The Neon‐to‐Magnesium Abundance Ratio as a Tracer of the Source Region of Prominence Material

Spicer, D. S.; Feldman, U.; Widing, K. G.; Rilee, M. L.

doi:10.1086/305203

Cited by 36 publications

(22 citation statements)

References 5 publications

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“…Therefore, our analysis cannot definitively determine whether the filament plasma comes from the photosphere or chromosphere. Nonetheless, in agreement with Spicer et al (1998), our study does not support the coronal origin of filament plasma.…”

Section: Summary and Discussionsupporting

confidence: 60%

“…Filaments are about one hundred times cooler (T ∼10 4 K) and denser than the coronal material (T ∼10 6 K). Two crucial issues need to be addressed to understand the filament formation (e.g., Parenti 2014;Li & Zhang 2013;Zhou et al 2014): what is their magnetic structure (Yan et al 2015(Yan et al , 2016 and where does their material come from (Spicer et al 1998;Mackay et al 2010)? Our understanding on the origin of the filament material remains controversial.…”

Section: Introductionmentioning

confidence: 99%

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The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances

Song

Chen

et al. 2017

ApJL

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Solar filaments/prominences are one of the most common features in the corona, which may lead to energetic coronal mass ejections (CMEs) and flares when they erupt. Filaments are about one hundred times cooler and denser than the coronal material, and physical understanding of their material origin remains controversial. Two types of scenarios have been proposed: one argues that the filament plasma is brought into the corona from photosphere or chromosphere through a siphon or evaporation/injection process, while the other suggests that the material condenses from the surrounding coronal plasma due to thermal instability. The elemental abundance analysis is a reasonable clue to constrain the models, as the siphon or evaporation/injection model would predict that the filament material abundances are close to the photospheric or chromospheric ones, while the condensation model should have coronal abundances. In this letter, we analyze the elemental abundances of a magnetic cloud that contains the ejected filament material. The corresponding filament eruption occurred on 1998 April 29, accompanying an M6.8 class soft X-ray flare located at the heliographic coordinates S18E20 (NOAA 08210) and a fast halo CME with the linear velocity of 1374 km s −1 near the Sun. We find that the abundance ratios of elements with low and high First

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Section: Summary and Discussionsupporting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances

Song

Chen

et al. 2017

ApJL

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“…It is interesting to note that an FIP bias of a factor of 2 was measured in prominences by Spicer et al (1998) using Skylab, although they also found that different prominences had different compositions. Thus, a second possible origin of the XPE plasma might be the erupting prominence itself, and we might speculate that the portion closer to the reconnection site is partially heated by reconnection.…”

Section: Element Compositionmentioning

confidence: 99%

Hot Plasma Associated With a Coronal Mass Ejection

Landi

Miralles

Raymond

et al. 2013

ApJ

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We analyze coordinated observations from the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) on board Hinode of an X-ray Plasma Ejection (XPE) that occurred during the coronal mass ejection (CME) event of 2008 April 9. The XPE was trailing the CME core from behind, following the same trajectory, and could be identified both in EIS and XRT observations. Using the EIS spectrometer, we have determined the XPE plasma parameters, measuring the electron density, thermal distribution, and elemental composition. We have found that the XPE composition and electron density were very similar to those of the pre-event active region plasma. The XPE temperature was higher, and its thermal distribution peaked at around 3 MK; also, typical flare lines were absent from EIS spectra, indicating that any XPE component with temperatures in excess of 5 MK was likely either faint or absent. We used XRT data to investigate the presence of hotter plasma components in the XPE that could have gone undetected by EIS and found that-if at all present-these components have small emission measure values and their temperature is in the 8-12.5 MK range. The very hot plasma found in earlier XPE observations obtained by Yohkoh seems to be largely absent in this CME, although plasma ionization timescales may lead to non-equilibrium ionization effects that could make bright lines from ions formed in a 10 MK plasma not detectable by EIS. Our results supersede the XPE findings of Landi et al., who studied the same event with older response functions for the XRT Al-poly filter; the differences in the results stress the importance of using accurate filter response functions.

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“…This suggests a chromospheric origin for the cool material observed by UVCS. Spicer et al (1998) studied the FIP e †ect in prominences by measuring the Ne VI : Mg VI ratios from Skylab spectroheliograph data. They found intermediate values of the Ne/Mg abundance ratio, ranging from 1.4 to 2.2, compared with the photospheric value of 3.2 and the coronal value of 0.7.…”

Section: Emission Measure and Abundancesmentioning

confidence: 99%

Solar and Heliospheric ObservatoryObservations of a Helical Coronal Mass Ejection

Ciaravella

Raymond

Thompson

et al. 2000

ApJ

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The EUV Imaging Telescope (EIT), Large Angle Spectrometric Coronagraph (LASCO), and Ultraviolet Coronagraph Spectrometer (UVCS) instruments aboard the SOHO satellite observed a prominence eruption (coronal mass ejection) on 1997 December 12. Ejected plasma moved at about 130 km s~1 in the plane of the sky and showed Doppler shifts between [350 and ]30 km s~1. The eruption appeared as a strongly curved arch in EIT images low in the corona. Emission in ions ranging from Si III to O VI in the UVCS spectra indicates a temperature range between 104.5 and 105.5 K. The morphology of the bright emission regions seen by all three instruments suggests several strands of a helical structure of moderate pitch angle. A reasonable Ðt to the spatial structure and the velocity evolution measured by UVCS is provided by a left-handed helix untwisting at a rate of about 9 ] 10~4 radians s~1.

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The Neon‐to‐Magnesium Abundance Ratio as a Tracer of the Source Region of Prominence Material

Cited by 36 publications

References 5 publications

The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances

The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances

Hot Plasma Associated With a Coronal Mass Ejection

Solar and Heliospheric ObservatoryObservations of a Helical Coronal Mass Ejection

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