Papers
Papers
The list below is shown in inverse chronological order by default.
Use the rail on the left to bring first-author papers,
collaborative papers, or the dataset record to the front without
changing the underlying record.
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Summary
Coronal elemental abundance patterns (FIP bias) encode chromospheric physics. Coupling HYDRAD chromospheric simulations with the ponderomotive-force code FIPpy, we show the ponderomotive model remains viable under dynamic heating, while acoustic flux and turbulence strongly reshape fractionation: very low acoustic flux lets thermal velocities dominate and produce unusual element ordering, whereas turbulence—including enhanced turbulence in flares—suppresses fractionation and may explain weaker FIP bias observed during flares.
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Summary
Elemental abundances in solar flares vary spatially and in time; we use radiative hydrodynamic simulations of strong evaporation that advect low-FIP-enhanced plasma into loops. Sharply peaked enhancements produce a localized abundance peak near the apex and favour coronal rain, whereas broader, weaker heating yields a more uniformly fractionated corona without rain; stronger heating compresses enriched plasma toward the apex and again enables rain—suggesting observational links between rain intensity, flare heating, and fractionation.
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Summary
Sulphur sits just above the canonical low-/high-FIP divide (10.36 eV), so its fractionation is especially sensitive to how plasma is processed in the solar atmosphere. Using nine Hinode/EIS rasters and potential-field source-surface (PFSS) models of coronal loops, we quantify how sulphur’s FIP bias relates to loop properties, employing four diagnostic line pairs and differential emission measures from a regularised inversion. We find abundances of low-FIP species, sulphur included, decline relative to high-FIP argon once mean magnetic fields exceed about 150 G, with no clear dependence on loop length—evidence that FIP fractionation is modulated by coronal loop field strength.
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Summary
Coronal composition varies in space and time; when we include those variations in flare simulations we can produce coronal rain in hydrodynamic models. We start from an initial corona with inverse-FIP composition like active M dwarfs rather than a solar-like FIP corona, and we find flare evolution can resemble the solar high-FIP-enrichment case, but coronal rain is harder to form when low-FIP elements are depleted.
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Summary
We bring together recent solar observations and theoretical work on inverse-FIP plasma. We summarize the main physical interpretations, observational signatures, and open questions about where and how inverse-FIP composition is produced.
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Summary
Coronal plumes are narrow bright structures rooted in coronal holes; their composition probes magnetic connectivity and fractionation. Using Solar Orbiter/SPICE with the SAFFRON pipeline—plus EUV imaging and magnetograms—we derive sulfur-to-nitrogen in two equatorial-hole plumes (March–April 2024). Sulfur fractionation is steady within uncertainties and co-located with strong magnetic footpoints versus interplume plasma, supporting sulfur fractionation in plumes and chromospheric wave driving in line with the ponderomotive-force picture.
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Summary
Photospheric and coronal compositions differ (the FIP effect); typical FIP bias is near unity in coronal holes, roughly 1.5–2 in the quiet Sun, and around 3 in active regions. We compare three Hinode/EIS diagnostics—Si X/S X, Ca XIV/Ar XIV, and Fe XVI/S XIII—between quiet Sun and an active region, varying per-pixel signal-to-noise cuts: cuts change how many pixels remain usable and trim high-bias tails, while median FIP bias is largely unchanged—arguing for nuanced interpretation rather than a single default recipe.
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Summary
This manuscript looks for chromospheric observables that can be directly associated with the ponderomotive force thought to drive solar abundance fractionation. It links spectroscopic behaviour in the lower atmosphere to the processes that later shape coronal composition.
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Summary
Using a Hinode/EIS catalogue of 1,449 flares from 2011-2024, this paper measures how EUV non-thermal velocities evolve before soft X-ray flare onset across C-, M-, and X-class events. It finds that line broadening typically begins 4-25 minutes before GOES start in C and M flares, with earlier and more extended precursor behaviour in many eruptive M-class events.
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Summary
This paper introduces spatiotemporally varying elemental abundances into radiative hydrodynamic flare simulations to test how local composition changes feed back on loop cooling. It shows that abundance shifts driven by evaporation can modify radiative losses enough to promote condensations in impulsively heated loops, linking low-FIP enrichment to coronal rain formation.
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Summary
This paper tracks FIP bias through the 2017 September 10 X8.2 flare using 12 Hinode/EIS rasters and two abundance diagnostics. It finds persistent high-FIP-bias plasma near loop tops and near-photospheric values at footpoints, consistent with mixing between reconnection-downflow plasma and chromospheric evaporation.
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Summary
This paper investigates localized inverse-FIP plasma in complex active regions and asks whether subchromospheric reconnection can generate the waves needed for this fractionation pattern. The results point to strong light bridges and coalescing sunspot umbrae as favored sites, with flare-driven evaporation helping the inverse-FIP plasma become visible in the corona.
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Summary
This paper measures upward and downward propagating Alfvén waves in the chromosphere and finds clear evidence for wave reflection. The observed differences between resonant and nonresonant cases connect chromospheric wave behaviour to ponderomotive-force fractionation and the solar FIP effect.
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Summary
This paper combines Hinode/EIS and IRIS observations of AR 12759 to look for direct chromospheric signatures of plasma fractionation. Differences between the leading and following polarities in both coronal FIP bias and IRIS line widths are consistent with resonant and nonresonant wave-driven fractionation in the chromosphere.
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Summary
This paper tests why the Sun-as-a-star correlation between coronal composition and F10.7 becomes nonlinear during higher activity. Using coordinated JVLA, Hinode/EIS, and SDO observations, it shows that strong magnetic concentrations and gyroresonance above sunspots alter the local relationship between radio flux and coronal abundance.
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Summary
This coordination paper describes the Slow Wind Solar Orbiter Observing Plan and its joint remote-sensing and in situ campaign around the first close perihelion passage. Post-observation analysis showed that slow wind from two of the three target regions reached the spacecraft, providing a template for future magnetically guided observing campaigns.
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Summary
This paper studies a 2022 March 18 event in which a coronal dimming merged with the southern polar coronal hole for at least 72 hr. Multi-spacecraft imaging, Hinode/EIS spectroscopy, and magnetic-field analysis show that the merged region took on coronal-hole-like flow properties and point to component reconnection as the mechanism that allowed the dimming to intrude onto the coronal-hole boundary.
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Summary
This paper tracks NOAA AR 12967 simultaneously from Solar Orbiter and Earth to test whether an S-web magnetic corridor can supply the slow solar wind. Blueshifted upflows along a narrow open-field corridor and magnetic modelling support the interpretation that S-web structure provided a source region for the observed wind.
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Summary
This survey paper measures FIP bias in 28 active regions with Hinode/EIS and compares the results with age, flux, and evolutionary state. It finds no simple dependence on total unsigned flux or age, but does find weaker trends with evolutionary stage and magnetic flux density, indicating that active-region composition depends on a combination of local processes.
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Summary
This paper follows plasma composition as a sigmoid formed into a flux rope and later erupted as a CME. Photospheric-composition plasma appeared near the polarity inversion line during strong flux cancellation, while the core field remained more coronal, supporting flux-rope formation through photospheric cancellation and reconnection.
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Summary
Using Hinode/EIS observations of a small flare, this paper compares abundance diagnostics before and during the event. It finds a strong flare-time increase in the Ca XIV/Ar XIV ratio while Si X/S X remains comparatively unchanged, and discusses how flare heating and chromospheric plasma injection may affect different diagnostics.
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Summary
This paper uses high-resolution spectropolarimetry to study intensity and circular-polarization fluctuations in a sunspot chromosphere. It finds a clear link between the two signals over a narrow range of field inclinations, consistent with Alfvénic perturbations in the sunspot.
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Summary
This paper combines photospheric, chromospheric, and coronal observations with magnetic modelling to map composition structure around a large sunspot. It finds that fractionated coronal plasma is magnetically linked to locations of chromospheric Alfvénic fluctuations, tying sunspot wave activity to observable coronal abundance variation.
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Summary
This paper studies inverse-FIP patches in the complex active region AR 12673 and links them to strong light bridges and coalescing sunspots. The results support a scenario in which subphotospheric reconnection generates waves below the chromosphere, while flare evaporation lifts the resulting inverse-FIP plasma into the corona.
Representative figures for the first-author papers are collected on
the figures page. The public dataset is
included in this list as a research output.