The total number of spicules on the solar surface and their role in heating and mass balanace in the solar corona

Mamedov, S. G.; Kuli-Zade, D. M.; Alieva, Z. F.; Musaev, M. M.; Mustafa, F. R.

doi:10.1134/s1063772916080060

Cited by 4 publications

(4 citation statements)

References 19 publications

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“…Super-sonic motions associated with spicules and some fibrils are notable by their absence. For a typical length of a spicule of 5-10 , and assuming that 10 5 such spicules are present at any time on the Sun (Mamedov et al 2016), we would expect to see one spicule cross a randomly oriented slit of this length at any time. The small-scale features at line-center observed almost everywhere are therefore not related to spicules.…”

Section: Discussionmentioning

confidence: 99%

“…We note that the area coverage of spicules inferred from data above the limb is too small to contribute signifi-cantly to the spatially-averaged profiles, (e.g. Judge & Carlsson 2010;Mamedov et al 2016). However, models do show that the k 2 and K 2 peaks form substantially lower in the atmosphere (Vernazza et al 1981;Leenaarts et al 2013;Bjørgen et al 2018).…”

Section: Observations and Their Analysesmentioning

confidence: 91%

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New light on an old problem of the cores of solar resonance lines

Judge,

Kleint,

Leenaarts

et al. 2020

Preprint

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We re-examine a 50+ year-old problem of deep central reversals predicted for strong solar spectral lines, in contrast to the smaller reversals seen in observations. We examine data and calculations for the resonance lines of H I, Mg II and Ca II, the self-reversed cores of which form in the upper chromosphere. Based on 3D simulations as well as data for the Mg II lines from IRIS, we argue that the resolution lies not in velocity fields on scales in either of the micro-or macro-turbulent limits. Macroturbulence is ruled out using observations of optically thin lines formed in the upper chromosphere, and by showing that it would need to have unreasonably special properties to account for critical observations of the Mg II resonance lines from the IRIS mission. The power in "turbulence" in the upper chromosphere may therefore be substantially lower than earlier analyses have inferred. Instead, in 3D calculations horizontal radiative transfer produces smoother source functions, smoothing out intensity gradients in wavelength and in space. These effects increase in stronger lines. Our work will have consequences for understanding the onset of the transition region, the energy in motions available for heating the corona, and for the interpretation of polarization data in terms of the Hanle effect applied to resonance line profiles.

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Section: Discussionmentioning

confidence: 99%

Section: Observations and Their Analysesmentioning

confidence: 91%

New light on an old problem of the cores of solar resonance lines

Judge,

Kleint,

Leenaarts

et al. 2020

Preprint

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“…De Pontieu et al (2009) derived an energy of 10 23 erg for Type II spicules, while Klimchuk (2012) derived 8 × 10 22 erg based on an emission measure distribution. Mamedov et al (2016) discussed several possibilities for energy input due to both classical and Type II spicules, which in some instances are an order of magnitude larger than the above values. In a recent work, Samanta et al (2019) performed an order-of-magnitude estimate of the kinetic energy of spicules (1.2 × 10 23 erg), and the maximum available magnetic energy (2.5 × 10 25 erg) at the foot-points of spicules based on Hα spectral scans and magnetic field data from the Goode Solar Telescope.…”

Section: Introductionmentioning

confidence: 93%

Implications of spicule activity on coronal loop heating and catastrophic cooling

Nived

Scullion

Doyle

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report on the properties of coronal loop foot-point heating with observations at the highest resolution, from the CRisp Imaging Spectro-Polarimeter (CRISP) located at the Swedish 1-m Solar Telescope (SST) and co-aligned NASA Solar Dynamics Observatory (SDO) observations, of Type II spicules in the chromosphere and their signatures in the EUV corona. Here, we address one important issue, as to why there is not always a one-to-one correspondence, between Type II spicules and hot coronal plasma signatures, i.e. beyond TR temperatures. We do not detect any difference in their spectral properties in a quiet Sun region compared to a region dominated by coronal loops. On the other hand, the number density close to the foot-points in the active region is found to be an order of magnitude higher than in the quiet Sun case. A differential emission measure analysis reveals a peak at ∼5 × 105 K on the order of 1022 cm−5 K−1. Using this result as a constraint, we conduct numerical simulations and show that with an energy input of 1.25 × 1024 erg (corresponding to ∼10 RBEs contributing to the burst) we manage to reproduce the observation very closely. However, simulation runs with lower thermal energy input do not reproduce the synthetic AIA 171 Å signatures, indicating that there is a critical number of spicules required in order to account for the AIA 171 Å signatures in the simulation. Furthermore, the higher energy (1.25 × 1024 ergs) simulations reproduce catastrophic cooling with a cycle duration of ∼5 hours, matching a periodicity we observe in the EUV observations.

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“…De Pontieu et al (2009) derived an energy of 10 23 erg for Type II spicules, while Klimchuk (2012) derived 8 × 10 22 erg based on an emission measure distribution. Mamedov et al (2016) discussed several possibilities for energy input due to both classical and Type II spicules, which in some instances are an order of magnitude larger than the above values. In a recent work, Samanta et al (2019) performed an order-of-magnitude estimate of the kinetic energy of spicules (1.2 × 10 23 erg), and the maximum available magnetic energy (2.5 × 10 25 erg) at the footpoints of spicules based on Hα spectral scans and magnetic field data from the Goode Solar Telescope.…”

Section: Introductionmentioning

confidence: 93%

Implications of spicule activity on coronal loop heating and catastrophic cooling

Nived,

Scullion,

Doyle

et al. 2021

Preprint

View full text Add to dashboard Cite

We report on the properties of coronal loop foot-point heating with observations at the highest resolution, from the CRisp Imaging Spectro-Polarimeter (CRISP) located at the Swedish 1-m Solar Telescope (SST) and co-aligned NASA Solar Dynamics Observatory (SDO) observations, of Type II spicules in the chromosphere and their signatures in the EUV corona. Here, we address one important issue, as to why there is not always a one-to-one correspondence, between Type II spicules and hot coronal plasma signatures, i.e. beyond TR temperatures. We do not detect any difference in their spectral properties in a quiet Sun region compared to a region dominated by coronal loops. On the other hand, the number density close to the foot-points in the active region is found to be an order of magnitude higher than in the quiet Sun case. A differential emission measure analysis reveals a peak at ∼ 5 × 10 5 K on the order of 10 22 cm −5 K −1 . Using this result as a constraint, we conduct numerical simulations and show that with an energy input of 1.25 × 10 24 erg (corresponding to ∼10 RBEs contributing to the burst) we manage to reproduce the observation very closely. However, simulation runs with lower thermal energy input do not reproduce the synthetic AIA 171 Å signatures, indicating that there is a critical number of spicules required in order to account for the AIA 171 Å signatures in the simulation. Furthermore, the higher energy (1.25 × 10 24 ergs) simulations reproduce catastrophic cooling with a cycle duration of ∼5 hours, matching a periodicity we observe in the EUV observations.

show abstract

The total number of spicules on the solar surface and their role in heating and mass balanace in the solar corona

Cited by 4 publications

References 19 publications

New light on an old problem of the cores of solar resonance lines

New light on an old problem of the cores of solar resonance lines

Implications of spicule activity on coronal loop heating and catastrophic cooling

Implications of spicule activity on coronal loop heating and catastrophic cooling

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