قارن الطرق
راجع الطرق التي اخترتها جنبًا إلى جنب؛ الصفوف المختلفة مميَّزة.
| المسافة الكينماتيكية× | تحليل منحنى الدوران× | |
|---|---|---|
| المجال | علم الفلك | علم الفلك |
| العائلة | Process / pipeline | Process / pipeline |
| سنة النشأة≠ | 1957 | 1970 |
| صاحب الطريقة≠ | Bert Westerhout | Vera Rubin |
| النوع≠ | Kinematic measurement method | Observational kinematic method |
| المصدر التأسيسي≠ | 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 ↗ | 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 ↗ |
| الأسماء البديلة | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis |
| ذات صلة | 3 | 3 |
| الملخص≠ | 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. | 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. |
| ScholarGateمجموعة البيانات ↗ |
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