Physics
Scientific paper
Aug 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...37..301g&link_type=abstract
Solar Physics, vol. 37, Aug. 1974, p. 301-307.
Physics
6
Chromosphere, H Alpha Line, Photosphere, Solar Granulation, Spectroheliographs, Doppler Effect, Solar Atmosphere, Stellar Structure, Wavelengths
Scientific paper
Photographs obtained in the core of H-alpha, free of parasitic continuum radiation, reveal a granular structure in supergranule centers wherever not obscured by mottles or fibrils. Granulation is seen well in the wings out to plus or minus 0.5 A from line center, the contrasts being largely reversed in opposite wings. The granule diameters (from boundary to boundary) are observed down to 800 km, and are typically 1200 km, both probably upper limits imposed by telescope resolution. At 0.25 A, the intensity fluctuates over a greater range (some 14%) in the blue wing than in the red (about 10%). The fluctuation is only 4% at line center. This smaller value represents a real variation at the local line center, whereas the appearance of granulation in the wings reflects to a large extent Doppler shifts due to vertical velocities. There is a tendency for the bright features at line center to be moving downwards. While of similar sizes, there is no direct superposition of chromospheric over photospheric granules.
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