These images were rendered using Pixar's RenderMan (TM). Technically, this is not a raytracer, and therefore shadows are not implemented for most of the images. The initial images were 24-bit TIFF files, most of which I have converted to JPEG. The "thumbnail" versions on this page are GIF, so that people without access to JPEG viewers can at least see the half-size versions.
Planetary radii were obtained from Glass (1982). All units were converted to 10^3 kilometres (i.e. the Earth's radius is 6.378*10^3km) for convenience. Viewpoints are normally located on the surface of the Earth, and are expressed in terms of a paleolatitude from the pole of the Earth, which was apparently aligned with the axis of the other planets. The camera direction is normally set to look directly at Saturn. This means high paleolatitudes (e.g., 90 degrees) near the pole look almost straight up, while lower paleolatitudes look closer to the horizon.
I gave Mars a reddish-brown colour, Venus a white colour. For Saturn
I used the "wood" shader to give the (crude) appearance of banded clouds
with an off-yellow-brown colour (it needs work). The bodies are illuminated
either from a lightsource approximately "behind" the Earth (i.e. the
opposite side from the other planets) in order to clearly show the
shape of the bodies, or from a position off to one side of the arrangement,
in a crude attempt to duplicate the "crescent" appearance as depicted
by the
image
at
Ted Holden's WWW page. Again, shadows
are *not* implemented, so beware of the assumption the illumination
is accurate! Someday, if there is interest, this might be fixed.
Initial experimentation with shadows (Using BMRT) suggests the variations
in illumination orientation (as predicted by Talbott's model)
would regularly produce obvious shadows and eclipses on one or more of
the planets:
45 degree viewpoint, slight offset of lightsource
The experimental images do not implement umbra-penumbral effects, so they still need some work before they can be used to really test this effect.
This shows Saturn on the left, followed by Venus, Mars, and Earth on the right. At this scale the latter three are very small in the "lateral view" image (only two or three pixels!). These images also have rings around Saturn thanks to my initial confusion about the model. According to Ev, these were not present at the time the arrangement existed, and they are removed from subsequent images.
Ev provided the following distances, all measured from Earth, in article
<pM4Y-E0.ecochrane@delphi.com>on March 27, 1995:
Saturn 807000 km
Venus 500000 km
Mars 400000 km
These images also have the Moon at its current distances from Earth,
displaced a bit to the "up" side of these images, and
in the upper left of all the "from Earth" views. This provides a relative
angular scale to judge the visual size of the views from Earth. Basically,
this planetary arrangement would be *HUGE* from Earth:
Original model, 90 degrees viewpoint.
Try to imagine this next time you are out looking at the Moon :-)
More recently (Nov. 1995), people have noticed the image at the
Aeon home page, and have pointed out that it
does not correspond to the previous distances Ev has provided
(For that matter, the same thing was said of the
image on Ted's page). Venus
and Mars are proportionally much bigger, implying they are closer. Wayne
Throop (throop@aur.alcatel.com) has anaylzed the image using simple geometrical
calculations, and determined the relative position of the planets.
His results, including images, are presented at:
Wayne's analysis. Basically, the geometrical calculations result in a
ratio of distances between the planets, which can be scaled to the furthest
distance, Saturn, using Ev's previous distance:
Ev's original Ratio Revised to fit Aeon page
Saturn 807000 km 1.000 807000 km
Venus 500000 km 0.352 807000km*0.352 = 284064 km
Mars 400000 km 0.241 807000km*0.241 = 194487 km
Subsequent to Wayne' work, and Ev's claim there was no problem,
I decided to revise my 3D models to double-check Wayne's results:
Aeon model, 90 degrees viewpoint.
There is a close correspondance.
Aeon model, 50 degrees viewpoint
Aeon model, 45 degrees viewpoint
Aeon model, 30 degrees viewpoint
As 0 degrees is approached (i.e. the "paleoequator"), the image of the planets begin to sink below the horizon:
Aeon model, 0 degrees viewpoint
[NOTE: The Moon appears larger in this image because the relative positions of the planets was changed for this model. This does not change the qualitative appearance of the planets. See the next image for justification.]
Changing the absolute distance of the planetary bodies while keeping the relative distance the same does not change the appearance of the geometry of the bodies, only their relative size. This next image was rendered with the planetary positions at twice the distance in the model above (i.e. 1614000 km for Saturn with the others suitably scaled). In order to make it approximately the same rendered image size as before, the field of view of the camera was reduced by about half (from 15 to 8 degrees). This is reflected in the much larger relative appearance of the Moon. In reality, the Moon would be the same size, but the planets would appear smaller because they are more distant (think of the effect of using a zoom lens: smaller field of view == greater magnification).
Aeon model -- 2x distance, 70 degrees
Other than the size difference, the "off centre" position is the same as in the 70 degree image above.
The only way to "fix" this would be to make the spin axis of the Earth out of alignment with the linear arrangment of the planets (which would produce other interesting variations), or to change the *relative* planetary distances. Absolute changes with the same planetary distance ratio make *NO* significant difference in the visual appearance other than size.
As before, the viewpoint is from Earth, this time at "90 degrees".
Understanding the model requires familiarity with discussions in the newsgroup talk.origins about a year ago. I do not have time to put the details in here. If you have questions, please send e-mail.
Glass, B.P., 1982. Introduction to Planetary Geology. Cambridge University Press: Cambridge, 469pp.
Andrew MacRae macrae@geo.ucalgary.ca