A new source alignment technique applied to PSP and SO data reveals the solar wind speed increases by an average of 45% per radial decade between the spacecraft, indicating ongoing acceleration beyond 15 solar radii.
2016 Slow Solar Wind: Observations and Modeling
7 Pith papers cite this work. Polarity classification is still indexing.
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Sulphur abundances decrease above 150 G in coronal loops, indicating FIP fractionation is modulated by mean magnetic field strength.
Leading boundary of a coronal hole has higher plasma temperature, stronger unipolar field, and lower spatial irregularity than trailing boundary due to organized loops versus dispersed bipoles.
Polytropic stellar wind models are extended beyond extreme adiabatic cases to non-adiabatic localized heating, with added energy shown plausible relative to flares and relevant to solar wind observations.
Time-dependent MHD models of the corona-heliosphere system produce magnetic connectivities consistent with observed strahl occurrence rates, unlike steady-state models.
A multi-ion solar wind simulation with reflection-driven turbulence reproduces observed preferential heating of oxygen ions when compared to UVCS and SWICS data.
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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Signs of Sulphur fractionation under high magnetic field strength
Sulphur abundances decrease above 150 G in coronal loops, indicating FIP fractionation is modulated by mean magnetic field strength.
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Investigating the Relationship Between Physical Properties and Spatial Irregularities at Coronal Hole Boundaries
Leading boundary of a coronal hole has higher plasma temperature, stronger unipolar field, and lower spatial irregularity than trailing boundary due to organized loops versus dispersed bipoles.
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Polytropic stellar wind models with strongly localized heating
Polytropic stellar wind models are extended beyond extreme adiabatic cases to non-adiabatic localized heating, with added energy shown plausible relative to flares and relevant to solar wind observations.
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Magnetic Connectivity in the Time-Dependent Corona and Heliosphere
Time-dependent MHD models of the corona-heliosphere system produce magnetic connectivities consistent with observed strahl occurrence rates, unlike steady-state models.
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Global Multi-ion Solar Wind Model. I. Ion Temperatures
A multi-ion solar wind simulation with reflection-driven turbulence reproduces observed preferential heating of oxygen ions when compared to UVCS and SWICS data.
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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.