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Team:Tokyo Tech/Ibuki test
From 2009.igem.org
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Revision as of 13:24, 19 October 2009
- アルベドと温度の関係について
According to Stefan-Boltzmann law, blackbody emit per surface in unit time is calculated as
σT4,
where T is the temperature of the black body and <math>\sigma=5.67*10^{-8} (W/m^2K^4)</math> is constant value. The total energy that comes from the sun is calculated as
S(1 − A)πr2,
where <math>S=597 (W/m^2)</math>is the energy which actually reaches the mars from the sun, A is the albedo of the Mars and <math>r=3.3972*10^6 (m)</math> is the radius of the Mars. Regarding the Mars as blackbody, the radiative equilibrium temperature of the Mars is estimated as
<math>T=\sqrt[4]{\frac{S(1-A)}{4\lambda}}</math>.
According to Yurij Shkuratov and Larissa Starukhina, albedo A can be calculated as
<math>A=\frac{1+\rho_b^2-\rho_f^2}{2\rho_b}-\sqrt{(\frac{1+\rho_b^2-\rho_f^2}{2\rho_b})^2-1}</math>,
where <math>\rho_b</math> and <math>\rho_f</math> are the one-dimensional indicatrix back and forward.
If we succeeded in decreasing the albedo by making the Mars black, the temperature will change as the graph shows. x axis is year and y axis is temperature.
If we could change the albedo from 0.15 to 0.05, the temperature of the Mars would increase by about 6 Celsius degree.
