EXPLOSIVE EVENTS ON A SUBARCSECOND SCALE IN<i>IRIS</i>OBSERVATIONS: A CASE STUDY

Huang, Zhaoqin; Madjarska, M. S.; Xia, Lidong; Doyle, J. G.; Galsgaard, K.; Fu, Hui

doi:10.1088/0004-637x/797/2/88

Cited by 57 publications

(69 citation statements)

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“…Obvious enhancement in one or both wings of the Si IV lines, which are usually believed to be associated with reconnection outflows (bidirectional jets or unidirectional jets, Innes et al 1997), can be clearly identified for most bombs. These line profiles are generally similar to those of transition region explosive events (EEs), which are also believed to result from reconnection (e.g., Dere et al 1989;Innes et al 1997;Chae et al 1998;Madjarska et al 2004;Ning et al 2004;Teriaca et al 2004;Zhang et al 2010;Huang et al 2014;Gupta & Tripathi 2015). The most distinct difference between EEs and IBs may be the formation height: EEs are formed in the transition region, and IBs are formed lower down as suggested by the chromospheric absorption lines.…”

Section: Identification Of Ibsmentioning

confidence: 58%

Are Iris Bombs Connected to Ellerman Bombs?

Tian

et al. 2016

ApJ

117

190

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Recent observations by the Interface Region Imaging Spectrograph (IRIS) have revealed pockets of hot gas (∼2-8 × 10 4 K) potentially resulting from magnetic reconnection in the partially ionized lower solar atmosphere (IRIS bombs; IBs). Using joint observations between IRIS and the Chinese New Vacuum Solar Telescope, we have identified 10 IBs. We find that 3 are unambiguously and 3 others are possibly connected to Ellerman bombs (EBs), which show intense brightening of the extended a H wings without leaving an obvious signature in the a H core. These bombs generally reveal the following distinct properties: (1) the O IV 1401.156 Å and 1399.774 Å lines are absent or very weak; (2) the Mn I 2795.640 Å line manifests as an absorption feature superimposed on the greatly enhanced Mg II k line wing; (3) the Mg II k and h lines show intense brightening in the wings and no dramatic enhancement in the cores; (4) chromospheric absorption lines such as Ni II 1393.330 Å and 1335.203 Å are very strong; and (5) the 1700 Å images obtained with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory reveal intense and compact brightenings. These properties support the formation of these bombs in the photosphere, demonstrating that EBs can be heated much more efficiently than previously thought. We also demonstrate that the Mg II k and h lines can be used to investigate EBs similarly to a H , which opens a promising new window for EB studies. The remaining four IBs obviously have no connection to EBs and they do not have the properties mentioned above, suggesting a higher formation layer, possibly in the chromosphere.

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Section: Identification Of Ibsmentioning

confidence: 58%

Are Iris Bombs Connected to Ellerman Bombs?

Tian

et al. 2016

ApJ

117

190

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“…De Pontieu et al (2014b) have demonstrated that twisting motions of small-scale TR loops and jets can result in EEtype line profiles. Huang et al (2014) found an EE associated with plasma ejection followed by retraction in the chromosphere.…”

Section: Introductionmentioning

confidence: 97%

Investigating the Transition Region Explosive Events and Their Relationship to Network Jets

Chen

Tian

Huang

et al. 2019

ApJ

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Recent imaging observations with the Interface Region Imaging Spectrograp (IRIS) have revealed prevalent intermittent jets with apparent speeds of 80-250 km s −1 from the network lanes in the solar transition region (TR). On the other hand, spectroscopic observations of the TR lines have revealed the frequent presence of highly non-Gaussian line profiles with enhanced emission at the line wings, often referred as explosive events (EEs). Using simultaneous imaging and spectroscopic observations from IRIS, we investigate the relationship between EEs and network jets. We first identify EEs from the Si iv 1393.755Å line profiles in our observations, then examine related features in the 1330Å slit-jaw images. Our analysis suggests that EEs with double peaks or enhancements in both wings appear to be located at either the footpoints of network jets, or transient compact brightenings. These EEs are most likely produced by magnetic reconnection. We also find that EEs with enhancements only at the blue wing are mainly located on network jets, away from the footpoints. These EEs clearly result from the superposition of the high-speed network jets on the TR background. In addition, EEs showing enhancement only at the red wing of the line are often located around the jet footpoints, possibly caused by the superposition of reconnection downflows on the background emission. Moreover, we find some network jets that are not associated with any detectable EEs. Our analysis suggests that some EEs are related to the birth or propagation of network jets, and that others are not connected to network jets.

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“…The recently launched Interface Region Imaging Spectrograph (IRIS, De Pontieu et al 2014b), which provided images and spectrum with considerably high temporal and spatial resolution, has opened a new window for investigating the small-scale energy release events in the interface region. Some impressive findings (Hansteen et al 2014;De Pontieu et al 2014a;Tian et al 2014;Peter et al 2014;Rouppe van der Voort et al 2015;Vissers et al 2015) and more specific works (Huang et al 2014;Martínez-Sykora et al 2015;Kim et al 2015;Park et al 2016;Skogsrud et al 2016;Brooks et al 2016) have been introduced. Most of them have focused on the transition region loops, torsional motions, solar spicules, bright grains, explosive events, Ellerman bombs (EBs) and the hot bombs which turn out to be the analogies of EBs (Tian et al 2016).…”

Section: Introductionmentioning

confidence: 99%