Elemental composition in quiescent prominences

Parenti, S.; Zanna, G. Del; Vial, J. C.

doi:10.1051/0004-6361/201935147

Cited by 20 publications

(14 citation statements)

References 49 publications

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“…The dominantly photospheric plasma composition of the erupting sigmoid/flux rope is in agreement with the photospheric origin material in erupting (e.g. Widing et al 1986;Feldman 1992;Spicer et al 1998) and quiescent prominences/filaments (Parenti et al 2019).…”

Section: Local Evolution -Flux Ropesupporting

confidence: 80%

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Evolution of Plasma Composition in an Eruptive Flux Rope

Baker,

Green,

Brooks

et al. 2021

Preprint

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Magnetic flux ropes are bundles of twisted magnetic field enveloping a central axis. They harbor free magnetic energy and can be progenitors of coronal mass ejections (CMEs), but identifying flux ropes on the Sun can be challenging. One of the key coronal observables that has been shown to indicate the presence of a flux rope is a peculiar bright coronal structure called a sigmoid. In this work, we show Hinode EUV Imaging Spectrometer (EIS) observations of sigmoidal active region 10977. We analyze the coronal plasma composition in the active region and its evolution as the sigmoid (flux rope) forms and erupts as a CME. Plasma with photospheric composition was observed in coronal loops close to the main polarity inversion line during episodes of significant flux cancellation, suggestive of the injection of photospheric plasma into these loops driven by photospheric flux cancellation. Concurrently, the increasingly sheared core field contained plasma with coronal composition. As flux cancellation decreased and the sigmoid/flux rope formed, the plasma evolved to an intermediate composition in between photospheric and typical active region coronal compositions. Finally, the flux rope contained predominantly photospheric plasma during and after a failed eruption preceding the CME. Hence, plasma composition observations of active region 10977 strongly support models of flux rope formation by photospheric flux cancellation forcing magnetic reconnection first at the photospheric level then at the coronal level.

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Section: Local Evolution -Flux Ropesupporting

confidence: 80%

“…Feldman 1992;Spicer et al 1998;Ciaravella et al 2000). Parenti et al (2019) confirmed that quiescent prominences also have photospheric composition.…”

Section: Introductionmentioning

confidence: 63%

Evolution of Plasma Composition in an Eruptive Flux Rope

Baker,

Green,

Brooks

et al. 2021

Preprint

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“…Another environment to which this work may extend is that of prominences. These regions of cooler, higher density plasma in the TR and corona are shown in the recent work of Parenti et al (2019) to have similar pressure to that which is used in the modelling here. The structures are relatively low in the atmosphere, and so the radiation field will be diluted by a similar amount as here.…”

Section: Discussionsupporting

confidence: 53%

The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere

Dufresne,

Del Zanna,

Badnell

2021

Preprint

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To predict line emission in the solar atmosphere requires models which are fundamentally different depending on whether the emission is from the chromosphere or the corona. At some point between the two regions, there must be a change between the two modelling regimes. Recent extensions to the coronal modelling for carbon and oxygen lines in the solar transition region have shown improvements in the emission of singly-and doubly-charged ions, along with Li-like ions. However, discrepancies still remain, particularly for singly-charged ions and intercombination lines. The aim of this work is to explore additional atomic processes that could further alter the charge state distribution and the level populations within ions, in order to resolve some of the discrepancies. To this end, excitation and ionisation caused by both the radiation field and by atom-ion collisions have been included, along with recombination through charge transfer. The modelling is carried out using conditions which would be present in the quiet Sun, which allows an assessment of the part atomic processes play in changing coronal modelling, separately from dynamic and transient events taking place in the plasma. The effect the processes have on the fractional ion populations are presented, as well as the change in level populations brought about by the new excitation mechanisms. Contribution functions of selected lines from low charge states are also shown, to demonstrate the extent to which line emission in the lower atmosphere could be affected by the new modelling.

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“…Prominences and filaments can be fairly stable regions. These quiescent structures retain photospheric composition according to Parenti et al (2019). Quiescent filaments, that may exist at all latitudes, at solar minimum are preferentially located at high latitudes, 45 • -50 • , and often form a crown around the polar caps.…”

Section: Coronal Streamers During the Solar Cyclementioning

confidence: 99%

Observations of the Solar Corona from Space

et al. 2020

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Space observations of the atmosphere of the Sun, obtained in half a century of dedicated space missions, provide a well established picture of the medium and large-scale solar corona, which is highly variable with the level of solar activity through a solar cycle and evolves with the long-term evolution of the magnetic cycles. In this review, we summarize the physical properties and dynamics of the medium and large-scale corona, consisting primarily of active regions, streamers and coronal holes; describe the dependence of coronal patterns on the magnetic field patterns changing through the solar cycle and the properties of the regions of open magnetic flux channeling the solar wind; the ubiquitous presence of fluctuations in the outer corona; the rotational properties of the large-scale corona; and the persistent hemispheric asymmetries in the emergence of magnetic fields and the distribution of the coronal emission.

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Elemental composition in quiescent prominences

Cited by 20 publications

References 49 publications

Evolution of Plasma Composition in an Eruptive Flux Rope

Evolution of Plasma Composition in an Eruptive Flux Rope

The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere

Observations of the Solar Corona from Space

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