That is called parallax and it happens when a nearby star appears to move against the background as the Earth moves round the Sun. The baseline is the mean radius of the Earth's orbit (not the diameter) and a star which has a parallax of 1 arc-second would be at a distance of 1 parsec.
In practice the nearest stars have a parallax of about 0.7 seconds so are at a distance of 1.4 parsecs or 4 light-years.
Parallaxes are always small and require sensitive instruments to measure. The lack of parallax was formerly used as a proof that the Earth must be fixed, and it took until 1838 for Bessel to measure the first stellar parallax. After that people began to realise that the stars are much further away than they had thought.
They use trigonometry to measure the parallax error in the nearby star's position based on a large triangle, the base of which is formed by two times the distance of the Earth to the Sun. Simply stated, they plot the star's position on one day, and again six months later, when the Earth is 186,000 miles away from its original position. They use the far distant stars as a calibration standard, and use the Pythagorean theorem to figure out the rest.
Astronomers measure parallax by using a large base. Often, the base is 186,000,000 miles long, the distance between two positions of the Earth six months apart. When looking at a star field using these two relative positions, it is possible to see some of the stars being in a different position relative to other more distant stars. This is parallax and it allows us to estimate the distance to that particular star using trigonometry.
On average, Neptune orbits the Sun at a distance of 30.1 AU, approximately 30 times the Earth-Sun distance Unexpected changes in the orbit of Uranus led astronomers to deduce that its orbit was subject to gravitational perturbation by an unknown planet. Neptune was subsequently found within a degree of its predicted position, and its largest moon, Triton, was discovered shortly thereafter.
velocity
Displacement is the term for the change in position of an object. You find displacement by taking the final position of the object and subtract the initial position of the object.
Nearby stars appear to change their position against the distant background in an annual cycle, because of the Earth's changing position 'across' its orbit. This apparent shift is called the star's "parallax".
by using the position on the sky and the redshift to determine a distance along the line of sight
by using the position on the sky and the redshift to determine a distance along the line of sight
Astronomers use a method called parallax to measure the distance to nearby stars. Astronomers can measure parallax by measuring the position of a nearby star with respect to the distant stars behind it. Then, they measure the same stars again six months later when the Earth is on the opposite side of its orbit.
by changing the position of the object being observed
motion can be observed from any position
No , I can't , it is job of astrologist and astronomers !
The distance between the final position and the starting position is the
Not calipers. Astronomers snap a photo, wait six months, then snap another. The apparent change in position with respect to much further background stars gives them a decent estimate, using the diameter of Earth's solar orbit as one leg of an extremely long isosceles triangle. We gauge distances to further stars using apparent brightness of Cepheid variables, and so on.
No, the position of the Moon and the Sun as OBSERVED from the Earth.
Distance 1 is -4 so the position is -4!
Yes