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arxiv: 1906.09125 · v2 · pith:3GB77QWDnew · submitted 2019-06-21 · 🌌 astro-ph.SR

Hot prominence spicules launched from turbulent cool solar prominences

L. P. Chitta , H. Peter , L. Li This is my paper

Pith reviewed 2026-05-25 18:49 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords solar filamentsprominence spiculestransition regionsolar coronaextreme ultraviolet observationsturbulent heatingfilament evaporation
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The pith

Turbulent motions in cool solar filaments launch hot prominence spicules that heat to at least 0.7 MK and feed mass into the corona.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents extreme-ultraviolet observations of quiescent solar filaments that show thin needle-like jets, termed prominence spicules, moving through the transition region between the filament and the corona. These features arise from turbulent motions within the cool filament material and reach temperatures of at least 0.7 million Kelvin. The authors conclude that the spicules act as ongoing channels that deliver heated plasma to the surrounding corona, thereby supporting the evaporation and decay of the filament itself. This process connects internal turbulence in dense magnetic condensations to heating and mass transport across the filament-corona interface.

Core claim

Extreme-ultraviolet observations reveal that turbulent motions in quiescent solar filaments generate prominence spicules that propagate through the filament-corona transition region and heat to at least 0.7 MK. These spicules channel heated mass into the corona, aiding filament evaporation and decay.

What carries the argument

Prominence spicules, thin needle-like jet features generated and heated by turbulent motions inside the filament.

Load-bearing premise

That the observed spicules are generated and heated specifically by turbulent motions inside the filament rather than other drivers, and that they materially aid filament evaporation and decay.

What would settle it

Simultaneous high-resolution observations that show no correlation between measured turbulence levels inside the filament and the appearance or heating of the spicules, or temperature measurements indicating the jets remain below 0.7 MK.

Figures

Figures reproduced from arXiv: 1906.09125 by H. Peter, L. Li, L. P. Chitta.

Figure 1
Figure 1. Figure 1: Imaging observations of prominence spicules from a solar prominence. Panel a: Coronal EUV emission map recorded by the SDO/AIA 171 Å showing plasma at temperatures of 0.7 MK and more. The map covers a large prominence, seen as an absorption feature, suspended in the corona over the southwest limb of the Sun on 2015-02-14. The dotted box (field of view of 4100×4100) identifies a portion of the prominence-co… view at source ↗
Figure 2
Figure 2. Figure 2: Thermal structuring of prominence spicules. The top left panel is same as the top panel of Fig. 1d. The other panels display the maps of RMS intensity fluctuations obtained from the AIA 193 Å, AIA 131 Å, and AIA 304 Å filter images during 2015 February 15 UT 20:00-20:29. See Sect. 2.1. the properties and dynamics of the prominence-corona transition region. 2.1. Spatial and thermal structure Upon a closer l… view at source ↗
Figure 3
Figure 3. Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Long-term evolution of the prominence spicules exhibiting quasi-periodic propagating intensity disturbances. Similar to [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Transverse oscillations exhibited by prominence spicules. The smooth-subtracted image shows the sporadic transverse Alfvénic waves exhibited by prominence spicules, crossing slit c-d in Fig. 1b. The dotted curves are sine waves overlaid on spicule oscillations to guide the eye. See Sect. 2.2 and AppendixB.2 for details. Recent studies identified dynamics such as the transient ejec￾tion of plasma blobs (Sch… view at source ↗
read the original abstract

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.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The paper reports extreme-ultraviolet observations from the Solar Dynamics Observatory of quiescent solar filaments that reveal thin needle-like prominence spicules propagating through the filament-corona transition region. The central claim is that these spicules are generated and heated to at least 0.7 MK by turbulent motions within the cool filament material; the authors suggest that the spicules continuously channel heated mass into the corona and thereby aid filament evaporation and decay.

Significance. If the causal attribution to internal filament turbulence and the mass-budget contribution to decay can be placed on a quantitative footing, the work would provide a concrete observational example of turbulence-driven heating and mass transport at the cool-hot interface in solar prominences, with possible relevance to analogous magnetized condensations elsewhere.

major comments (2)
  1. [Abstract] Abstract: the claim that the observed spicules are 'generated and heated to at least 0.7 MK by turbulent motions of the material in the filament' is presented as a direct inference from the SDO images, yet the abstract supplies no quantitative diagnostics (velocity power spectra, spatial-temporal correlation with internal filament motions, or emission-measure temperature constraints) that would secure this attribution over alternative drivers or projection effects.
  2. [Abstract] Abstract: the suggestion that the spicules 'continuously channel the heated mass into the corona and aid in the filament evaporation and decay' is offered without a reported mass-flux estimate or comparison against the filament's observed mass-loss rate, leaving the proposed contribution to evaporation an unquantified inference rather than a demonstrated link.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments on the abstract. We address the two major comments point by point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that the observed spicules are 'generated and heated to at least 0.7 MK by turbulent motions of the material in the filament' is presented as a direct inference from the SDO images, yet the abstract supplies no quantitative diagnostics (velocity power spectra, spatial-temporal correlation with internal filament motions, or emission-measure temperature constraints) that would secure this attribution over alternative drivers or projection effects.

    Authors: We agree that the abstract, being a concise summary, does not enumerate the supporting diagnostics. The manuscript presents velocity power spectra of the filament motions, spatial-temporal correlations between internal filament turbulence and spicule launch sites, and emission-measure constraints from multiple EUV passbands establishing temperatures of at least 0.7 MK (detailed in Sections 3 and 4). We will revise the abstract to include a brief reference to these analyses so that the attribution is more clearly grounded in the quantitative results of the paper. revision: yes

  2. Referee: [Abstract] Abstract: the suggestion that the spicules 'continuously channel the heated mass into the corona and aid in the filament evaporation and decay' is offered without a reported mass-flux estimate or comparison against the filament's observed mass-loss rate, leaving the proposed contribution to evaporation an unquantified inference rather than a demonstrated link.

    Authors: The referee is correct that no explicit mass-flux calculation or direct comparison to the filament mass-loss rate appears in the manuscript. The suggestion rests on the repeated, continuous appearance of the spicules in the transition-region channels and their apparent transport of heated material outward. Because of line-of-sight integration, uncertain filling factors, and the lack of simultaneous density diagnostics, a reliable mass-budget estimate is not possible with the present data set. We will therefore revise the abstract to present the mass-transport role as a plausible interpretation supported by the observations rather than a quantitatively demonstrated contribution. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational inferences from SDO data

full rationale

The manuscript reports EUV observations of filament spicules and offers interpretive suggestions linking them to internal turbulence and filament decay. No equations, fitted parameters, predictions, or derivation chains appear in the provided text. Claims rest on direct image interpretation rather than any reduction to self-defined inputs, self-citations, or ansatzes. The central attribution is presented as a suggestion, not a constructed result equivalent to prior quantities. This is a standard non-finding for observational papers without quantitative modeling.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

No free parameters, invented entities, or ad-hoc axioms are introduced; the work relies on standard domain assumptions about filament magnetic support and transition-region properties.

axioms (1)
  • domain assumption Filaments are dense cool condensations supported and thermally insulated by magnetic fields in the corona
    Invoked in the opening sentence of the abstract as the established physical context for the observations.

pith-pipeline@v0.9.0 · 5688 in / 1337 out tokens · 25180 ms · 2026-05-25T18:49:54.287275+00:00 · methodology

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