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Qu'est-ce (qui) est proper motion - définition
![Proper motion of [[61 Cygni]] in one year intervals.](https://commons.wikimedia.org/wiki/Special:FilePath/61 Cygni Proper Motion.gif?width=200 "Proper motion of [[61 Cygni]] in one year intervals.")
![March equinox]] (center of the sun's position then) at the J2000 epoch, is vector ''V''.<br>In red the diagram adds the components of proper motion across the [[celestial sphere]].<br>An ideal time to measure exactly such a small annual shift is at culmination. The culmination of the star is daily reached when the observer (and earth) passes as shown by the blue arrows "beneath" the star.<br>The positive axes of the two components of its usually annually measured or published shift in proper motion are the exaggerated red arrows, note: the right arrows point to the east horizon. One red annotation is subtly shorter as the cosine of a star resting at 0° declination is 1, so such a star's east or west shift would not need to be multiplied by the cosine of its declination.<br>The proper motion vector is '''''μ''''', ''α'' = [[right ascension]], ''δ'' = [[declination]], ''θ'' = [[position angle]].](https://commons.wikimedia.org/wiki/Special:FilePath/Components of proper motion.svg?width=200 "March equinox]] (center of the sun's position then) at the J2000 epoch, is vector ''V''.<br>In red the diagram adds the components of proper motion across the [[celestial sphere]].<br>An ideal time to measure exactly such a small annual shift is at culmination. The culmination of the star is daily reached when the observer (and earth) passes as shown by the blue arrows \"beneath\" the star.<br>The positive axes of the two components of its usually annually measured or published shift in proper motion are the exaggerated red arrows, note: the right arrows point to the east horizon. One red annotation is subtly shorter as the cosine of a star resting at 0° declination is 1, so such a star's east or west shift would not need to be multiplied by the cosine of its declination.<br>The proper motion vector is '''''μ''''', ''α'' = [[right ascension]], ''δ'' = [[declination]], ''θ'' = [[position angle]].")
Wikipédia
Proper motion is the astrometric measure of the observed changes in the apparent places of stars or other celestial objects in the sky, as seen from the center of mass of the Solar System, compared to the abstract background of the more distant stars.
The components for proper motion in the equatorial coordinate system (of a given epoch, often J2000.0) are given in the direction of right ascension (μα) and of declination (μδ). Their combined value is computed as the total proper motion (μ). It has dimensions of angle per time, typically arcseconds per year or milliarcseconds per year.
Knowledge of the proper motion, distance, and radial velocity allows calculations of an object's motion from our star system's frame of reference and its motion from the galactic frame of reference – that is motion in respect to the Sun, and by coordinate transformation, that in respect to the Milky Way.
