Question

write short note on color index​

Answer 1

Answer:

Color depth or colour depth (see spelling differences), also known as bit depth, is either the number of bits used to indicate the color of a single pixel, in a bitmapped image or video framebuffer, or the number of bits used for each color component of a single pixel.

Explanation:

PLZ MARK ME AS A BRAINLIEST  

Answer 2

color index is a simple numerical expression that determines the color of an object, which in the case of a star gives its temperature. The smaller the color index, the more blue (or hotter) the object is. Conversely, the larger the color index, the more red (or cooler) the object is. This is a consequence of the logarithmic magnitude scale, in which brighter objects have smaller (more negative) magnitudes than dimmer ones. For comparison, the yellowish Sun has a B−V index of 0.656 ± 0.005,[2] whereas the bluish Rigel has a B−V of −0.03 (its B magnitude is 0.09 and its V magnitude is 0.12, B−V = −0.03).[3] Traditionally, the color index uses Vega as a zero point.

To measure the index, one observes the magnitude of an object successively through two different filters, such as U and B, or B and V, where U is sensitive to ultraviolet rays, B is sensitive to blue light, and V is sensitive to visible (green-yellow) light (see also: UBV system). The set of passbands or filters is called a photometric system. The difference in magnitudes found with these filters is called the U−B or B−V color index respectively.

In principle, the temperature of a star can be calculated directly from the B−V index, and there are several formulae to make this connection.[4] A good approximation can be obtained by considering stars as black bodies, using Ballesteros' formula[5] (also implemented in the PyAstronomy package for Python):[6]

T
=
4600
K
(
1
0.92
(
B
−
V
)
+
1.7
+
1
0.92
(
B
−
V
)
+
0.62
)
.
{\displaystyle T=4600\,\mathrm {K} \left({\frac {1}{0.92(B-V)+1.7}}+{\frac {1}{0.92(B-V)+0.62}}\right).}
Color indices of distant objects are usually affected by interstellar extinction, that is, they are redder than those of closer stars. The amount of reddening is characterized by color excess, defined as the difference between the observed color index and the normal color index (or intrinsic color index), the hypothetical true color index of the star, unaffected by extinction. For example, in the UBV photometric system we can write it for the B−V color:

E
B
−
V
=
(
B
−
V
)
observed
−
(
B
−
V
)
intrinsic
.
{\displaystyle E_{B-V}=(B-V)_{\text{observed}}-(B-V)_{\text{intrinsic}}.}