Generation of solar spicules and subsequent atmospheric heating

Samanta, Tanmoy; Tian, Hui; Yurchyshyn, Vasyl; Peter, Hardi; Cao, Wenda; Sterling, Alphonse C.; Erdélyi, R.; Ahn, Kwangsu; Feng, Song; Utz, D.; Banerjee, D.; Chen, Yajie

doi:10.1126/science.aaw2796

Cited by 151 publications

(156 citation statements)

References 85 publications

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“…In addition, given the increasing evidence for the presence of unresolved minority polarities in the photosphere (e.g., Solanki et al 2017;Smitha et al 2017), such ejections resulting from flux cancellation can give rise to jet-like features found inside plages and strong network associated with the unresolved underlying minority polarities (Wang 2016;Wang et al 2019). We expect that other small-scale phenomena, such as spicules, could be associated with reconnection at lower atmospheric heights between converging cancelling polarities, and can potentially be associated with the cool outflows predicted from our model for different values of parameter space (e.g., Samanta et al 2019).…”

Section: Discussionmentioning

confidence: 86%

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Syntelis

Priest

2020

ApJ

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Inspired by recent observations suggesting that photospheric magnetic flux cancellation occurs much more frequently than previously thought, we analytically estimated the energy released from reconnection driven by photospheric flux cancellation, and proposed that it can act as a mechanism for chromospheric and coronal heating (Priest et al. 2018). Using two-dimensional simulations we validated the analytical estimates and studied the resulting atmospheric response (Syntelis et al. 2019). In the present work, we set up three-dimensional resistive MHD simulations of two cancelling polarities in a stratified atmosphere with a horizontal external field to further validate and improve upon the analytical estimates. The computational evaluation of the parameters associated with the energy release are in good qualitative agreement with the analytical estimates. The computational Poynting energy flux into the current sheet is in good qualitative agreement with the analytical estimates, after correcting the analytical expression to better account for the horizontal extent of the current sheet. The atmospheric response to the cancellation is the formation of hot ejections, cool ejections, or a combination of both hot and cool ejections, which can appear with a time difference and/or be spatially offset, depending on the properties of the cancelling region and the resulting height of the reconnection. Therefore, during the cancellation, a wide spectrum of ejections can be formed, which can account for the variety of multi-thermal ejections associated with Ellerman bombs, UV bursts and IRIS bombs, and also other ejections associated with small-scale cancelling regions and spicules.

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Section: Discussionmentioning

confidence: 86%

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Syntelis

Priest

2020

ApJ

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“…Because of this, information on the magnetic field of the whole atmosphere is required to study the interplay between the solar plasma and magnetic field. However, routine and reliable measurements of the solar magnetic field have only been achieved at the photospheric level (e.g., [1,2]). We still do not have a precise knowledge of the magnetic field in the upper solar atmo-sphere, especially the corona, which impedes our complete understanding of a wide range of phenomena including the solar cycle, solar eruptions and heating of the coronal plasma.…”

Section: Introductionmentioning

confidence: 99%

Mapping the magnetic field in the solar corona through magnetoseismology

Yang

Tomczyk

Morton

et al. 2020

Sci. China Technol. Sci.

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of magnetic field diagnostics based on observations of magnetohydrodynamic (MHD) waves, has been widely used to estimate the field strengths of oscillating structures in the solar corona. However, previously magnetoseismology was mostly applied to occasionally occurring oscillation events, providing an estimate of only the average field strength or one-dimensional distribution of field strength along an oscillating structure. This restriction could be eliminated if we apply magnetoseismology to the pervasive propagating transverse MHD waves discovered with the Coronal Multi-channel Polarimeter (CoMP). Using several CoMP observations of the Fe xiii 1074.7 nm and 1079.8 nm spectral lines, we obtained maps of the plasma density and wave phase speed in the corona, which allow us to map both the strength and direction of the coronal magnetic field in the plane of sky. We also examined distributions of the electron density and magnetic field strength, and compared their variations with height in the quiet Sun and active regions. Such measurements could provide critical information to advance our understanding of the Sun's magnetism and the magnetic coupling of the whole solar atmosphere.

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“…These jets appear to originate 2-3 Mm above the limb, which roughly places them at the top of H α RBEs. Samanta et al (2019) identified magnetic flux cancellations at the footpoint of some analyzed RBEs. Two events considered in the present study do exhibit morphological features and evolutionary pattern consistent with the flux cancellation scenario.…”

Section: Summary and Discussionmentioning

confidence: 97%

Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk H_α Images

Yurchyshyn

Cao

Abramenko

et al. 2020

ApJL

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We analyze ground-based chromospheric data acquired at a high temporal cadence of 2 s in wings of the H α spectral line using Goode Solar Telescope (GST) operating at the Big Bear Solar Observatory. We inspected a 30 minute long H α -0.08 nm data set to find that rapid blue-shifted H α excursions (RBEs), which are a cool component of type II spicules, experience very rapid morphological changes on the time scales of the order of 1 second. Unlike typical reconnection jets, RBEs very frequently appear in situ without any clear evidence of H α material being injected from below. Their evolution includes inverted "Y", "V", "N", and parallel splitting (doubling) patterns as well as sudden formation of a diffuse region followed by branching. We also find that the same feature may undergo several splitting episodes within about 1 min time interval.

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Generation of solar spicules and subsequent atmospheric heating

Cited by 151 publications

References 85 publications

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Mapping the magnetic field in the solar corona through magnetoseismology

Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk H_α Images

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Generation of solar spicules and subsequent atmospheric heating

Cited by 151 publications

References 85 publications

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Mapping the magnetic field in the solar corona through magnetoseismology

Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk Hα Images

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Product

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Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk H_α Images