Abstract
Extreme ultraviolet observations of a quiet region of the Sun on August 18, 1969, with the Harvard spectroheliometer on OSO 6 indicate that the chromospheric network can be observed in lines of the chromosphere and transition region (T = 8.4 × 105 K) with almost identical structure. At coronal heights, the network changes but some residual structure can still be discerned in Mgx and perhaps Sixii (T = 2.3 × 106 K), although there is little or no evidence remaining in Fexvi (T = = 3.5 × 106 K).
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References
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Reeves, E.M., Parkinson, W.H. EUV observations of the chromospheric network. Sol Phys 24, 113–117 (1972). https://doi.org/10.1007/BF00231087
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DOI: https://doi.org/10.1007/BF00231087