Abstract
A new spectroscopic method of deriving the three-dimensional information (‘escalation’) worked out at the Pulkovo Observatory was applied to observations of solar faculae. The size of the investigated area was 70″ × 18″. Two series of spectra were obtained simultaneously in four spectral regions (Hα, D1,2, (Nai), Hβ, and H, K (Caii)) with a quadruple-camera spectrograph attached to the second horizontal solar telescope at Pulkovo on 13 August, 1968.
It was found from the analysis of the maps of brightness distribution in the cores of the lines and continuum that the facular emission lies in ropes which incline to the solar surface.
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Stoyanova, M.N. Vertical structure of plages. Sol Phys 15, 349–355 (1970). https://doi.org/10.1007/BF00151840
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DOI: https://doi.org/10.1007/BF00151840