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heliophobia.
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A way to probe the density of the photosphere of the Sun is by using limb darkening. Limb darkening is the observation of the center part of a star appearing brighter than the edge or limb of the luminous disk.
In 1902, Frank Very demonstrated that limb darkening was a frequency dependent phenomenon [101] which he attributed to scattering in the solar atmosphere and reflection with carbon particles.
2) the limb darkening of the photosphere, 3) the directional spectral emissivity of sunspots, and 4) the directional spectral emissivity of granulations [28], the emissivity of faculae constitutes one of the most powerful lines of evidence that the Sun is condensed matter.
Details such as limb darkening and a slightly brighter polar region may be detectable in large scopes under good seeing.
The appearance of sunspots has fascinated mankind for centuries [1-8] and while limb darkening [9-11] has been documented from the days of Galileo [3, p.274], the phenomenon only became well-established in the 1800's [7, 12].
The Fermi bubbles appear uniformly bright across their surfaces and at their boundaries -- no limb darkening as we see on the Sun, but no edge brightening, either.
A further Jovian feature that plays a role is limb darkening, the gradual, uniform darkening toward the edge of the planet's disk caused by the absorption and scattering of sunlight by high-altitude hazes located above the main cloud layers.
A discussion of each physical feature follows: (1) the thermal spectrum, (2) limb darkening, (3) solar collapse, (4) the solar density, (5) seismic activity, (6) mass displacement, (7) the chromosphere and critical opalescence, (8) shape, (9) surface activity, (10) photospheric/coronal flows, (11) photospheric imaging, (12) the solar dynamo, and (13) the presence of Sun spots.
When the planet is near quadrature, one limb will have more pronounced limb darkening than the other.
Comas Sola never reported limb darkening on these four virtually airless bodies.