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- W1615692450 abstract "A coronal hole is a region of the solar corona characterised by diverging magnetic fields of single polarity and lower-than-average densities (and probably temperatures). It is now generally accepted that coronal holes are the source of high-speed streams in the solar wind (Munro and Withbroe 1972, Kopp and Holzer 1976, Steinolfson and Tandberg-Hanssen 1977, Munro and Jackson 1977; see Pneuman 1980 for references to most of the theoretical and observational papers on coronal holes since their recognition in 1968). We consider an infinitesimal field-aligned flow tube with cross-sectional area A(r) where r is the heliocentric radius (Figure 1), and we adopt the functional form A ( r )/ A ( r ) = ( r / r 0 ) 8 where r is the coronal base radius, and 5 is a parameter which measures the divergence of the flow. If s = 2 then the flow is purely spherically symmetric, while if s > 2 the flow is more strongly divergent as is expected to be the case for a coronal hole. The cross-section of a typical coronal hole is shown schematically in Figure 2." @default.
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- W1615692450 date "1982-01-01" @default.
- W1615692450 modified "2023-09-23" @default.
- W1615692450 title "A Simple Model of a Coronal Hole" @default.
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- W1615692450 doi "https://doi.org/10.1017/s1323358000021202" @default.
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