Mass Flows in a Prominence Spine as Observed in Euv

Kucera, T. A.; Gilbert, H. R.; Karpen, J. T.

doi:10.1088/0004-637x/790/1/68

Cited by 8 publications

(5 citation statements)

References 39 publications

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“…Our Fig. 5a clearly shows that counterstreamings are present in our simulations due to random heating localised at the footpoints, as also suggested by Kucera et al [35]. While Fig.…”

Section: Discussionsupporting

confidence: 89%

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Simulations of solar filament fine structures and their counterstreaming flows

et al. 2020

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Solar filaments, also called solar prominences when appearing above the solar limb, are cold, dense materials suspended in the hot tenuous solar corona, consisting of numerous long, fibril-like threads. These threads are the key to disclosing the physics of solar filaments. Similar structures also exist in galaxy clusters. Besides their mysterious formation, filament threads are observed to move with alternating directions, which are called counterstreaming flows. However, the origin of these flows has not been clarified yet. Here we report that turbulent heating at the solar surface is the key, which randomly evaporates materials from the solar surface to the corona, naturally reproducing the formation and counterstreamings of the sparse threads in the solar corona. We further suggest that while the cold Hα counterstreamings are mainly due to longitudinal oscillations of the filament threads, there are million-kelvin counterstreamings in the corona between threads, which are alternating unidirectional flows.

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“…Our Fig. 5a clearly shows that counterstreamings are present in our simulations due to random heating localised at the footpoints, as also suggested by Kucera et al [35]. While Fig.…”

Section: Discussionsupporting

confidence: 89%

“…The counterstreamings were also detected in extreme ultraviolet (EUV) spectral lines, which correspond to plasma with the temperature around 10 5 − 10 6 degrees [refs. 5,[34][35][36][37]. A puzzling characteristic of the EUV counterstreamings is that their velocity can be up to 100 km s −1 [ref .…”

Section: Introductionmentioning

confidence: 99%

Simulations of solar filament fine structures and their counterstreaming flows

et al. 2020

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“…Using the canonical values of the prominence density (10 −11 to 10 −10 kg m −3 ) (Labrosse et al 2010) and the observed speeds of the prominence surge (10 to 25 km s −1 ), we obtained an energy flux of 10 W m −2 to 1000 W m −2 . This is in the range of energy fluxes that are sufficient to generate and sustain a quiescent corona (Withbroe & Noyes 1977;Kucera et al 2014) around a prominence.…”

Section: Discussionmentioning

confidence: 99%

Hot prominence spicules launched from turbulent cool solar prominences

Chitta

Peter

Li³

2019

A&A

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A solar filament is a dense cool condensation that is supported and thermally insulated by magnetic fields in the rarefied hot corona. Its evolution and stability, leading to either an eruption or disappearance, depend on its coupling with the surrounding hot corona through a thin transition region, where the temperature steeply rises. However, the heating and dynamics of this transition region remain elusive. We report extreme-ultraviolet observations of quiescent filaments from the Solar Dynamics Observatory that reveal prominence spicules propagating through the transition region of the filament-corona system. These thin needle-like jet features are generated and heated to at least 0.7 MK by turbulent motions of the material in the filament. We suggest that the prominence spicules continuously channel the heated mass into the corona and aid in the filament evaporation and decay. Our results shed light on the turbulence-driven heating in magnetized condensations that are commonly observed on the Sun and in the interstellar medium.

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“…Mass flows of the cool prominence material are observed ubiquitously in prominence threads (see the review by Parenti (2014), and recent observations by Alexander et al (2013); Kucera et al (2014); Diercke et al (2018)). Combined flows in small-scale threads and waves were also detected and studied in solar prominences by Okamoto et al (2007) and in coronal loops with cool prominence material by Ofman & Wang (2008).…”

Section: Introductionmentioning

confidence: 99%

Fast Magnetosonic Waves and Flows in a Solar Prominence Foot: Observations and Modeling

Ofman,

Kucera

2020

Preprint

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We study recent observations of propagating fluctuations in a prominence foot with Hinode Solar Optical Telescope (SOT) high-resolution observations in Ca II and Hα emission which we identify as nonlinear fast magnetosnic waves. Here we analyze further the observations of propagating waves and flows with Interface Region Imaging Spectrograph (IRIS) Mg II slit jaw images, in addition to Hinode/SOT Ca II images. We find that the waves have typical periods in the range of 5 − 11 minutes and wavelengths in the plane of the sky (POS) of about 2000 km, while the flows in narrow threads have typical speed in the POS of ∼ 16 − 46 km s −1 . We also detect apparent kink oscillations in the threads with flowing material, and apply coronal seismology to estimate the magnetic field strength in the range 5-17 G. Using 2.5D MHD we model the combined effects of nonlinear waves and flows on the observed dynamics of the prominence material, and reproduce the propagating and refracting fast magnetosonic waves, as well as standing kink-mode waves in flowing material along the magnetic field. The modeling results are in good qualitative agreements with the observations of the various waves and flows in the prominence foot, further confirming coronal seismology analysis and improving the understanding of the fine scale dynamics of the prominence material.

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Mass Flows in a Prominence Spine as Observed in Euv

Cited by 8 publications

References 39 publications

Simulations of solar filament fine structures and their counterstreaming flows

Simulations of solar filament fine structures and their counterstreaming flows

Hot prominence spicules launched from turbulent cool solar prominences

Fast Magnetosonic Waves and Flows in a Solar Prominence Foot: Observations and Modeling

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