New EIS effective area curves confirm factor-of-two long-wavelength degradation without fine structure and reveal inverse FIP bias with Fe/H at 0.57 of photospheric value at 10 MK, confirmed by Chandrayaan-2 SXM spectra.
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1D multi-fluid MHD models show inverse FIP effect can arise for upward Alfvén waves when magnetic field strength and flux-tube expansion counteract multi-fluid dissipation and damping.
SEUSHI is a compact dual-mode instrument that delivers 1-arcmin temperature maps every 5 seconds plus 0.2-nm EUV spectra and photon-counting SXR spectroscopy to study flare initiation and elemental abundances.
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.
Observational evidence points to the chromosphere as the site of chemical fractionation responsible for the FIP effect in the solar corona.
citing papers explorer
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Modeling Flare Continuum Emission Observed by Hinode/EIS: Instrument Calibration and Element Composition Results
New EIS effective area curves confirm factor-of-two long-wavelength degradation without fine structure and reveal inverse FIP bias with Fe/H at 0.57 of photospheric value at 10 MK, confirmed by Chandrayaan-2 SXM spectra.
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Multi-fluid multi-species models for inverse FIP-effect
1D multi-fluid MHD models show inverse FIP effect can arise for upward Alfvén waves when magnetic field strength and flux-tube expansion counteract multi-fluid dissipation and damping.
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Solar Extreme Ultraviolet Spectrograph and High-energy Imager (SEUSHI): Design, Development, and Pre-Flight Calibration
SEUSHI is a compact dual-mode instrument that delivers 1-arcmin temperature maps every 5 seconds plus 0.2-nm EUV spectra and photon-counting SXR spectroscopy to study flare initiation and elemental abundances.
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Investigating Pre-flare Signatures in Spectroscopic Observations of an X9-class Solar Flare
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.
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The connection between solar coronal abundances and the underlying lower atmospheric properties
Observational evidence points to the chromosphere as the site of chemical fractionation responsible for the FIP effect in the solar corona.
- Transport of electrons in tangled magnetic fields