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The directly visible outer layer or atmosphere of a star, especially of the sun.

pho′to·spher′ic (-sfîr′ĭk, -sfĕr′ĭk) adj.
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Young also believed that the polarization was due to the scattering of photospheric light by small particles.
His topics include radiative transfer in the sun's atmosphere, the dynamics of solar plasmas, observations of photospheric activity and magnetism, the solar wind and heliosphere, and influences of solar variability on Earth.
The study of the photospheric stellar abundances of the planet-host stars is the key to understanding how protoplanets form, as well as which protoplanetary clouds evolve planets and which do not.
7 times brighter than the normal photospheric background at visible wavelengths and although the mean time for existence is 15 minutes, they can last for up to two hours.
Asplund's team published estimates of solar photospheric oxygen abundance that were 30 to 40 percent lower than commonly accepted values, with similar changes for carbon, nitrogen and neon.
In introducing 54 papers that presented a sample of its first results and related theoretical models at the 2007 ASP conference, Matthews (UCL Mullard Space Science Laboratory, Surrey, UK) and coauthors from NASA and the National Astronomical Observatory of Japan explain Hinode's mission to provide information on how solar magnetic fields are formed, evolve, and interact with plasmas to create the photospheric and chromospheric phenomena observed.
Near disk center, the Coronal Cells looked like photospheric granules with bright centers and dark, narrow intercellular lanes.
In the case of magnetic bright points, it is the 'floor' which is viewed as bright, as light is said to originate from "deeper photospheric layers that are usually hotter" [138].
The smallest scale photospheric magnetic field seems to come in isolated points in the dark intergranular lanes, rather than the predicted continuous sheets confined to the lanes," said Goode.
Eighty contributions are organized into sections on photospheric magnetism, radiative transfer methods and inversion techniques, new solar polarimeters and techniques, atomic spectro- polarimetry, theory of collisional polarization, laboratory experiments and molecular spectro-polarimetry, stellar spectro- polarimetry, and chromospheric electromagnetism.
Thomas states, "Computer simulations of photospheric magnetoconvection show very small structures, but the simulations have not yet achieved sufficient resolution to determine the limiting size.
CaX), which is the highest ionization stage of a chemical element ever discovered in a photospheric stellar spectrum.