A blackbody or *planckian radiator* is an ideal thermal radiator that absorbs completely all incident radiation, whatever the wavelength, the direction of incidence or the polarization. [1]

A *blackbody* in thermal equilibrium emits electromagnetic radiation called blackbody radiation.

The spectral radiance of a blackbody at thermodynamic temperature $T [K]$ in a medium having index of refraction $n$ is given by the Planck's law equation: [2]

$$ \begin{equation} L_{e\lambda}(\lambda,T)=\cfrac{C_1n^{-2}\lambda^{-5}}{\pi}{\Biggl[\exp\biggl(\cfrac{C_2}{n\lambda T}\biggr)-1\Biggr]^{-1}} \end{equation} $$where $$ \begin{equation} \begin{aligned} C_1&=2\pi hc^2\\ C_2&=\cfrac{hc}{k} \end{aligned} \end{equation} $$

$h$ is Planck's constant, $c$ is the speed of light in vacuum, $k$ is the Boltzmann constant and $\lambda$ is the wavelength.

As per *CIE 015:2004 Colorimetry, 3rd Edition* recommendation $C_2$ value when used in colorimetry should be $C_2= 1,4388x10^{-2}mK$ as defined by the International Temperature Scale (ITS-90).

$C_1$ value is given by the Committee on Data for Science and Technology (CODATA) and should be $C_1=3,741771x10^{16}Wm^2$.

In the current *CIE 015:2004 Colorimetry, 3rd Edition* recommendation, colour temperature and correlated colour temperature are calculated with $n=1$.

Colour implements various *blackbody* computation related objects in the `colour.colorimetry`

sub-package:

In [1]:

```
import colour.colorimetry
```

Note:

`colour.colorimetry`

package public API is also available from the`colour`

namespace.

*Planck's law* is called using either the `colour.planck_law`

or `colour.blackbody_spectral_radiance`

definitions, they are expecting the wavelength $\lambda$ to be given in nanometers and the temperature $T$ to be given in degree kelvin:

In [2]:

```
import colour
colour.colorimetry.planck_law(500 * 1e-9, 5500)
```

Out[2]:

20472701909806.578

*blackbody* is done using the `colour.sd_blackbody`

definition:

In [3]:

```
with colour.utilities.suppress_warnings(python_warnings=True):
colour.sd_blackbody(6500, colour.SpectralShape(0, 10000, 10))
```

In [4]:

```
from colour.plotting import *
```

In [5]:

```
colour_style();
```

In [6]:

```
# Plotting various *blackbodies* spectral distributions.
blackbodies_sds = [colour.sd_blackbody(i, colour.SpectralShape(0, 10000, 10))
for i in range(1000, 15000, 1000)]
with colour.utilities.suppress_warnings(python_warnings=True):
plot_multi_sds(blackbodies_sds,
y_label='W / (sr m$^2$) / m',
use_sds_colours=True,
normalise_sds_colours=True,
legend_location='upper right',
bounding_box=[0, 1000, 0, 2.25e15]);
```

Let's plot the blackbody colours from temperature in domain [150, 12500, 50]:

In [7]:

```
plot_blackbody_colours(colour.SpectralShape(500, 12500, 50));
```

In [8]:

```
# Comparing theoretical and measured *Sun* spectral distributions.
# Arbitrary ASTMG173_ETR scaling factor calculated with
# :def:`colour.sd_to_XYZ` definition.
ASTMG173_sd = ASTMG173_ETR.copy() * 1.37905559e+13
blackbody_sd = colour.sd_blackbody(
5778,
ASTMG173_sd.shape)
blackbody_sd.name = 'The Sun - 5778K'
plot_multi_sds([ASTMG173_sd, blackbody_sd],
y_label='W / (sr m$^2$) / m',
legend_location='upper right');
```

As you can see the *Sun* spectral distribution is very close to the one from a blackbody at similar temperature $T$.

Calculating theoritical colour of any star is possible, for example the VY Canis Majoris red hypergiant in the constellation *Canis Major*.

In [9]:

```
plot_blackbody_spectral_radiance(temperature=3500, blackbody='VY Canis Majoris');
```

*Orion* and the seventh brightest star in the night sky.

In [10]:

```
plot_blackbody_spectral_radiance(temperature=12130, blackbody='Rigel');
```

And finally the Sun, our star:

In [11]:

```
plot_blackbody_spectral_radiance(temperature=5778, blackbody='The Sun');
```

- ^ CIE. (n.d.). 17-960 Planckian radiator. Retrieved June 26, 2014, from http://eilv.cie.co.at/term/960
- ^ CIE TC 1-48. (2004). APPENDIX E. INFORMATION ON THE USE OF PLANCK’S EQUATION FOR STANDARD AIR. In
*CIE 015:2004 Colorimetry, 3rd Edition*(pp. 77–82). ISBN:978-3-901-90633-6