方法对比
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| 旋转曲线分析× | 天体测量学（视差）× | 运动距离× | |
|---|---|---|---|
| 领域 | 天文学 | 天文学 | 天文学 |
| 方法族 | Process / pipeline | Process / pipeline | Process / pipeline |
| 起源年份≠ | 1970 | 1838 | 1957 |
| 提出者≠ | Vera Rubin | Friedrich Wilhelm Bessel | Bert Westerhout |
| 类型≠ | Observational kinematic method | Astrometric distance measurement | Kinematic measurement method |
| 开创性文献≠ | 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 ↗ | Reid, M. J., et al. (2014). Trigonometric parallaxes of high mass star forming regions: the structure and kinematics of the Milky Way. Astrophysical Journal, 783(2), 130. DOI ↗ |
| 别名 | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax |
| 相关 | 3 | 3 | 3 |
| 摘要≠ | 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. | Kinematic distance is a method for estimating distances to objects in the Milky Way using their observed radial velocities and the known rotation curve of the Galaxy. Developed in the 1950s by Bert Westerhout and others, this technique enables distance determination to distant molecular clouds and masers without trigonometric parallax or individual object luminosities. |
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