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Omega: Jurnal Fisika dan Pendidikan Fisika5(1), 23 - 26 (2019) (Journal of Physics and Physics Education)
Simulation of Radiation Calculation of Black Body by Using the Interpolation Method
Feli Cianda Adrin Burhendi1,∗, Rizky Dwi Siswanto2, Wahyu Dian Laksanawati1
1Physics Education Study Programme, Universitas Muhammadiyah Prof. DR. HAMKA Jl. Tanah Merdeka, Pasar Rebo, Jakarta 13830, Indonesia
2Mathematics Education Study Programme, Universitas Muhammadiyah Prof. DR. HAMKA Jl. Tanah Merdeka, Pasar Rebo, Jakarta 13830, Indonesia
(Received 15 Februari 2019; published 6 July 2019)
Abstract
Simulation of radiation calculation of black body by using the interpolation method is designed to facilitate the determination of radiation in black matter efficiency. Fortran programming languages are chosen for computa- tional processes. The calculation program that has been designed is able to calculate the efficiency of black body radiation easily and quickly with a fairly small error rate of 0.5%. The light radiation spectrum of objects is around 1000, 1100, 1200, and 1300◦C. Thexaxis shows the wavelength, while the yaxis shows the intensity or strength of light. If we pay attention to the curvature of 1000◦C, along with the increasing frequency of light, the intensity of light is also getting stronger aka more bright. But at certain light frequencies, the line reaches the peak, and after that the light intensity drops dramatically. At temperatures of 1200◦C and 1300 ◦C, even though the temperature rises, the outline of the line graph is similar to the line 1000◦C. This is in accordance with the existing theoretical and experimental results.
c
2019 The Authors. Published by Pendidikan Fisika UHAMKA
Keywords: black body radiation, interpolation method, efficiency
DOI:10.31758/OmegaJPhysPhysEduc.v5i1.23
∗Corresponding author. E-mail address: [email protected]
Introduction
In Physics, black body is objects absorbs all light falling him, no light that went or reflected.
The term black body was first introduced by gus- tav kirchoff in 1862. Light emitted by objects black called black body radiation. If objects is heated at high temperature emitting light waves looked in lenght, like metal, incandescence long time later there will candescant, and brings forth light [1].
Knowledge of the laws governing thermal radi- ation of bodies enables understanding and descrip- tion of large number of phenomena in nature, and
operation principles for a wide range of devices used in everyday life and scientific applications. As ex- amples, it is worth mentioning cosmologic research, the greenhouse effect, heat transfer processes used in harvesting of energy from renewable resources, such as solar collectors or solar ponds, cooling of electronic systems, measurement of thermal prop- erties of bodies, motion detectors used in alert and protection systems or thermal vision cameras [2].
In line with that, the conclusion of the math- ematical model of the law of perfect black matter radiation made by Max Planck at the beginning of the 20th century was based on ideas and ideas,
Feli Cianda Adrin Burhendiet al. / Omega: Jurnal Fisika dan Pendidikan Fisika5(1), 23 - 26 (2019)
which were considered contrary to the laws of clas- sical physics [3].
Here we will take a closer look at the Maxwell field and then in particular its properties at finite temperature in the form of black-body radiation. It is characterized by a pressure p and an energy den- sityρ. In a spacetime with three spatial dimensions, these are related byρ=ρ/3. This can be derived by purely kinematic arguments which are used in the following section to find the corresponding relation in a D-dimensional Minkowski spacetime. When the radiation is in thermal equilibrium at tempera- tureT, we then get by thermodynamic arguments the generalization of the Stefan-Boltzmann law in the formρ∝TD [4].
The generalized statistical mechanics has suc- cessfully been applied to investigate physical sys- tems which exhibit nonextensive features like stel- lar polytrops, Levy-like anomalous diffusions, two dimensional turbulence, cosmic background radi- ation, solar neutrino problem and many others.
Within the framework of the nonextensive statisti- cal mechanics, we have generalized the Planck’s law for the black-body radiation. Earlier, an attempt was made to generalize the Planck’s radiation law (known as the asymptotic approach) [5] for the ex- planation of the cosmic microwave background ra- diation [6] at a temperature of 2.725 K. Another attempt was made to generalize statistics of quan- tum and classical gases using the factorization ap- proach [7]. There are some versions of generalized Planck’s law available in the existing literature[8] in this regard. There are also recent attempts to gen- eralize the Planck’s radiation law using Kaniadakis approach [9,10].
The total radiant intensity of all wavelengths is directly proportional to the temperature of a four- levelT, so it can be written
Z ∞
0
Rdλ=σT4 (1) This equation is called the Stefan law and σis known as the Stefan-Bolzman constant, theσcon- stant value is equal to
σ= 5.6703×10−8 W
m2K4 (2) The wavelength where each curve reaches its maximum value, which is called λmaks (although it is not a maximum wavelength), decreases if the transmitter temperature is increased, it is propor- tional to the increase in temperature, soλmaks∝1T is found
λmaksT = 2.898×10−3mK (3) This result is known as the Wien shift law.
Classic calculations for radiant energy emitted for each wavelength now are divided into several cal- culation stages. Without the proof being presented, the following points out the important parts of the decline. First, the calculation of the amount of ra- diation for each wavelength, then the contribution of each wave to the total energy in the box, and finally the intensity of radians associated with that energy. The box contains electromagnetic standing waves. If all the walls of a box are metal, then the radiation is reflected back and forth with the nodes (electric nodes) found on each wall (the electric field must be zero in a conductor).
The number of standing waves with a wave- length between λandλ+ dλis
N(λ) dλ= 8πv
λ4 dλ (4)
V is the volume of the box. For a one-dimensional standing wave, such as in a tension rope along L, the permissible wavelength is fE= 2L/n,´ (n = 1,2,3, ...). The number of possible standing waves with a wavelength betweenfE1 and´ fE2 is so that´ in the interval betweenfE and´ fE + df´ E there will´ be as many different waves.
Each wave gives a share ofkT energy to radia- tion in the box. This result is obtained from clas- sical thermodynamics. Radiation in the box is in a state of thermal equilibrium with the wall at tem- peratureT. This radiation is reflected by the wall of the box because it is absorbed by the wall and then emitted immediately by wall atoms, which in this process vibrate at the radiation frequency. To ob- tain radiant intensity from energy density (energy per unit volume) multiply by c/4. These results were also obtained from the theory of electromag- nets and classical thermodynamics.
By combining the elements above, the estimated radiant intensity is
R(λ) =8π λ4kTc
4 (5)
This is known as the Rayleigh-Jeans formula.
The decline uses classical electromagnetic theory and thermodynamics, which is a maximum effort in applying classical physics to understand the prob- lem of black matter radiation.
In Planck’s theory, each oscillator can emit or absorb energy only in quantities that are multiples of integers of a basic energy
E=nε, n= 1,2,3, ... (6) ndenotes the number of quanta. Furthermore, the energy of each quanta is determined by frequency according to
ε=hν (7)
24
Feli Cianda Adrin Burhendiet al. / Omega: Jurnal Fisika dan Pendidikan Fisika5(1), 23 - 26 (2019)
his an appeal constant known as the Planck con- stant. Based on this assumption, the spectrum of radiant intensity Planck calculates is
R(λ) =c 4
8π λ4
"hc λ
1 eλkThc−1
# (8)
Methods
The are many methods that able us to measure more or less accurately Planck’s constant. The most useful, for a college or high school physics labora- tory, are based on aplication of the photoelectric ef- fect or black body radiation. Those are not the most accurate, but are the easiest to implement under the above-mentioned conditions. The first method relies upon Einstein formula describing the energy of electrons emitted from an illuminated surface for different frequencies of incoming photons. This method is quite often used in introductory laborato- ries. The second method seems more interestingas its implementation requires more knowledge about basic of quantum and statistical physics [11]. While implementing the method of interpolation.
Interpolation calculations were carried out to obtain theoretical results, then computation was carried out with the fortran95 program to obtain experimental data.
Results
The graph of the black body radiation spectrum can be seen in Figure 1. The bottom curved line is the spectrum of light radiation from objects at around 1000◦C. Thexaxis shows the wavelength, while the y axis shows the intensity or strength of light. If we pay attention to the curvature of 1000
◦C, along with the increasing frequency of light, the intensity of light is also getting stronger aka more bright. But at certain light frequencies, the line reaches the peak, and after that the light intensity drops dramatically. At temperatures of 1200 ◦C and 1300◦C, even though the temperature rises, the outline of the line graph is similar to the line 1000
◦C. Only the difference, the peak point is higher and slightly shifted to the right (to a greater frequency of light). We can also see that the frequency of light at the highest intensity is directly proportional to the temperature of the object.
Figure 1: Graph of the black body radiation spectrum
Conclusion
The use of the interpolation method for calcu- lating the efficiency of black body radiation can be used because it is in accordance with practical data or experiments that have been carried out by Wien and Max Planck. So this facilitates accurate data retrieval and forecasting data for different energy levels.
References
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[3] M. A. Ramirez-Moreno, S. Gonzalez-Hernandez, and G. A. De Parga, A semiclassical approach to the matte black-body, Eur. J. Phys.36(6), 65039 (2015).
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[9] K. Ourabah and M. Tribeche, Planck radiation law and Einstein coefficients reexamined in Kaniadakis κstatistics, Phys. Rev. E89, 062130 (2014).
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[10] I. Lourek and M. Tribeche, Thermodynamic prop- erties of the blackbody radiation: a Kaniadakis ap- proach, Phys. Lett. A381(5), 452-456 (2017).
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