Порівняння методів
Переглядайте обрані методи поруч; рядки з відмінностями підсвічено.
| Аналіз кривих обертання× | Кінематична відстань× | |
|---|---|---|
| Галузь | Астрономія | Астрономія |
| Родина | Process / pipeline | Process / pipeline |
| Рік появи≠ | 1970 | 1957 |
| Автор методу≠ | Vera Rubin | Bert Westerhout |
| Тип≠ | Observational kinematic method | Kinematic measurement 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 ↗ | 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 ↗ |
| Інші назви | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax |
| Пов'язані | 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. | 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. |
| ScholarGateНабір даних ↗ |
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