Dynamics of solar coronal loops I. Condensation in cool loops and its effect on transition region lines

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Coronal Loops: Observations and Modeling of Confined Plasma (2010, background): “These equations can be solved numerically and several specific codes have been used extensively to investigate the physics of coronal loops and of X-ray flares (e.g., Nagai, 1980; Peres et al., 1982; Doschek et al., 1982; Nagai and Emslie, 1984; Fisher et al., 1985a,b,c; MacNeice, 1986; Gan et al., ”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “Red field lines are too short; the helical black field line can host only a condensation sitting at the bottom of the dip; and green field lines are capable of hosting small, intermittent, short-lived condensations known as coronal rain (Müller et al., 2003, 2005).”