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Cited article:

Three Types of Solar Coronal Rain during Magnetic Reconnection between Open and Closed Magnetic Structures

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Morphological evidence for nanoflares heating warm loops in the solar corona

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Heating of Quiescent Coronal Loops Caused by Nearby Eruptions Observed with the Solar Dynamics Observatory and the Solar Upper Transition Region Imager

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Temperature Analysis of Flaring (AR 11283) and Non-flaring (AR 12194) Coronal Loops

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A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona

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Direct Measurement of AIA 171 Coronal Loop Transparency

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On-disk Solar Coronal Condensations Facilitated by Magnetic Reconnection between Open and Closed Magnetic Structures

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Magnetic Reconnection between Loops Accelerated By a Nearby Filament Eruption

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Revisiting the formation mechanism for coronal rain from previous studies

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Formation of a Solar Filament by Magnetic Reconnection and Coronal Condensation

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The Astrophysical Journal Letters 919 (2) L21 (2021)
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Relation of Coronal Rain Originating from Coronal Condensations to Interchange Magnetic Reconnection

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The Astrophysical Journal 905 (1) 26 (2020)
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Manifestations of Three-dimensional Magnetic Reconnection in an Eruption of a Quiescent Filament: Filament Strands Turning to Flare Loops

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Signatures of the non-Maxwellian κ-distributions in optically thin line spectra

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Astronomy & Astrophysics 626 A88 (2019)
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