activity
20082025
most citedHigh-resolution observations of flare precursors in the low solar atmosphere

112 citations · 1.3k across the 55 of their papers we have counts for

collaborators
Showing 2017Show all

6 papers · 1 filter

astro-ph.SR2017★ 24 cited

Extending Counter-Streaming Motion from an Active Region Filament to Sunspot Light Bridge

Haimin Wang, Rui Liu, Qin Li +6

We analyze the high-resolution observations from the 1.6m telescope at Big Bear Solar Observatory that cover an active region filament. Counter-streaming motions are clearly observ…

astro-ph.SR2017★ 112 cited

High-resolution observations of flare precursors in the low solar atmosphere

Haimin Wang, Chang Liu, Kwangsu Ahn +9

Solar flares are generally believed to be powered by free magnetic energy stored in the corona, but the build up of coronal energy alone may be insufficient for the imminent flare…

astro-ph.SR2017★ 29 cited

Multi-wavelength Spectral Analysis of Ellerman Bombs Observed by FISS and IRIS

Jie Hong, M. D. Ding, Wenda Cao

Ellerman bombs (EBs) are a kind of solar activities that is suggested to occur in the lower atmosphere. Recent observations using the Interface Region Imaging Spectrograph (IRIS) s…

astro-ph.IM2017

Objective Image Quality Assessment for High Resolution Photospheric Images by Median Filter Gradient Similarity

Hui Deng, Dandan Zhang, Tianyu Wang +6

All next generation ground-based and space-based solar telescopes require a good quality assessment metric in order to evaluate their imaging performance. In this paper, a new imag…

astro-ph.SR2017★ 29 cited

Material supply and magnetic configuration of an active region filament

P. Zou, C. Fang, P. F. Chen +3

It is important to study the fine structures of solar filaments with high-resolution observations since it can help us understand the magnetic and thermal structures of the filamen…

astro-ph.SR2017★ 16 cited

Magnetic separatrix as the source region of the plasma supply for an active-region filament

P. Zou, C. Fang, P. F. Chen +2

Solar filaments can be formed via chromospheric evaporation followed by condensation in the corona or by the direct injection of cool plasma from the chromosphere to the corona. In…