Simultaneous Observation of a Hot Explosion by NST and Iris

Kim, Yeon Han; Yurchyshyn, Vasyl; Bong, Su-Chan; Cho, Il Hyun; Cho, Kyung-Suk; Lee, Jaejin; Lim, Eun-Kyung; Park, Young Deuk; Yang, Heesu; Ahn, Kwangsu; Goode, Philip R.; Jang, Bi-Ho

doi:10.1088/0004-637x/810/1/38

Cited by 48 publications

(68 citation statements)

References 18 publications

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“…The Hα synthetic profiles are consistent either with Hα THEMIS profiles (CB E) (black profile in Fig. 2) and/or with those obtained with the SST/CRISP and the NST (Vissers et al 2015;Kim et al 2015). The wings of the Hα C profile have enhanced intensities up to 25% in Hα +/−2 Å similar to the EBs of the NST (see the Fig.…”

Section: Discussionsupporting

confidence: 81%

“…The wings of the Hα C profile have enhanced intensities up to 25% in Hα +/−2 Å similar to the EBs of the NST (see the Fig. 5 in Kim et al 2015) and up to 50% at Hα − 1.25 Å as for EB1 (see Fig. 4 in Vissers et al 2015).…”

Section: Discussionsupporting

confidence: 55%

“…EBs are mainly defined by the Hα line profiles. To be sure about the properties of EBs in Mg II h and k lines we need simultaneous observations in Hα, as in the papers of Vissers et al (2015) and Kim et al (2015). Our observation of AR11850 in Hα is from the same day, but not simultaneous.…”

Section: Discussionmentioning

confidence: 99%

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Height formation of bright points observed by IRIS in Mg II line wings during flux emergence

Grubecka

Schmieder

Berlicki

et al. 2016

A&A

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Context. A flux emergence in the active region AR 111850 was observed on September 24, 2013 with the Interface Region Imaging Spectrograph (IRIS). Many bright points are associated with the new emerging flux and show enhancement brightening in the UV spectra. Aims. The aim of this work is to compute the altitude formation of the compact bright points (CBs) observed in Mg II lines in the context of searching Ellerman bombs (EBs). Methods. IRIS provided two large dense rasters of spectra in Mg II h and k lines, Mg II triplet, C II and Si IV lines covering all the active region and slit jaws in the two bandpasses (1400 Å and 2796 Å) starting at 11:44 UT and 15:39 UT, and lasting 20 min each. Synthetic profiles of Mg II and Hα lines are computed with non-local thermodynamic equlibrium (NLTE) radiative transfer treatment in 1D solar atmosphere model including a hotspot region defined by three parameters: temperature, altitude, and width. Results. Within the two IRIS rasters, 74 CBs are detected in the far wings of the Mg II lines (at +/−1 Å and 3.5 Å). Around 10% of CBs have a signature in Si IV and CII. NLTE models with a hotspot located in the low atmosphere were found to fit a sample of Mg II profiles in CBs. The Hα profiles computed with these Mg II CB models are consistent with typical EB profiles observed from ground based telescopes e.g. THEMIS. A 2D NLTE modelling of fibrils (canopy) demonstrates that the Mg II line centres can be significantly affected but not the peaks and the wings of Mg II lines. Conclusions. We conclude that the bright points observed in Mg II lines can be formed in an extended domain of altitudes in the photosphere and/or the chromosphere (400 to 750 km). Our results are consistent with the theory of heating by Joule dissipation in the atmosphere produced by magnetic field reconnection during flux emergence.

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Section: Discussionsupporting

confidence: 81%

Section: Discussionsupporting

confidence: 55%

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Height formation of bright points observed by IRIS in Mg II line wings during flux emergence

Grubecka

Schmieder

Berlicki

et al. 2016

A&A

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“…We speculate that an EB-specific atmospheric model may be needed, which has different atmospheric abundances, enabling the Ca II 8542 Å line core and Mg II h and k line wings to form at different heights. We also find that we were unable to superheat the plasma to >10,000 K, as previous works speculate, in order to explains the Mg II h and k line formation (Peter et al 2014;Kim et al 2015;Vissers et al 2015;Tian et al 2016).…”

Section: Discussionsupporting

confidence: 66%

“…More recently, observations using the IRIS instrument indicate that EB signatures have been found in the Mg II h and k wings, Si IV, and C II lines (Peter et al 2014;Kim et al 2015;Vissers et al 2015;Tian et al 2016). These lines are sensitive to much higher temperatures (50,000-100,000 K)and sample the upper chromosphere and transition region.…”

Section: Introductionmentioning

confidence: 99%

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

Reid

Mathioudakis

Kowalski

et al. 2017

ApJL

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Recent observations from the Interface Region Imaging Spectrograph appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground-based observations in Hα, appear cospatial to Ellerman Bombs (EBs). We use the RADYN one-dimensional radiative transfer code in an attempt to try and reproduce the observed line profiles and simulate the atmospheric conditions of these events. Combined with the MULTI/RH line synthesis codes, we compute the Hα, Ca II 8542 Å, and Mg II h and k lines for these simulated events and compare them to previous observations. Our findings hint that the presence of superheated regions in the photosphere (>10,000 K) is not a plausible explanation for the production of EB signatures. While we are able to recreate EB-like line profiles in Hα, Ca II 8542 Å, and Mg II h and k, we cannot achieve agreement with all of these simultaneously.

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A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

et al. 2021

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The Interface Region Imaging Spectrograph (IRIS) has been obtaining near- and far-ultraviolet images and spectra of the solar atmosphere since July 2013. IRIS is the highest resolution observatory to provide seamless coverage of spectra and images from the photosphere into the low corona. The unique combination of near- and far-ultraviolet spectra and images at sub-arcsecond resolution and high cadence allows the tracing of mass and energy through the critical interface between the surface and the corona or solar wind. IRIS has enabled research into the fundamental physical processes thought to play a role in the low solar atmosphere such as ion–neutral interactions, magnetic reconnection, the generation, propagation, and dissipation of waves, the acceleration of non-thermal particles, and various small-scale instabilities. IRIS has provided insights into a wide range of phenomena including the discovery of non-thermal particles in coronal nano-flares, the formation and impact of spicules and other jets, resonant absorption and dissipation of Alfvénic waves, energy release and jet-like dynamics associated with braiding of magnetic-field lines, the role of turbulence and the tearing-mode instability in reconnection, the contribution of waves, turbulence, and non-thermal particles in the energy deposition during flares and smaller-scale events such as UV bursts, and the role of flux ropes and various other mechanisms in triggering and driving CMEs. IRIS observations have also been used to elucidate the physical mechanisms driving the solar irradiance that impacts Earth’s upper atmosphere, and the connections between solar and stellar physics. Advances in numerical modeling, inversion codes, and machine-learning techniques have played a key role. With the advent of exciting new instrumentation both on the ground, e.g. the Daniel K. Inouye Solar Telescope (DKIST) and the Atacama Large Millimeter/submillimeter Array (ALMA), and space-based, e.g. the Parker Solar Probe and the Solar Orbiter, we aim to review new insights based on IRIS observations or related modeling, and highlight some of the outstanding challenges.

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Simultaneous Observation of a Hot Explosion by NST and Iris

Cited by 48 publications

References 18 publications

Height formation of bright points observed by IRIS in Mg II line wings during flux emergence

Height formation of bright points observed by IRIS in Mg II line wings during flux emergence

Solar Ellerman Bombs in 1D Radiative Hydrodynamics

A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

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