Comet Lovejoy deposits 10^14-10^16 W via SPMI, below the 10^17 W brightening intensity but potentially able to trigger solar flares as a magnetic perturbation.
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5 Pith papers cite this work. Polarity classification is still indexing.
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astro-ph.SR 5representative citing papers
3D MHD modeling reveals Y-points do not coincide with cusp tips in candle-flame flares and apparent downflow speeds underestimate Alfvén speeds by 2-10x due to projection effects.
MHD modeling of the 2024 October 26 CME demonstrates that specific pre-eruptive magnetic flux rope footpoint locations and near-real-time background fields are required to reproduce observed complex morphology from multiple viewpoints without fine-tuning.
Column mass and temperature profile steepness dominate He II 304 Å line formation in the February 15 2022 eruptive prominence, with radiative processes outweighing collisional excitation.
3D MHD simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.
citing papers explorer
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Sungrazer comets as analogs of star-planet magnetic interactions
Comet Lovejoy deposits 10^14-10^16 W via SPMI, below the 10^17 W brightening intensity but potentially able to trigger solar flares as a magnetic perturbation.
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On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\'enic Supra-Arcade Plasma Downflows
3D MHD modeling reveals Y-points do not coincide with cusp tips in candle-flame flares and apparent downflow speeds underestimate Alfvén speeds by 2-10x due to projection effects.
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Understanding the complex morphology of a CME II: how pre-eruptive conditions shape CME evolution
MHD modeling of the 2024 October 26 CME demonstrates that specific pre-eruptive magnetic flux rope footpoint locations and near-real-time background fields are required to reproduce observed complex morphology from multiple viewpoints without fine-tuning.
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Analysis of Eruptive Prominence Plasma Parameters' Effects on the \ion{He}{2} 304~\AA\ Line with Solar Orbiter EUI Observations
Column mass and temperature profile steepness dominate He II 304 Å line formation in the February 15 2022 eruptive prominence, with radiative processes outweighing collisional excitation.
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Evolution of reconnection flux during eruption of magnetic flux ropes
3D MHD simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.