विधियों की तुलना करें
चुनी हुई विधियों की आमने-सामने समीक्षा करें; भिन्नता वाली पंक्तियाँ रेखांकित हैं।
| घूर्णन वक्र विश्लेषण (Rotation Curve Analysis)× | गतिक दूरी× | |
|---|---|---|
| क्षेत्र | खगोल विज्ञान | खगोल विज्ञान |
| परिवार | Process / pipeline | Process / pipeline |
| उद्भव वर्ष≠ | 1970 | 1957 |
| प्रवर्तक≠ | Vera Rubin | Bert Westerhout |
| प्रकार≠ | Observational kinematic method | Kinematic measurement method |
| मौलिक स्रोत≠ | 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 ↗ | 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 ↗ |
| उपनाम | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax |
| संबंधित | 3 | 3 |
| सारांश≠ | 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. | 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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