Estimating the temperature

The temperature of a solar spot or a facula can be estimated from an intensity profile.

The Stefan-Boltzmann law gives a correlation between emitted radiative power P of a black body, the emitting area A, and its absolute temperature T:

\begin{equation*} P = \sigma \cdot A \cdot T^4 \end{equation*}

For details, see the relevant literature or Wikipedia.

To determine the temperature by the Stefan-Boltzmann law, compare two radiative powers $P_1$ and $P_2$.

\begin{equation*} \frac{P_1}{P_2}=\frac{T_1^4}{T_2^4} \end{equation*}

As proxy of the radiative power one can use the measured count number (see here).

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  • en/praktikum/sunspot-temp.txt
  • Last modified: 2016/06/28 00:15
  • by rhainich