Astrophysics (index)

Surface Temperature

(temperature of the surface of a star or planet)

The term Surface Temperature is used in astronomy for stars an planets.

In the case of stars, the Effective Temperature (Teff) is generally used/quoted as the surface Temperature. In fact, where the surface of a star is located is unclear as the star is Plasma and beyond the star is more plasma, so the Surface is generally what appears to be the "outside" of the star, that part which produces the light we see, which is the Photosphere. As opposed to the center or deeper regions of the star, this is the part whose temperature determines the spectrum and therefore color of the star. The photosphere has a finite depth and the emerging light comes from a range of depths at a range of temperatures. The effective temperature is a relatively easy-to-determine quantity used to estimate the general area of this temperature range. Spectral Lines, whose form and magnitude are depend on temperature, can be used to determine more accurately the photosphere's temperature at different depths.

For planets, the surface temperature is more defined, especially for Rocky Planets. The reflection of Electromagnetic Radiation (EMR) means the observed spectrum does not reflect surface temperature, so other means are required, including determining the Black Body (BB) contribution of the spectrum, and investigating the temperature of the Atmosphere through analysis of spectral lines.


(stars,planets,temperature)
http://en.wikipedia.org/wiki/Photosphere

Referenced by:
A-Type Star (A)
B-Type Star (B)
F-Type Star (F)
G-Type Star (G)
HITEMP
K-Type Star (K)
L-Type Star (L)
M-Type Star (M)
O5 Spectral Class (O5)
O-Type Star (O)
Red Dwarf
Red Giant
Spectral Class
Stellar Temperature Determination
T-Type Star (T)
Y-Type Star (Y)

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