Luminous Intensity

The intensity emitted by the surface area of one cm² or one m² of the light source is known as Luminance (L). Mathematically it can be written as;
L=I/S
Where;
I = Luminous intensity
S =Area of the source surface
Luminance can be expressed as cd/m² or cd/cm² or lm/cm² or Lambert. The value of luminance indicates glare and discomfort to see a lighting source. For example the luminance value for sun is very high or very less for a small lamp. I like to share this de broglie wavelength problems with you all through my article.

The quantity of the energy of the light emitted per second in all directions is known as Luminous flux which can be expressed as lumen (lm). The ability to emit light into a given direction is known as Luminous Intensity. In other words; this intensity can be defined as the luminous flux which is radiated by the light source in a given direction within the unit of the spatial angel and can be expressed as candela.
I=Ø/ß
Where;
Ø = Luminous flux
ß= Small spatial angel
I = Luminous intensity
Let’s define Luminosity. The Definition of Luminosity states that it is the criteria that how much energy is coming from the object in one second. It is expressed in watts (W). Generally astronomers use another term for measurement that is known as absolute magnitude which is based on a ratio scale.
The value of luminosity for the Sun is 3.9 x 1026 W while for starts, it is around5.2 x Lsun, therefore the star has 5.2 times more energy output per second of the Sun.
The intensity of the starlight is called as apparent brightness or the flux of light. It is measured in watts per square meter (W/m2).
The Luminosity Equation for star can be written as;
L = (4?d2) b

Where;
L = luminosity of the star
d = distance to the star
b= brightness of the star
The Luminosity Distance can calculate by using given equation;
b= L/ 4?d2
Or d2 = L/ 4?b
Or d= vL/4?b

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Fundamentally the ‘L’ value for a body or object like for star depends upon two factors; the effective temperature, Teff and the size or radius (R) of the star. The temperature of a black body depends upon the radiations emitted by it. As the temperature increases; the rate of radiates power output per unit surface area also increase. You can observe this in the filament of light bulb; as it gets hotter it gets brighter and emits more energy. The relation between the power radiated by a black body per unit surface area and effective temperature, Teff is as given below;
l ? T4    or l = sT4
Where s is a constant known as Stefan-Boltzmann constant and its value is 5.67 × 10-8 W m-2 K-4.