Electromagnetic wave radiation
Electromagnetic wave radiationEdit
Electromagnetic wave radiation are quantized as a packet of photon's energy
Quanta ; h ; sometime behaves like a wave of wavelength λ and somtime behave like a particle of a momentum p
- Wave like .
- Particle like .
Electromagnetic wave radiation statesEdit
Electromagnetic wave radiations exist in the form of quantum's energy called photon . Electromagnetic photons are found in 2 states Radiant photon at threshold frequency and Non radiant photon at frequency above threshold frequency .
- Radiant photon .
- Non-radiant photon .
Electromagnetic photon cannot exit in 2 states at the same time . The chance of finding Electromagnetic photons in any state is one half can be expressed mathematically as
Electromagnetic radiation spectrumEdit
The wavefront of electromagnetic waves emitted from a point source (such as a lightbulb) is a sphere. The position of an electromagnetic wave within the electromagnetic spectrum could be characterized by either its frequency of oscillation or its wavelength
Frequency spectrum Speed Work Quanta Momentum Wavelength
The Electromagnetic spectrum includes, in order of increasing frequency and decreasing wavelength
Electromagnetic wave radiation and MatterEdit
Heat transfer Heat conduction Heat convection Heat radiation Heat effects Change matter's temperature
Matter absorbs heat energy
matter absorbs heat energy to its maximum
at threshold frequency
matter uses energy above maximum energy to free electron from atom
With f > fo and hf=(n+1)hfo
Electromagnetic wave radiation typesEdit
Plank knew that black body absorbs heat better than any other matter . He went go perform an experience on black matter . His experienment has shown that
Planck's law of black-body radiationEdit
Planck's law states that
- Bν(T) is the spectral radiance (the power per unit solid angle and per unit of area normal to the propagation) density of frequency ν radiation per unit frequency at thermal equilibrium at temperature T.
- h is the Planck constant;
- c is the speed of light in a vacuum;
- k is the Boltzmann constant;
- ν is the frequency of the electromagnetic radiation;
- T is the absolute temperature of the body.
For a black body surface the spectral radiance density (defined per unit of area normal to the propagation) is independent of the angle of emission with respect to the normal. However, this means that, following Lambert's cosine law, is the radiance density per unit area of emitting surface as the surface area involved in generating the radiance is increased by a factor with respect to an area normal to the propagation direction. At oblique angles, the solid angle spans involved do get smaller, resulting in lower aggregate intensities.
Wien's displacement lawEdit
Wien's displacement law shows how the spectrum of black-body radiation at any temperature is related to the spectrum at any other temperature. If we know the shape of the spectrum at one temperature, we can calculate the shape at any other temperature. Spectral intensity can be expressed as a function of wavelength or of frequency.
A consequence of Wien's displacement law is that the wavelength at which the intensity per unit wavelength of the radiation produced by a black body is at a maximum, , is a function only of the temperature:
where the constant b, known as Wien's displacement constant, is equal to 2.8977729(17)×10−3
Planck's law was also stated above as a function of frequency. The intensity maximum for this is given by
By integrating over the frequency the integrated radiance is
by using with and with being the Stefan–Boltzmann constant. The radiance is then
per unit of emitting surface.
On a side note, at a distance d, the intensity per area of radiating surface is the useful expression
when the receiving surface is perpendicular to the radiation.
By subsequently integrating over the solid angle (where ) the Stefan–Boltzmann law is calculated, stating that the power j* emitted per unit area of the surface of a black body is directly proportional to the fourth power of its absolute temperature:
Sun's Light DecompositionEdit
When visible light interacts with prism, visible light will decompose itself into color lights of six color Red, Orange, Yellow, Violet, Blue and Green
Color Angle of diffraction Wavelength Red Orange Yellow Violet Blue Green