$$T\left(x\right)=\ -\frac{\sigma}{2\lambda}x^2+C1x\ +C2$$

$$T\left(x\right)=\ \frac{\sigma}{2\lambda}x^2+C1x\ +C2$$

$$T\left(x\right)=\ -\frac{\sigma}{\lambda}x^2+C1x\ +C2$$

$$T\left(x\right)=\ -\frac{2\sigma}{\lambda}x^2+C1x\ +C2$$

0.00345

7

0.7

None of the above

Nu = 2 + Re^0.3Pr^0.4

Nu = 0.15Ra^1/3

Nu = 0.023Re^0.8Pr^1/3

Nu = 0.023Ra^0.8Pr^1/3

$$Gr\ =\ \frac{g\beta\left(Ts-Tair\right)Lc^3}{\upsilon^2}$$

$$Gr\ =\ \frac{g\beta\left(Ts-Tair\right)Lc^2}{\upsilon^2}$$

$$Gr\ =\ \frac{g\rho\beta\left(Ts-Tair\right)Lc^3}{\upsilon^2}$$

$$Gr\ =\ \frac{g\beta\left(Ts-Tair\right)Lc^2}{\upsilon^3}$$

It enables the calculation of the amount of radiation emitted in all directions an over all wavelengths, if the temperature of the blackbody is known 

The maximum spectral emissive power is displaced to shorter wavelengths with increasing temperature of the body

The maximum spectral emissive power is displaced at maximum wavelengths 

  $$T_{\max}\cdot\lambda\ =\ 2898\ \left[\mu m\cdot K\right]$$

Equal surfaces should only be counted once when calculating the mean radiant temperature

The sum of all the view factors must be equal to 1

The abscissa in the view factor table is on a logarithmic scale, while the ordinate is on a linear scale 

The abscissa in the view factor table is on a linear scale, while the ordinate is on a logarithmic scale