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The position of the star is given as two angles and a distance.What I would like physicists to understand because it is doubly important, for the beauty of the thing, and then for the scientific truth of the equations that will result from it, is the notion of universal anisochrony, and the fact that what we believe to be an absolute present time, does not exist.
The angles are Right ascension (RA) and Declination(DEC).
The former is equivalent to longitude and the latter to latitude.
The distance is given in Parsecs or light years.
It is of course a trivial matter to convert these three coordinates
to a Cartesian frame of reference.
Your system have the transit time of the light from the star
as a fourth coordinate, which is redundant because it is given
by the distance.
I didn't fail to notice that your √(x² + y² + z²) = -To⋅c.
So you could remove the To from your system.
When it comes to the time of the observation t, it would be
very inconvenient if the stars in the star catalogues were
observed at different times given in the catalogue, so the
data are given as they would be at the same time.
The current standard is Epoch J2000 (January 1, 2000)
That means that if a star is observed at another time,
the data must be calculated to what they were at Epoch J2000.
(The angular and radial velocity will normally be known).
Now to the real reason why this system is better than yours.
When you know the RA and DEC of the star, you know where
to point the telescope! (Corrected for stellar aberration and parallax.)
You can now buy amateur telescopes where you can enter the RA and DEC
of an astronomical object, and the computer will know where to point
the telescope on a rotating Earth, and even track the object.
You do not have to know the distance.
And when you observe a star, the direction of your telescope
give you the RA and DEC.
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