parallax method

par·al·lax meth·od

localization of a foreign body by observing the direction of its motion on a fluoroscopic screen while moving the x-ray tube or the screen.
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This level of precision allowed astronomers to track the true movement of stars, instead of relying on an approximation using the parallax method - the apparent shift seen in object's position in the sky, as Earth orbits the sun.
Two ways in which these CG volume holograms can be recorded is by either the single parallax method or the full parallax method.
However, the parallax method can only be applied for stars which are reasonably close to us, since beyond distances of 1600 light years, the angles of inclination are too small to be measured by the Hipparcos satellite, a precursor to Gaia.
In the 19th century, astronomers learned how to convert a star's apparent brightness into its intrinsic brightness (luminosity) by measuring its distance using the parallax method. But it wasn't until the early 20th century that astronomers started to measure the temperatures of the outer atmospheres of stars.
The parallax method is feasible only if the basis is not too small with respect to the distance of the object.
After the 1874 transit, astronomers realized that Halley's parallax method would not nail down the value of the astronomical unit as precisely as they had hoped.
The team used the 0.9-meter telescope at the Cerro Tololo Inter-American Observatory in Chile to measure the distances to the red dwarfs using the classic trigonometric parallax method. Thanks to RECONS and other groups, the number of known star systems within 10 parsecs has grown by 34 members (16%) in the past six years.
FEEBLEST DWARF A team of Chilean and US astronomers using the classic parallax method have measured the distance to a cool object (probably a brown dwarf) known as DEN 0255-4700 and found that it is the nearest known object of its spectral type.
Moreover, as a practical matter, few distances in modern astronomy are directly measured by the parallax method anymore.
The most common way of measuring the distances of the nearby stars is the parallax method. As the Earth orbits the Sun during the course of a year our changing vantage causes the apparent position of a nearby star to shift minutely.