Порівняння методів
Переглядайте обрані методи поруч; рядки з відмінностями підсвічено.
| Аналіз кривих обертання× | Астрометрія (Паралакс)× | Масив таймінгу пульсарів× | |
|---|---|---|---|
| Галузь | Астрономія | Астрономія | Астрономія |
| Родина | Process / pipeline | Process / pipeline | Process / pipeline |
| Рік появи≠ | 1970 | 1838 | 1979 |
| Автор методу≠ | Vera Rubin | Friedrich Wilhelm Bessel | Stephen Detweiler |
| Тип≠ | Observational kinematic method | Astrometric distance measurement | Observational timing method |
| Основоположне джерело≠ | Vera C. Rubin & W. Kent Ford Jr. (1970). Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions. Astrophysical Journal, 159, 379-403. DOI ↗ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ | Sazhin, M. V. (1978). Opportunities for detecting ultralong gravitational waves. Soviet Astronomy, 22, 36-38. link ↗ |
| Інші назви | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals |
| Пов'язані | 3 | 3 | 3 |
| Підсумок≠ | Galaxy rotation curve analysis is the technique of measuring how orbital velocities change with distance from the center of a galaxy. Pioneered by Vera Rubin and W. Kent Ford Jr. in 1970, rotation curves revealed one of astronomy's great mysteries: galaxies rotate too fast to be held together by their visible stars alone, providing direct evidence for dark matter. | Astrometric parallax is the foundational geometric method for measuring distances to nearby stars, based on observing the apparent shift in a star's position as Earth orbits the Sun. First successfully demonstrated by Friedrich Wilhelm Bessel in 1838 for the star 61 Cygni, parallax remains the most direct and reliable distance measurement in astronomy, anchoring the entire cosmic distance ladder. | A pulsar timing array uses multiple millisecond pulsars as a distributed network of gravitational wave detectors across the galaxy. Proposed theoretically by Stephen Detweiler in 1979, this method exploits the extraordinary timing precision of pulsars to detect the subtle spacetime distortions caused by gravitational waves. In 2023, the first evidence for a stochastic background of gravitational waves was announced using pulsar timing arrays. |
| ScholarGateНабір даних ↗ |
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