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luminous, apparently opaque layer of gases that forms the visible surface of the sunsun,
intensely hot, self-luminous body of gases at the center of the solar system. Its gravitational attraction maintains the planets, comets, and other bodies of the solar system in their orbits.
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 or any other star. The photosphere lies between the dense interior gases and the more attenuated gases of the chromospherechromosphere
[Gr.,=color sphere], layer of rarefied, transparent gases in the solar atmosphere; it measures 6,000 mi (9,700 km) in thickness and lies between the photosphere (the sun's visible surface) and the corona (its outer atmosphere).
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. The incandescent gases of the photosphere, estimated to be at temperatures near 6,000°K;, are so much brighter than the other layers of the sun that they seem to form a surface. These gases are in a constant state of agitation due to convection currents that reach down to 150,000 mi (241,000 km) below the photosphere. Differences in the density of the gases result in a grainy appearance of the photosphere; the small bright patches, or granules, are several hundred miles in diameter and are constantly shifting. Another feature of the photosphere, observed only near the sun's edge, is the appearance near sunspots of bright, veinlike regions known as faculae.


(foh-tŏ-sfeer) The ‘visible’ surface of the Sun and source of the absorption spectrum that is characteristic of most stars. The photosphere of a star is considerably more dense than the atmospheric layers that lie above it, i.e. the chromosphere and corona.

The solar photosphere is a stratum several hundred kilometers thick, from which almost all the energy emitted by the Sun is radiated into space. Within the photosphere the temperature falls from about 6000 K just above the convective zone to about 4000 K at the temperature minimum, where the photosphere merges with the chromosphere.

The intensity of the solar photosphere, which decreases at visible wavelengths from the center to the limb of the disk (see limb darkening), is due to the radiation emitted, principally by negative hydrogen ions (H), at depths of up to a few hundred kilometers. At higher levels, where the density of H ions is too low for appreciable opacity, the lower temperature gives rise to the absorption of radiation at discrete wavelengths. The Fraunhofer lines of the resulting absorption spectrum have provided the key to determining the chemical composition of the photosphere, because a direct comparison can be made with the laboratory spectra of known elements under various conditions.

Regions of the solar photosphere (and lower chromosphere) several thousand kilometers in diameter rhythmically rise and fall with a period of about 5 minutes over a time span of less than half an hour, attaining a maximum velocity of about 0.5 km s–1. These vertical oscillations are thought to be produced by the outward propagation of low-frequency sound waves, generated by turbulence in the convective zone. The internal vibrations of the Sun, the subject area of helioseismology, can reveal information on the solar interior.

See also faculae; granulation; supergranulation; sunspots.



the deepest and densest layer of a stellar atmosphere, including the solar atmosphere, from which most of the stellar radiant energy escapes.

A large part of the continuous spectrum of stars, chiefly the visible spectrum, and most of the Fraunhofer absorption lines arise in the photosphere. The photosphere is generally in radiative equilibrium. It is easier for radiation to escape from the higher layers of a stellar atmosphere, and consequently the temperature of the star decreases as the outer layers are approached. On the average, the temperature is close to the effective temperature of the star. The size of the photosphere of the main-sequence stars (on the Hertzsprung-Russell diagram) relative to the radius of the stars is 10–4–10–3, of white dwarfs of the order of 10–6, and of giants and supergiants 10–3–10–2. The average gas densities of the photospheres of various stars vary from 10–9 g/cm3 for hot stars of the main sequence to 10–6 g/cm3 for white dwarfs.

The photosphere of the sun, which coincides with its apparent surface, has been studied in greatest detail. It is 200–300 km thick, and its temperature ranges from 4500° to 8000°K; the pressure of the gas varies from 10–5 to 10–3 dyne/cm2. The photosphere is the only region of the sun with relatively weak ionization of the sun’s predominant chemical element—hydrogen—the degree of ionization of which is about 10–4. In stars similar to the sun, the strong opacity of the photospheric gases is due to a small impurity of negative hydrogen ions.

By using a photosphere telescope it is possible to observe the fine structure of the solar photosphere—granulation—consisting of small round (about 1,000 km in diameter) bright granules that are separated by dark intergranular regions.



The intensely bright portion of the sun visible to the unaided eye; it is a shell a few hundred miles in thickness marking the boundary between the dense interior gases of the sun and the more diffuse cooler gases in the outer portions of the sun.
References in periodicals archive ?
Such models try to reproduce the churning and flowing of gases in the sun's photosphere.
In related news Photosphere has begun offering discounts for its newsletter subscribers and has also recently redesigned the web site.
A level of interest did, however, develop regarding the Sun's photosphere and plasma properties of the solar corona.
The sun's visible surface, called the photosphere, is some 6,000 Kelvins, while the corona regularly reaches temperatures which are 300 times as hot.
Long before the flare the magnetic field lines are un-entangled and they appear in a smooth arc between two points on the photosphere (the Sun's visible surface) -- areas called field line footpoints.
This interface region between the sun's photosphere and corona powers its dynamic million-degree atmosphere and drives the solar wind.
The interface region lies between the sun's 6,000-degree, white-hot, visible surface, the photosphere, and the much hotter multi-million-degree upper corona.
Magnetic fields from the photosphere to the corona; proceedings.
On Oct 15 the photosphere around the group appeared darker than the rest of the disk.
Photosphere [Ward 2002] runs on MacOS and is a free system with which any camera and lens can be used, although it requires some equipment calibration procedures.
Each multiple exposure sequence is fused into an HDR image using software called Photosphere (Ward, 2005).