Thin Threads of Solar Filaments

By Yong Lin, O. Engvold, L. R. V. Voort, J. E. Wiik, T. Berger. 2005

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QUIESCENT PROMINENCE DYNAMICS OBSERVED WITH THE HINODE SOLAR OPTICAL TELESCOPE. I. TURBULENT UPFLOW PLUMES (2010, background): “But while on-disk observations (e.g., Lin et al. 2007; Lin et al. 2005; Zirker et al. 1998) invariably show filaments to be composed of short horizontal threads in support of the magnetostatic models, limb observations of prominences, as noted above, usually show vertically structured “hedgerow”…”
Hinode SOT Observations of Solar Quiescent Prominence Dynamics (2008, background): “Observations of filaments on the disk show that they are indeed resolvable into thin horizontal threads, often with measurable motions along the threads and up- or downflows in the footpoint regions (Kubota & Uesegi 1986; Zirker et al. 1998; Lin et al. 2005).”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “The threads are found to have widths of about 200 km (Lin et al., 2005a,b, 2008a,b) and are not necessary aligned with the structural component of the filament to which they belong.”
Physics of Solar Prominences: I—Spectral Diagnostics and Non-LTE Modelling (2010, background): “Later studies by Lin et al. (2003, 2005) and Schmieder et al. (2008) found counterstreaming in threads in Hα with average transverse velocities in the range 7−15 km s−1 and speeds in one instance as high as 30 km s−1.”