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什么是回热加热效应的计算公式在温室气体辐射吗?

温室气体吸收热量和辐射的能力有些回到原来的热源看起来像一个有用的热性能可能纳入双层玻璃、墙绝缘,等等有什么公式。这将使我们计算这个额外的热效应的正常传导热量损失参数,热容,U值等等?我们还想找到细节的原始实验被用来证实说公式的准确性与互联网搜索所有我能找到的都知道用塑料瓶和学校类型实验证明原则但不充分的加热灯,定量准确。我们问了一个类似的问题在物理栈交流我们认为一个问题涉及气体的基本物理性质(热)江南电子竞技平台,但有小的反应。

回答

你已经提到过,有一些物理现象负责热量和能量转移。我会重新列表的完整性、虽然你已经解决了你的问题。1。办理2。对流3。汽化潜热4。辐射到你的问题:辐射是能量的传输通过电磁波的身体发出absoulte温度uneqal绝对零度。这是什么意思?辐射并不依赖于接触或运输液体传导和对流。相反,它相当于其绝对温度的四次方。 This is what we know as "Black Body Radiation". The equation for this is: $$ E = \sigma * T^4$$ where σ is the [Stefan-Boltzman Constant][1] and T is the absolute Temperature in Kelvin. This law is obtained by integrating Planck's law over the solid angle and wavelength, in order to determinate the energy which is transmitted not only by one particular wavelength, but the whole spectrum and in all directions. Combined with [Kirchhoffs Law][2], which says, that the absorbtivity of an object equals its emissivity, you can calculate the radiated Energy of any object or atmospheric layer. The emissivity (ε) of a body is a value between zero and one with one being the perfect black body. For most things you can find values in the [web][3]. It also explains why aluminum foil is such a good insulator. $$ E = ε * \sigma * T^4$$ To put all of this in an example: Everything around you radiates heat. Beginning with the most obvious, the sun. The sun's surface has an approximate temperature of 6000K. This means it emits radiation of the following spectrum: [![https://upload.wikimedia.org/wikipedia/commons/e/e7/Solar_spectrum_en.svg][4]][4] As you can see, the maximum of the energy of the sun is radiated in the part which we know as visible light. Also a big part of the radiated energy is absorbed in the atmosphere (the difference between yellow and red graphs). Responsible for these are particularly Ozone (O3), Water (H2O) and (CO2) which are also our most important greenhouse gases. What happens, is that the radiated energy of a particular wavelength "hits" the molecules and excites them into a state of higher kinetic energy. The average random kinetic energy of a substance is what we know as the temperature of this substance. Hence, also the atmosphere acts like a black body and radiates energy back to space but also back to earth. Unfortunately I can't really say much about the second part of your question. I don't know about the original experiments. But I suggest a read about Gustav Kirchhoff, who introduced the idea in 1860 which then has been proceeded by Josef Stefan in 1879 and Ludwig Boltzman (1884). Also Planck's works from 1900 could be helpful. I hope I was able to point you in the right direction with your studies. [1]: https://en.wikipedia.org/wiki/Stefan%E2%80%93Boltzmann_constant [2]: https://en.wikipedia.org/wiki/Kirchhoff%27s_law_of_thermal_radiation [3]: https://en.wikipedia.org/wiki/Emissivity [4]: https://i.stack.imgur.com/QT9ok.png

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