Coronal polar plumes

摘要: The purpose of this investigation was to determine what connection exists between coronal plumes and polar surface features. To end the properties were re-examined by making a detailed statistical analysis photographs three eclipses (1962, 1963, 1965) last sunspot minimum. It is found that ‘typical’ plume has core density ≈ 108 cm−3, half width 3.3 × 104km, profile with distance r from its axis characterized $$N \approx {\text{10}}^{\text{8}} \left( {1 - \frac{r}{{3.9 \times 10^4 }}} \right)^{1.6} $$ There some (although only weak) regularity in projected spacing mean separation 7 104 km. relation various features examined. Although little direct evidence can be assembled, we conclude photospheric faculae, bright K3 small-scale magnetic structure present chromospheric network. hypothesized originate at cores rosettes which lie along distribution field corona above covered idealized network cells calculated. fact shape size flux tubes originating rosette agrees observed supports hypothesis.