Multiwavelength Imaging and Spectral Analysis of Jet-like Phenomena in a Solar Active Region Using IRIS and AIA

Humphries, Llŷr Dafydd; Verwichte, E.; Kuridze, David; Morgan, Huw

doi:10.3847/1538-4357/ab974d

Cited by 3 publications

(3 citation statements)

References 55 publications

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“…Evidence of such emission was independently found in the IRIS Si IV lines by Nóbrega-Siverio et al (2017) and Guglielmino, Young, and Zuccarello (2019). Other examples of chromospheric ejections with associated TR emission observed with IRIS are fan-shaped jets originating from light bridges (Yang et al, 2015;Bharti, 2015;Bai et al, 2019) and penumbral microjets Humphries et al, 2020), although penumbral microjets are not genuine jets with significant mass motions, but rather manifestations of heat fronts (Esteban Buehler et al, 2019; Rouppe van der Voort and Drews, 2019; Drews and Rouppe van der Voort, 2020). In order to properly understand the TR emission of the aforementioned phenomena, one has to take the highly dynamic nature of the chromosphere into account as well as the fact that some elements in the TR have long ionization and recombination timescales, leading to relevant non-equilibrium ionization effects (e.g.…”

Section: Solar Jets and Surgesmentioning

confidence: 99%

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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Section: Solar Jets and Surgesmentioning

confidence: 99%

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

et al. 2021

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“…From chromospheric and transition region observations, several types of small-scale dynamic phenomena have been reported on LBs. One prominent phenomenon is the surge-like activity repeatedly occurring above LBs, called Hα surges, light wall oscillations, plasma ejections or chromospheric jets by various authors (Asai et al 2001;Shimizu et al 2009;Yang et al 2015;Toriumi et al 2015a;Su et al 2016;Robustini et al 2016;Reid et al 2018;Humphries et al 2020;Li et al 2020;Kotani & Shibata 2020;Shen 2021). The surge-like activity appears to have at least two components: persistent up-and-down motions driven by the upward leakage of magnetoacoustic waves, and intermittent high-speed jets triggered by magnetic reconnection (Zhang et al 2017;Hou et al 2017;.…”

Section: Introductionmentioning

confidence: 99%

Statistical investigation on the formation of sunspot light bridges

Chen

Song

et al. 2021

Res. Astron. Astrophys.

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Light bridges (LBs) are bright lanes that divide one sunspot umbra into two or more parts. Though frequently observed in sunspots, their formation mechanisms have rarely been studied and thus are not well understood. Here we present results from the first statistical investigation on the formation of LBs. Using observations with the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we identified 144 LBs within 71 active regions (ARs) over the whole year of 2014. The formation processes of these LBs can be categorized into three groups: penumbral intrusion (type-A), sunspot merging (type-B) and umbral-dot emergence (type-C). The numbers of events in these three categories are 74, 57 and 13, respectively. The duration of the LB formation process is mostly less than 40 hours, with an average of ∼20 hours. Most LBs have a maximum length of less than 20″. For type-A LBs, we found a positive correlation between the LB length and the duration of the LB formation process, suggesting a similar speed of penumbral intrusion in different sunspots.

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“…The double peaks in the Doppler velocity and centroid distribution could be due to the different nature of flows in different parts of the observed active region. In a recent study, Humphries et al (2020) show redshift at the footpoints and blueshift near the top of the coronal protrusions. Studies by De Pontieu et al (2017) suggest that the outflows could be linked to chromospheric jets and spicules, which are heated while propagating into the corona.…”

Section: Discussionmentioning

confidence: 83%

Line Profile Studies of Coronal Active Regions in Fe xii λ195.12 Using Hinode/EIS

Prabhakar

Raju

2022

ApJ

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Coronal active regions are studied using Hinode/EIS observations in the EUV line Fe xii λ195.12 by analyzing their line profiles from 2006 December to 2019 December. The period covers the last 2 yr of solar cycle 23 and solar cycle 24 fully. Active regions are the main source of magnetic field in the solar atmosphere, important in its heating and dynamics. Line profiles were obtained from various active regions spread across the Sun on a monthly basis from which we obtained the intensity, line width, Doppler velocity, and centroid and examined their variation during the solar cycle. The histograms of the Doppler velocity and centroid show that they behave in six different ways with respect to the position of rest wavelength. In addition, the shifts in the centroid were found to be more compared to the Doppler velocity. The variation of the line width with respect to the Doppler velocity or the centroid mostly follows a second-degree polynomial. A multicomponent line profile is simulated to explain the difference in the behavior of the Doppler velocity and the centroid with respect to the line width. We also find that the intensity and the line width of the different data sets show a global dependence on the solar cycle with a good correlation. The implications of the results for the coronal heating and dynamics are pointed out.

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Multiwavelength Imaging and Spectral Analysis of Jet-like Phenomena in a Solar Active Region Using IRIS and AIA

Cited by 3 publications

References 55 publications

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

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

Statistical investigation on the formation of sunspot light bridges

Line Profile Studies of Coronal Active Regions in Fe xii λ195.12 Using Hinode/EIS

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