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| - | *アルベドと温度の関係について
| + | <html><img alt="Team photo" title="Team photo" width="200" height="200" border="0" src="https://static.igem.org/mediawiki/2009/8/89/Tokyotech.png" onmouseover="this.src='https://static.igem.org/mediawiki/2009/d/d9/Tokyo_Tech_1-2.jpg'" onmouseout="this.src='https://static.igem.org/mediawiki/2009/8/89/Tokyotech.png'"></html> |
| - | According to Stefan-Boltzmann law,
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| - | blackbody emit per surface in unit time is calculated as
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| - | <math>\sigma T^4</math>, | + | test<sup>[[#refrence|[1]]]</sup> |
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| - | where T is the temperature of the black body and <math>\sigma=5.67*10^{-8} (W/m^2K^4)</math> is constant value.
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| - | The total energy that comes from the sun is calculated as
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| - | <math>S(1-A)\pi r^2</math>, | + | <br> |
| - | | + | <br> |
| - | where <math>S=597 (W/m^2)</math>is the energy which actually reaches the mars from the sun,
| + | <br> |
| - | A is the albedo of the Mars and <math>r=3.3972*10^6 (m)</math> is the radius of the Mars.
| + | <br> |
| - | Regarding the Mars as blackbody, the radiative equilibrium temperature of the Mars is estimated as
| + | <br> |
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| - | <math>T=\sqrt[4]{\frac{S(1-A)}{4\lambda}}</math>. | + | <br> |
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| - | According to Yurij Shkuratov and Larissa Starukhina, albedo A can be calculated as
| + | <br> |
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| - | <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>, | + | ==refrence== |
| - | | + | *outside page[http://#] |
| - | where <math>\rho_b</math> and <math>\rho_f</math> are the one-dimensional indicatrix back and forward.
| + | <table bordercolor=#000 border="1" width=960px><tr><td></td><tr></table> |
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| - | If we succeeded in decreasing the albedo by making the Mars black,
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| - | the temperature will change as the graph shows.
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| - | x axis is year and y axis is temperature.
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| - | [[File:Temp.png|300px|thumb|temperature estimation]]
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| - | If we could change the albedo from 0.15 to 0.05, the temperature of the Mars would increase by about 6 Celsius degree.
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