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Effects to look for:
An excellent reference for this sort of calculation is the paper of McKinley and Doherty (1979).
The most realistic choice is the Yale Bright Stars, which is a catalog of stars brighter than magnitude 6.5, as seen from Earth. The view shown is towards Polaris, the North Star. If you look closely, you will be able to see the Big Dipper just to the left of center (it's tiny).
The other choices for stars:
Applies to the half-sky views only. Turn this setting on to see the half-sky radius (contains 'half the sky') and the neutral radius (where the doppler factor D=1).
This simulation makes the rough approximation that the light from the stars is identical to a black body spectrum, which is characterized by a single number - the black body surface temperature. Different surface temperatures have different colors, from reddish-orange (coolest), to white, to bluish-white (hottest).
The perception of the colour of starlight by the human eye is weak. The colors shown here are more like the colors you would see in a photograph of the stars, instead of by the human eye.
At the high density of stars you would see at high values of β, there should be visible a graduated color effect, with blue stars in the center, changing to white away from the center, and then red stars towards the edge.
Turn this off if your browser slows down. The animation does a lot of processing, and sometimes your computer may have trouble keeping up. Drawing stars as small squares instead of circles can sometimes help.
The number of stars per cubic parsec. This is used only for the randomly generated sets of stars, and not for stars from the Yale Bright Star Catalog. Increase the density a bit if you want to see more stars.
The cut-off point for showing stars, according to brightness. A higher limiting magnitude means you will see more stars.
There can be many stars in these simulations, but you usually won't see them all. There's a good reason for having stars in the simulation that you can't see all the time. Due to relativistic effects, stars can increase in brightness. So, stars that are initially not visible (and are below the limiting magnitude), can often become visible later on.
Stars on the celestial sphere need to be projected onto the flat plane of the screen. Various star map projections are provided. You can select the one that you prefer. Some show half the sky, and some show the whole sky. In each case, the center corresponds to the direction of motion.
Note that with the whole-sky projections, some of the motions of stars along the edge of the view are an artifact of the map projection being used.
Roughly equivalent to the number of Vega-like stars that would produce the same amount of apparent radiant energy produced by the visible stars. This is a measure of the total brightness of all the stars visible in the sky, as seen from the spacecraft. It includes only those stars that are brighter than the given limiting magnitude. It's calculated using a formula that relates differences in magnitude to differences in luminosity. Here, 1 unit of brightness is equivalent to 1 star of magnitude 0. The bright star Vega has magnitude 0.03, so this is roughly the equivalent number of Vegas that would produce the same apparent radiant energy. On the same scale, a full Moon is about 125,000 units.