Anemone Jets

Singh, Kumar Vikram; Isobe, Hiroaki; Nishizuka, Naoto; Nishida, Keisuke; Shibata, Kazunari

doi:10.1088/0004-637x/759/1/33

Cited by 62 publications

(81 citation statements)

References 60 publications

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“…On the other hand, both the sizes of blobs and CBP at the bottom on 2010 August 3 are about two times smaller than those for the event on 2011 July 22. In chromospheric anemone jets, the sizes of blobs (0.3−1.5 Mm) as well as the base loops are even smaller (Singh et al, 2012), implying that the same process may exist in different scales in the solar atmosphere. The lifetime of the blobs in coronal jets observed by AIA ranges from 12 s to 60 s, which is similar to the typical value of chromospheric blobs (Singh et al, 2012).…”

Section: Discussionmentioning

confidence: 99%

“…In chromospheric anemone jets, the sizes of blobs (0.3−1.5 Mm) as well as the base loops are even smaller (Singh et al, 2012), implying that the same process may exist in different scales in the solar atmosphere. The lifetime of the blobs in coronal jets observed by AIA ranges from 12 s to 60 s, which is similar to the typical value of chromospheric blobs (Singh et al, 2012). The apparent Zhang & Ji (2014b) speeds of the blobs in the order of coronal Alfvén speed, i.e., hundreds of km s −1 , are consistent in the FOVs of AIA and EUVI.…”

Section: Discussionmentioning

confidence: 99%

“…Most of the blobs have lifetime of 24−60 s before merging with the background plasma and disappearing. Such intermittent magnetic plasmoids or blobs created by magnetic reconnection have also been observed in the large-scale current sheet (CS) driven by CMEs and the smallscale CS associated with chromospheric jets (Asai et al, 2004;Lin et al, 2005;Takasao et al, 2012;Singh et al, 2012;Kumar & Cho, 2013;Lin et al, 2015). They are generally explained by the tearing-mode instability (TMI) of the thin CS where a series of magnetic islands are recurrently created during magnetic reconnection (Furth et al, 1963;Drake et al, 2006;Bárta et al, 2008;Innes et al, 2015), which makes electron acceleration more efficient and dynamic (Kliem et al, 2000).…”

Section: Introductionmentioning

confidence: 96%

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Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Zhang

2016

Sol Phys

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Coronal bright points (CBPs) and jets are ubiquitous small-scale brightenings that are often associated with each other. In this paper, we report our multiwavelength observations of two groups of homologous jets. The first group was observed by the Extreme-Ultraviolet Imager (EUVI) aboard the behind Solar TErrestrial RElations Observatory (STEREO) spacecraft in 171Å and 304Å on 2014 September 10, from a location where data from the Solar Dynamic Observatory (SDO) could not observe. The jets (J1−J6) recurred for six times with intervals of 5−15 minutes. They originated from the same primary CBP (BP1) and propagated in the northeast direction along large-scale, closed coronal loops. Two of the jets (J3 and J6) produced sympathetic CBPs (BP2 and BP3) after reaching the remote footpoints of the loops. The time delays between the peak times of BP1 and BP2 (BP3) are 240±75 s (300±75 s). The jets were not coherent. Instead, they were composed of bright and compact blobs. The sizes and apparent velocities of the blobs are 4.5−9 Mm and 140−380 km s −1 , respectively. The arrival times of the multiple blobs in the jets at the far-end of the loops indicate that the sympathetic CBPs are caused by jet flows rather than thermal conduction fronts. The second group was observed by the Atmospheric Imaging Assembly aboard SDO in various wavelengths on 2010 August 3. Similar to the first group, the jets originated from a short-lived bright point (BP) at the boundary of active region 11092 and propagated along a small-scale, closed loop before flowing into the active region. Several tiny blobs with sizes of ∼1.7 Mm and apparent velocity of ∼238 km s −1 were identified in the jets. We carried out the differential emission measure (DEM) inversions to investigate the temperatures of the blobs, finding that the blobs were multithermal with average temperature of 1.8−3.1 MK. The estimated number densities of the blobs were (1.7−2.8)×10 9 cm −3 .

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

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Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Zhang

2016

Sol Phys

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“…White-light blobs are observed to be quasi-periodically ejected out of the large-scale coronal streamers (Song et al 2009). Recurrent plasmoids in the chromospheric anemone jets with a size of ∼0.1 Mm are observed by Singh et al (2012) and reproduced in the numerical simulations of Yang et al (2013). In this paper, we investigated the thermodynamic evolutions of the recurrent and homologous jets observed by the Atmospheric Imaging Assembly (AIA; Lemen et al 2012) aboard the Solar Dynamics Observatory (SDO) on 2011 July 22 and report our discovery of blobs in the jets.…”

Section: Introductionmentioning

confidence: 97%

Blobs in recurring extreme-ultraviolet jets

Zhang

2014

A&A

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Context. Coronal jets are one type of ubiquitous small-scale activity that is caused by magnetic reconnection in the solar corona. They are often associated with cool surges in the chromosphere. Aims. In this paper, we report our discovery of blobs in the recurrent and homologous jets that occurred at the western edge of the NOAA active region 11259 on 2011 July 22. Methods. The jets were observed in the seven extreme-ultraviolet (EUV) filters of the Atmospheric Imaging Assembly instrument aboard the Solar Dynamics Observatory. Using the base-difference images of the six filters (94, 131, 171, 211, 193, and 335 Å), we carried out the differential emission measure (DEM) analyses to explore the thermodynamic evolutions of the jets. The jets were accompanied by cool surges observed in the Hα line center of the ground-based telescope in the Big Bear Solar Observatory. Results. The jets that had lifetimes of 20−30 min recurred at the same place for three times with an interval of 40−45 min. Interestingly, each of the jets intermittently experienced several upward eruptions at the speed of 120−450 km s −1 . After reaching the maximum heights, they returned back to the solar surface, showing near-parabolic trajectories. The falling phases were more evident in the low-T filters than in the high-T filters, indicating that the jets experienced cooling after the onset of eruptions. We identified bright and compact blobs in the jets during their rising phases. The simultaneous presence of blobs in all the EUV filters were consistent with the broad ranges of the DEM profiles of the blobs (5.5 ≤ log T ≤ 7.5), indicating their multi-thermal nature. The median temperatures of the blobs were ∼2.3 MK. The blobs that were ∼3 Mm in diameter had lifetimes of 24−60 s. Conclusions. To our knowledge, this is the first report of blobs in coronal jets. We propose that these blobs are plasmoids created by the magnetic reconnection as a result of tearing-mode instability and are ejected out along the jets.

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“…Based on the studies of Shibata et al (2007) and Nishizuka et al (2011), the chromospheric anemone jets have a lifetime of 100-500 s, a length of 1.0-5.0 Mm, a width of 100-400 km, and a velocity of 5-20 km s −1 . Multiple bright plasma ejections are often found in these jets, with a lifetime of around 20-60 s and a size of 0.3-1.5 Mm, showing the intermittent nature of magnetic reconnection (Singh et al 2012). The behavior of these jets is independent of their positions on the solar disk (Nishizuka et al 2011), and the jet flowing plasma after being ejected from the root undergoes some other acceleration rather than follows a ballistic motion (see Shibata et al 2007;Nishizuka et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Observational Evidence for the Causes and Consequences of Chromospheric Reconnection

Yan

Xia

et al. 2015

ApJ

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The chromospheric anemone jets with an inverse "Y" shape are ubiquitous, as revealed by the Solar Optical Telescope observations. These jets are considered to be consequences of chromospheric magnetic reconnections. Although these jets have been studied intensively, the dynamics and their driving causes remain unclear observationally. In this work, we report a case of a chromospheric jet showing complete observational evidencefor the cause and consequence of chromospheric intermittent reconnection. The intermittent eruption of this jet shows two distinct quasi-periods, 50-60 s and 600-700 s. The short-period eruptions may be related to the plasmoidinduced reconnection, and the long-period ones may be interpreted as sequences of cycles of energy storage and release during magnetic reconnections. The observations also reveal Alfvénic waves with a mean period around 88 s and a maximum transverse displacement around 0″ .26. The jet is hosted by a loop moving smoothly with a horizontal speed of ∼0.4 km s −1 . Our results provide observational evidence supporting the magnetic reconnection model of the formation of the chromospheric jets with related products, in which the loop advection drives intermittent magnetic reconnections, and the reconnection outflows carrying plasmoids collide further with the ambient field linesand finally excitewaves and jets.

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Multiple Plasma Ejections and Intermittent Nature of Magnetic Reconnection in Solar Chromospheric Anemone Jets

Cited by 62 publications

References 60 publications

Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Blobs in recurring extreme-ultraviolet jets

Observational Evidence for the Causes and Consequences of Chromospheric Reconnection

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