Stellar aberration

Definition and stakes

Henry Crozier Keating Plummer,  On the Theory of Aberration and the Principle of Relativity (1910)

“ We have thus given a perfectly precise meaning to the application of the principle of relativity to stellar aberration. In doing so we have excluded everything which does not belong to the purely optical aspect of the problem. But stellar aberration is not a purely optical problem. For in practice we do not actually observe the apparent motion of the Sun and use the result to correct our observed positions of the stars. The motion which we do use is derived by calculation from the theory of gravitation. ”
Source: Wikisource

Henry Crozier Keating Plummer,  On the Theory of Aberration and the Principle of Relativity (1910)

“ The latter equations give
or
which express the apparent wave-velocity in a moving medium in terms of the absolute, or vice versa. For a vacuum we put W = W' = U, and we have
8. The laws of stellar aberration and of the Doppler effect are at once deducible, as Einstein [3] has shown. For a star situated in the direction making an angle φ with the direction of motion of the observer we have a = - cos φ and a' = - cos φ', where φ' is the apparent direction. Then we see that
These expressions can, however, be simplified.
”
Source: Wikisource

Portrait of David P. Todd David P. Todd,  Astronomy: The Science of the Heavenly Bodies

“ In whatever part of the sky we observe, every star is affected by aberration. At the poles of the ecliptic, 231⁄2 degrees from the earth's poles, the annual aberration orbits of the stars are very small circles, 41" in diameter. Toward the ecliptic the aberration orbits become more and more oval, ellipses in fact of greater and greater eccentricity, but with their major axes all of the same length, until we reach the ecliptic itself; and then the ellipse is flattened into a straight line 41" in length, in which the star travels forth and back once a year. ”
Source: Gutenberg

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