Multi-wavelength synthesis of a flux rope-trapped mini-prominence eruption and post-flare coronal rain
Abstract
Small-scale eruptive phenomena in the solar corona including miniature flux ropes and associated cool plasma condensations are not fully understood despite increasing high-resolution observations. We perform forward modeling based on a 2.5D MHD simulation capturing homologous flux rope eruptions, in-situ condensation leading to a mini-prominence, and subsequent post-flare coronal rain. Synthetic diagnostics are obtained using optically-thin EUV and UV emissions, and non-LTE radiative transfer treatment for the Hα line. The synthetic EUV emission reveals the flux ropes as bright rim-like structures. The corresponding UV diagnostic shows bright region, which is co-spatial with the dark core due to embedded cool plasma (∼ tens of kK) inside the flux rope, identifying an erupting mini-prominence. Spectral synthesis of Si IV 1402.77 A indicates an upward motion of the mini-filament, and reveals the presence of two predominant velocity components during eruption. At a later stage, thermal instability in post-flare arcades produces coronal rain with temperatures of ≈ 104 K. The EUV diagnostics reveal brightening at the downstream of the rain blob, indicating localized heating associated with compressional effects. The Hα spectral synthesis shows enhanced absorption signatures and red-shifted profiles corresponding to downflows of the coronal rain blobs up to ≈ 23 km s−1, whereas the Si IV 1402.77 A spectral profile shows the maximum downflow velocity of ≈50 km s−1, highlighting the evidence of thermodynamic and kinematic structuring within the falling rain blobs. The synthetic diagnostics provide clear, multi-wavelength signatures that can guide future high-resolution observations, and highlight the importance of small-scale reconnection-driven processes in shaping the multi-thermal structure (between MK to kK) of the solar corona.
Related
- Coronal Green-Line Emission During a Solar Prominence Eruption: Spectroscopic Evidence of Its Correspondence with the EUV Late Phase
- Enhanced Coronal Heating Detected across the Prominence–Corona Boundary Using DKIST/Cryo-NIRSP Spectropolarimetric Observations
- Solar Soft X-ray Coronal Dimming in a Failed Eruption Associated with Plasma Cooling
- Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal Jets
- Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal Jets
BibTeX
@misc{sen2026multiwavelength,
title = {{Multi-wavelength synthesis of a flux rope-trapped mini-prominence eruption and post-flare coronal rain}},
author = {Samrat Sen and Alexander G. M. Pietrow and Veronika Jercic and Patrick Antolin},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2608.06478},
eprint = {2608.06478},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.06478},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Multi-wavelength synthesis of a flux rope-trapped mini-prominence eruption and post-flare coronal rain
AU - Samrat Sen
AU - Alexander G. M. Pietrow
AU - Veronika Jercic
AU - Patrick Antolin
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2608.06478
UR - https://arxiv.org/abs/2608.06478
AB - Small-scale eruptive phenomena in the solar corona including miniature flux ropes and associated cool plasma condensations are not fully understood despite increasing high-resolution observations. We perform forward modeling based on a 2.5D MHD simulation capturing homologous flux rope eruptions, in-situ condensation leading to a mini-prominence, and subsequent post-flare coronal rain. Synthetic diagnostics are obtained using optically-thin EUV and UV emissions, and non-LTE radiative transfer treatment for the Hα line. The synthetic EUV emission reveals the flux ropes as bright rim-like structures. The corresponding UV diagnostic shows bright region, which is co-spatial with the dark core due to embedded cool plasma (∼ tens of kK) inside the flux rope, identifying an erupting mini-prominence. Spectral synthesis of Si IV 1402.77 A indicates an upward motion of the mini-filament, and reveals the presence of two predominant velocity components during eruption. At a later stage, thermal instability in post-flare arcades produces coronal rain with temperatures of ≈ 10^4 K. The EUV diagnostics reveal brightening at the downstream of the rain blob, indicating localized heating associated with compressional effects. The Hα spectral synthesis shows enhanced absorption signatures and red-shifted profiles corresponding to downflows of the coronal rain blobs up to ≈ 23 km s^−1, whereas the Si IV 1402.77 A spectral profile shows the maximum downflow velocity of ≈50 km s^−1, highlighting the evidence of thermodynamic and kinematic structuring within the falling rain blobs. The synthetic diagnostics provide clear, multi-wavelength signatures that can guide future high-resolution observations, and highlight the importance of small-scale reconnection-driven processes in shaping the multi-thermal structure (between MK to kK) of the solar corona.
ER -