Propagating Disturbances in the Solar Corona and Spicular Connection

Samanta, Tanmoy; Pant, Vaibhav; Banerjee, D.

doi:10.1088/2041-8205/815/1/l16

Cited by 36 publications

(32 citation statements)

References 28 publications

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“…In the simulation, we only use the time scale of spicular activities that are found to be highly correlated with quasi-periodic propagating disturbances in polar plumes (Jiao et al 2015;Samanta et al 2015).…”

Section: Propagating Disturbances In Polar Plumesmentioning

confidence: 99%

Stochastic Transients as a Source of Quasi-Periodic Processes in the Solar Atmosphere

Yuan

Jiao

et al. 2016

ApJS

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Solar dynamics and turbulence occur at all heights of the solar atmosphere and could be described as stochastic processes. We propose that finite lifetime transients recurring at a certain place could trigger quasi-periodic processes in the associated structures. In this study, we developed a mathematical model for finite lifetime and randomly occurring transients, and found that quasi-periodic processes, with period longer than the time scale of the transients, are detectable intrinsically in form of trains. We simulate their propagation in an empirical solar atmospheric model with chromosphere, transition region and corona. We found that, due to the filtering effect of the chromospheric cavity, only the resonance period of the acoustic resonator is able to propagate to the upper atmosphere, such a scenario is applicable to slow magnetoacoustic waves in sunspots and active regions. If the thermal structure of the atmosphere is less wild and acoustic resonance does not take effect, the long period oscillations could propagate to the upper atmosphere. Such case would be more likely to occur at polar plumes.

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Section: Propagating Disturbances In Polar Plumesmentioning

confidence: 99%

Stochastic Transients as a Source of Quasi-Periodic Processes in the Solar Atmosphere

Yuan

Jiao

et al. 2016

ApJS

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“…These loops have long been known to be permeated by propagating coronal disturbances (PCDs): rapid (∼100 km s −1 ) intensity disturbances whose exact nature remains unknown. While it is clear that PCDs that originate from sunspot umbrae are caused by sound waves, it is less clear whether waves or flows cause these PCDs in plage regions, with both receiving observational and theoretical support (e.g., de Moortel et al 2002aMoortel et al , 2002bDe Pontieu et al 2005;De Moortel 2009;De Pontieu & McIntosh 2010;Verwichte et al 2010;De Moortel & Nakariakov 2012;Ofman et al 2012;Tian et al 2012;Wang et al 2013;Petralia et al 2014;De Moortel et al 2015;Samanta et al 2015;Bryans et al 2016). We also take advantage of recent developments in spicule modeling (Martínez-Sykora et al 2016, 2017) that appear to show coronal heating associated with spicules.…”

Section: Introductionmentioning

confidence: 99%

Observations and Numerical Models of Solar Coronal Heating Associated with Spicules

Pontieu

Moortel

Martínez-Sykora

et al. 2017

ApJL

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Spicules have been proposed as significant contributors to the mass and energy balance of the corona. While previous observations have provided a glimpse of short-lived transient brightenings in the corona that are associated with spicules, these observations have been contested and are the subject of a vigorous debate both on the modeling and the observational side. Therefore, it remains unclear whether plasma is heated to coronal temperatures in association with spicules. We use high-resolution observations of the chromosphere and transition region (TR) with the Interface Region Imaging Spectrograph and of the corona with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to show evidence of the formation of coronal structures associated with spicular mass ejections and heating of plasma to TR and coronal temperatures. Our observations suggest that a significant fraction of the highly dynamic loop fan environment associated with plage regions may be the result of the formation of such new coronal strands, a process that previously had been interpreted as the propagation of transient propagating coronal disturbances. Our observations are supported by 2.5D radiative MHD simulations that show heating to coronal temperatures in association with spicules. Our results suggest that heating and strong flows play an important role in maintaining the substructure of loop fans, in addition to the waves that permeate this low coronal environment.

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“…Recently, several authors have reported that small scale jets and spicules at transition region and chromosphere are associated with with PDs seen in polar plumes and polar coronal holes Jiao et al 2015;Samanta et al 2015;Bryans et al 2016;Yuan et al 2016). Reflections of propagating slow waves were also reported in hot and flaring coronal loops using AIA (Kumar et al 2013(Kumar et al , 2015 and XRT observations (Mandal et al 2016).…”

Section: Introductionmentioning

confidence: 99%

First Imaging Observation of Standing Slow Wave in Coronal Fan Loops

Pant

Tiwari

Yuan

et al. 2017

ApJL

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We observe intensity oscillations along coronal fan loops associated with the active region AR 11428. The intensity oscillations were triggered by blast waves which were generated due to X-class flares in the distant active region AR 11429. To characterise the nature of oscillations, we created time-distance maps along the fan loops and noted that the intensity oscillations at two ends of the loops were out of phase. As we move along the fan loop, the amplitude of the oscillations first decreased and then increased. The out-of-phase nature together with the amplitude variation along the loop implies that these oscillations are very likely to be standing waves. The period of the oscillations are estimated to be ∼27 min, damping time to be ∼45 min and phase velocity projected in the plane of sky ∼ 65-83 km s −1 . The projected phase speeds were in the range of acoustic speed of coronal plasma at about 0.6 MK which further indicates that these are slow waves. To best of our knowledge, this is the first report on the existence of the standing slow waves in non-flaring fan loops.

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Propagating Disturbances in the Solar Corona and Spicular Connection

Cited by 36 publications

References 28 publications

Stochastic Transients as a Source of Quasi-Periodic Processes in the Solar Atmosphere

Stochastic Transients as a Source of Quasi-Periodic Processes in the Solar Atmosphere

Observations and Numerical Models of Solar Coronal Heating Associated with Spicules

First Imaging Observation of Standing Slow Wave in Coronal Fan Loops

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