chaos syndrome wrote:... but I hadn't managed to convince myself that a blackbody distribution mapped to another blackbody distribution, though it seemed like that would be the case.
One way to convince yourself without wading through the maths is to look at a
log-log plot of black body spectra for various temperatures.
It's clear that all the curves are same shape, and differ only in their horizontal and vertical displacement. Since it's a log plot, we can see immediately that applying a constant multiple to all the frequencies in a given spectrum (as we do with Doppler) will simply move the curve to a new horizontal location without changing its shape. Let's call the relativistic Doppler multiplier for frequency ?·. If we multiply frequencies throughout by ?·, then the peak frequency will move from a location corresponding to the rest-frame temperature T, to a location corresponding (according to Wien) to a temperature of ?·.T.
But what about the necessary vertical scaling? This is proportional to the total flux, of course, which is in turn proportional to T^4. If our new apparent temperature under relativistic Doppler is to be ?·.T, then our flux F needs to be transformed to ?·^4.F. And it is: each photon is received in the moving frame with an energy ?· times its rest frame energy; such photons are received at ?· times the rest-frame rate; and the effect of relativistic stellar aberration alters the angular area of a radiant source by a factor of ?·^2. So the apparent flux per steradian is ?·^4 times the rest-frame flux.
We've therefore consistently accounted for the preservation of curve shape, the shift in position against the frequency axis and the shift in position against the flux axis: all the appearances in the moving frame are of a black body with temperature ?·.T.
If you do want to do the underlying maths, you'll find it's possible to recast Planck's equation for the black body spectrum (by inserting Stefan-Boltzmann and then moving terms around) so that the shape of the curve is defined by an expression in (h??/kT), and its height depends on T^4: playing with ?? and T by plugging in the ?·'s then reproduces the behaviour of the graphs in my link.
Grant