After some experiments in POV, after seeing some POV artits' artwork, it
appeared to me soooo clear that the only way to get realistic behaviour
and colors for atmosphere is to follow ... reality. IOW follow physics and
nature, as much as possible. Having a physically-realistic atmosphere will
produce correct colors, and correct lighting for scenes, and also correct
illumination for clouds and radiosity.
So, the main question is: what makes the atmosphere have such colors in
such circumstances? That is:
-) Why is the sky blue?
-) Why is blue deeper at high altitudes?
-) What makes the atmosphere become reddish at low elevations of the
-) What makes the atmosphre have such a variety of colors, especially
at low elevations of the sun?
-) How to have a correct illumination when the sun is below the
-) etc ...
-) How to make it 'automatic'?
The answer is: follow reality. That is:
-) Have a physical model that can be handled by POV-SDL
-) Determine the variables of this model
-) Implement the model
All the aforementionned behaviours are due to the interaction between the
sun's light and the atmosphere. This interaction is itself due to the
sun's light spectrum, to the kind and density of particles in the
atmosphere, and to the length of the path of the light through them. Every
kind of particle has a specific scattering and absorption behaviour.
Unless particular events (aurorae ...) air particules do not emit light by
themselves. I will consider such phenomena later. These interactions
produce a complex combination of colors which yields what we can observe.
This being said, lets deal a bit with those considerations.
A) SUN's spectrum
In nature, the sun's spectrum is not really white. Some wavelenghts are
missing. But, in outer space, the color of the sun is reported by
astronauts as being 'very' white. TerraPOV will default the sun's color to
B) Kind and density of particles
Until now, I distinguish global atmosphere and ground atmosphere.
Global atmosphere contains air molecules that are responsible for the
Rayleigh scattering which produces the blueness of the sky, yellowishness
of direct sunlight, and blueishness of shadowed areas. Please, refer to
the Web for further information about Rayleigh scattering and blue sky.
TerraPOV uses one media for that. The atmosphere also contains other
particles, in various shape, size and behaviour. This is described by
another media with scatterring and absorption parameters (color and
Ground atmosphere is reponsible for this haze we can see near horizon and
can influence a lot on resulting aspect of the sky. This includes all
kinds of pollution, water vapour, specific gases and so forth. This is
also described by a media with scatterring and absorption parameters.
As you know, the pressure of the atmosphere decreases with altitude. A
search on the web informed me that the pressure decreases 'quite'
exponentilly with height, and that the significant thickness is about
50km. Beyond this altitude, the relative pressure is less than 1/1000 than
that of sea level. The pressure at altitude h for an atmosphere of
thickness T can be expressed with a formula of the kind p = Pmax *
exp(-k*h/T). As density is directly related to pressure, TerraPOV use such
formulae for all altitude-related densities. In order to match the values
found on the web for the pressure/altitude relationship, the factor k is
around 6.7 fot a thickness of 50km. In TerraPOV, Dmax, k and thickness are
C) Length of the light path trough atmosphere
This aspect is due to geometrical considerations: the earth is round, and
the atmosphere is a shell around. Therefore, the length of the path of
light depends on the elevation of the sun, and the geometry determines the
way this length increases/decreases with elevation. This, with density, is
responsible of the reddening at low elevations. TerraPOV uses a round
earth and the atmosphere is a shell around it, with an exponentially
decreasing density as exposed above.
Well here we are for this article. Next article will deal in detail with
the geometrical model related to TerraPOV's sky system, and the first code
fragments will appear.
Utilisant le client e-mail révolutionnaire d'Opera :
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