PAllen said:
---Einstein's paper deals with total aberration, which is the combination of declination and ascension aberration (as a total displacement angle). I assume astronomers can detect both aberrations now. Having reviewed astronomic coordinates, I notice that stars at certain positions on the ecliptic will never undergo seasonal declination aberration; they will only have right ascension aberration. Stars at 90% on the ecliptic to these will have both aberrations, but the declination aberration will be smaller than the ascension aberration. Of course, for stars on the ecliptic, there will be no aberration at all twice a year.
For a star perpendicular to the ecliptic, there will always be aberration (of constant magnitude relative to position in a solar system frame), but twice a year it will include no declination aberration (it will be pure ascension aberration).
Stars in between, will have varying total aberration, and will also have no declination aberration twice a year.
Finally, I don't think any of this has to do with relativistic aberration per se. The size of the relativistic correction to classical aberration is, last I checked, undetectable for Earth's orbital speed. My guesstimate for the correction due to the difference between classical and relativistic aberration for seasonal aberration from Earth's motion would be of the order .002 arcseconds. Thus, none of this discussion has anything to do with special relativity. It only relates to the finite speed of light (Galilean versus Special relativity is not distinguished).
Stars in between declination θ
0 = 90° and θ
0 ≈ 0° will have varying declination aberration and varying right ascension aberration. However, stars in this range will have zero declination aberration when α
0 = 90° and 270° according to the Declination Aberration Model described in the 2010 Astronomical Almanac (AA). I agree there is no declination aberration for a star in the ecliptic plane; however, the attached "AA Declination Aberration Model for a star near the ecliptic plane" the declination aberration is zero two times a year (when α
0 = 90° and 270°). As for right ascension aberration, I can only say that the AA Right Ascension model seems to confirms that right ascension aberration is zero for a star in the ecliptic plane only when α
0 = 0.
According to Einstein’s 1905 paper: If we call the angle between the wave-normal (direction of the ray) in the moving system and the connecting line “source-observer” θ, the equation for θ assumes the form cos θ = - (cos θ
0 − v/c)/(1 − cos θ
0• (v/c)). This equation expresses the law of aberration in its most general form. If θ
0 = π/2 (i.e. if θ
0 = 90º) the equation becomes simply: cos θ = − v/c.
Therefore: When θ
0 = 90º, v = -29.783, c = 299792.458, then cos θ = -29.783/ 299792.458 = -0.005692072º = -20.491458542 arc seconds. This value agrees very closely to James Bradley’s Constant of Aberration (= -atan(v/c) = -20.491458475 arc seconds) which is the declination aberration for a star at the zenith (at θ
0 = 90º) according to Bradley’s Falling Rain Model. Bradley's model may be referred to as the "Classical" aberration model because it was the first since Bradley discovered stellar aberration in the late 1720's. Therefore, you can see that Bradley's "Classical" model and Einstein's 1905 "Relativistic" model closely agree to within 0.000001 arc seconds: That is, they both agree that the declination aberration of a zenith star (at θ
0 = 90°) has a declination aberration of -20.491458 arc seconds. I believe the Bradley model assumes a declination aberration close to 20.5 arc seconds every day of a year. Since many physicists claim that Bradley's "Classical" model and Einstein's "Relativistic" model closely agree, I must also assume that Einstein's "Relativistic" model predicts that declination aberration is about 20.5 arc seconds every day of a year.
The attached "AA Declination Aberration Model for a star at the ecliptic pole" disagrees with those who say that declination aberration is about 20.5 arc seconds every day of the year for a star at or very near an ecliptic pole. This attachment shows that declination aberration is zero when right ascension (α
0 = 90° and 270°). Also, the "AA Declination Aberration Model for declination = 75°" and "AA Declination Aberration Model for a star near the ecliptic plane" show that declination aberration is near zero when right ascension is 90° and 270°.
Finally, I believe that the AA Declination Aberration Model is the most accurate model because the Astronomical Almanac is a universally accepted authority on prediction of the precise apparent location for a star on a specific future date and time. Also, the AA Models predicted locations of important stars such as Polaris and gamma-Draconis at θ
0 = 75° (the star Bradley studied) (see attached AA Declination Aberration for Declination = 75 degrees) have been verified many times by telescopic observation.