Absolute Velocity and Total Stellar Aberration

It is generally accepted that stellar annual or secular aberration is attributed to the changes in velocity of the detector. We can say it in a slightly different way. By means of the all known experiments, stellar aberration is directly or indirectly detectable and measurable, only if a detector changes its velocity. Our presumption is that stellar aberration is not caused by the changes in the velocity of the detector. It exists due to the movement of the detector regarding to an absolute inertial frame. Therefore it is just the question of how to choose such a frame. In this paper it is proposed a method to detect and measure instantaneous stellar aberration due to absolute velocity. We can call it an “absolute” stellar aberration. Combining an “annual” and an “absolute” we can define a “total” stellar aberration.


Introduction
It is commonly assumed that due to the aberration the observed position of a star is displaced of about 150" toward the direction of the instantaneous velocity of the observer with respect to an inertial reference frame at rest. But, for an observer located at the barycenter of the solar system, the instantaneous effect of the relativistic aberration due to the galactic motion of the solar system (220 km/s) is not directly observable because the velocity-induced aberration pattern is constant [1] [2] [3].
Our hypothesis is in contradiction to the relativistic view on stellar aberration, because according to this theory an absolute frame does not exist nor a measurement of the absolute aberration is possible.
We will start a discussion by the classical explanation of the annual stellar ab-t . In the reference frame of the telescope AB is identical to A'B'. But in the sun's reference frame median lines AB and A'B' are represented by two different positions.
In referring to Figure 1, the following definitions apply Δt-a time required for light to traverse the length of the telescope θ-an angle between the earth velocity about the sun and light ray from the star Δθ-an angle at which a telescope should be tilted in the direction of motion in order for the photons move along the median line of the telescope. Actually this angle is obtained by the two measurements at six months intervals. (1.12) we can say that an approximate value for the stellar aberration θ ∆ is equal to v c θ ∆ ≈ (1.13) Its maximal value is approximately the same for all stars. The accepted value is 20.49552 arc seconds.
The problems related to the stellar aberration that are being treated in this paper, had been already defined and mentioned in the numerous works for example [4].

Description and Role of the "Telescope"
In this paper we will use a term "telescope", although a standard telescope is not suitable for this experiment. In other to perform this experiment instead of using a such telescope one have to design and build a new apparatus. Because of that it will be given its description, but just in few words. Point S represents a center of the top "plane" while S' represents a center of the bottom "plane" of the telescope. Photons enter the telescope at the point S and their direction is perpendicular to the top plane. This means that there is a some part of the telescope who has a role to point the "telescope" in such direction that median line SS ′ becomes parallel to the starlight.
At the bottom plane of the telescope it should be installed a camera in order to take an image of the star (Z) at the point A.
It will be assumed that a star (Z) is extremely far away, so that a parallax may be ignored. For now we can assume that extra-galactic stars are being observed only. Starlight moves in straight line and will remain in the same direction regarding to the ecliptic plane. Photons enter in a perpendicular direction to the top plane of the telescope.
The starlight represents an inertial frame of reference marked by (L) and the telescope represents a moving frame of reference that is marked by (T). We will assume that 1 P -speed of light c is constant and equal in all inertial frames (L) 2 P -there is a one common time for the all frames (L) and the moving frame (T)  -In the first case Figure 2(a), the relative velocity of the telescope v regarding to the frame of the starlight is equal to the 0. At some instant 0 t photon hits the top "plane" at the point S and at some instant 1 t hits the bottom "plane" at the point S'.
-In the second case Figure 2(b), under the same circumstances except that ≠ v 0 contrary to our expectations photon does not hit the bottom plane at the point S' but rather at a some point A. Referring to the Figure 2 -In the third case Figure 2(c), velocity at which a telescope moves relative to the starlight is decomposed to the two components. The first component noted by v is perpendicular to the starlight and the second one noted by u is parallel to starlight. Referring to the Figure 2(c), it follows d SS′ An additional explanation will be given for the third case.
-From the point view of a spectator at the frame (L) a photon hits top plane at the point S (this point is identical to the fixed point S L at the frame (L)). The telescope is moving parallel with the starlight by velocity u, therefore a distance between the point S L and the bottom plane changes. A total distance that photon On the basis of these observations the point S' will be used as a referential origin for measuring the drift caused by the movement of the frame (T) relative to the frame (L). Contrary to the classical experiments when the telescope must be tilted, thus the detection and measuring of displacement is possible, in this experiment the "telescope" will be pointed to the star at the beginning and fixed at the same position until the end of the experiment.

Coordinate Systems
We have already defined starlight as a referential inertial frame. In this section are given the descriptions of the three coordinate systems that will be used in a further discussion.  x"-axis. This is called a vernal equinox direction [5]. The position of the star is described by two angles called right ascension and declination ( Figure 4). The right ascension α is measured eastward in the plane of equator from the vernal equinox direction. The declination δ is measured northward from the equator to the line of sight, we would say that is an angle between the plane of equator and the direction of the starlight [5]. Unlike longitude, right ascension is usually measured in hours, minutes, and seconds with 24 hours being a full circle, but in this experiment it will be assumed that it Journal of Applied Mathematics and Physics is measured in radians.
Referring to the Figure 4 we have Now we will define a coordinate system ( ) S xyz ′ that is attached to the telescope in the following way ( Figure 4).
Let suppose that a telescope is positioned in such way that points S and S' lie in the same meridian plane (a plane that passes through the Earth's axis of rotation) (γ). The plane (γ) is rotating about z'-axis but at a fixed sidereal time that will be marked as s 0 (~α) this plane is parallel to the photons who are coming from a distant star. Just to mention that sidereal time has the same value as the right ascension of any celestial body that is crossing the local meridian at that same moment. At that same moment the telescope has to be tilted so starlight is perpendicular to the top plane of the telescope. That means that at that instant the starlight is perpendicular to the bottom plane as well. Let the point S' represents origin of the ( ) S xyz ′ coordinate system and direction S S ′  represents positive z-axis. A x-axis is determined by a intersection between the plane (γ) and the bottom plane of the telescope. Positive y-axis is perpendicular to the plane (γ) and eastward directed. Positive x-axis is chosen so as to form a right-handed coordinate system.
The meridian plane (γ) is perpendicular to the earth equatorial plane ( ) and y-axis is perpendicular to the plane (γ), therefore y-axis is parallel to the earth equatorial plane ( ) Plane (e) represents "ecliptic" plane and a line (n) represents an intersection between "ecliptic" and S xy ′ plane. The measurements will be taken daily dur- ing the year at the fixed sidereal time s 0 , when the top plane of the telescope is perpendicular to the starlight.

Coordinate Transformations
To each of these coordinate systems we are going to join an orthonormal basis.
It means that they are all unit vectors and orthogonal to each other.
The triplet ( ) The corresponding transformation matrix B is equal to Now we are going to derive a transformation matrix A. As shown in Figure 4, First we are going to rotate the coordinate system ( ) O x y z ′ ′ ′ about the positive z'-axis through an angle α, to a some temporary coordinate system K. The After that we are going to rotate the coordinate system K about its positive y-axis through an angle 2 δ Π − , to the coordinate system K'. The corres- In that way the coordinate frame In a different form we can write that A corresponding matrix of the transformation from the basis ( )ˆ, The proof is simple. ...etc.
we can write it in a different form   cos  sin  sin  cos  1  0  0   sin  cos  0  0 cos  sin  cos  cos  cos  sin  sin  0 sin  cos   sin  cos  sin  sin  cos  cos  sin  sin  sin  sin  cos  cos   sin  cos  cos  cos  sin  cos  cos  cos  sin  sin  sin  sin The latest equation can be written in following way

Experiment
The absolute motion of the Earth may be presumed to be resultant of the three components. One of these v is the Earth's orbital motion about the sun, the second component is the motion of the sun about the center of the Milky Way and the third one is the motion of our Galaxy regarding to other galaxies in the Universe. The sum of the second and third component will be marked by 0 v . An absolute earth velocity vector is given by equation: During the period of one year we can assume that ( ) was resultant of the two components, the first one that is changing in direction and magnitude and second one that is invariable.
Our task is to find out a relation between the Equations (5.2) and (5.1) in other words to find out relation between the absolute velocity ( ) Let the Z' and Z'' represent their images at the some instant T on the plane ( ) S xy ′ . Replacing A' by Z' and A' by Z'' we have got a situation similar to the that one shown in Figure 5.
What is not true. Because it has never been observed any major aberration between the two binary stars. That means that variable component of the vector    (5.29)

Transformation of the Vector v(t) from the Ecliptic Plane to the Frame of Telescope
Earth's orbital velocity about the sun.
With the respect to the basis ( ) is given by the equation: Using the matrix of transformation C we will transform vector ( ) In the special case when Let these instants are marked by 0 t and 2 t . Beside these two we can define new times 1 t and 3 t in that way that a difference between 1 t and 0 t and difference between 3 t and 2 t are approximately equal to three months. We must keep in mind that corresponding sidereal times for the instants 0 1 2 3 , , , t t t t are the same and equal to the s 0 . In this way we can make sure that at least two of these four instants fall in the nighttime.
Note that vectors ( )

Analysis
Now we will analyze the vector 1 w normal projection of the vector 0 w on the plane xy.
Depending on the vector ′ S A (5.29) there are two possibilities: 1) ( ′ ≠ S A 0 ) In this case we assume that measurements have been taken for the different stars and at least in one case ′ ≠ S A 0 . We can claim that the outcome of the experiment is positive, because some stellar aberration different from the Bradley's stellar aberration has been detected.
Let, with the respect to the basis ( )ˆ, is given by the equation: Referring to Figure 6 we obtain ( ) Analogously we can get following expression Let suppose that the two measurements have been made at the times 0 T and 1 T . A difference between the times 0 T and 1 T is equal to the six (or the three) months.
We get the linear system of two equations in two unknowns The solution is given by expression Analogously to the Equation (7.12) we can get value for the component y U .
The vector 0 w is given by the following equation In that way a vector The velocity 0 w given by (5.2) is equal to the velocity 0 v given by the Equation (5.1). We can make conclusion that the starlight represents absolute stationary frame and the velocity at which the Earth moves relative to starlight depends on Earth absolute velocity and an angle between the ecliptic and starlight.
By the time, because of the star movement through the space an angle between the ecliptic plane and the starlight will change. In long run it will affect stellar aberration but the velocity of the star is irrelevant for stellar aberration instant measuring. -Φ an angle between the plane S('xy) and vector ( ) arccos arccos Referring to (6.9) we obtain that  We must declare the experiment failed, and the definition of the "absolute" stellar aberration must be discarded, because aberration as such doesn't exist.
3) Stellar aberration in case when ′ ≠ S A 0 . In this section we will find formulas for Bradley's, "absolute" and "total" stel-Journal of Applied Mathematics and Physics lar aberration.