Порівняння методів
Переглядайте обрані методи поруч; рядки з відмінностями підсвічено.
| Гравітаційне мікролінзування× | Кінематична відстань× | |
|---|---|---|
| Галузь | Астрономія | Астрономія |
| Родина | Process / pipeline | Process / pipeline |
| Рік появи≠ | 1986 | 1957 |
| Автор методу≠ | Bohdan Paczynski | Bert Westerhout |
| Тип≠ | Observational detection method | Kinematic measurement method |
| Основоположне джерело≠ | Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5. 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≠ | Microlensing, Gravitational Lensing Method | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax |
| Пов'язані | 3 | 3 |
| Підсумок≠ | Gravitational microlensing is an observational technique that exploits Einstein's prediction that massive objects bend light. When a star or planet passes in front of a distant star from our perspective, its gravity acts as a lens, magnifying and distorting the background star's light. First proposed by Bohdan Paczynski in 1986, this method has discovered hundreds of exoplanets and provides unique sensitivity to low-mass planets and 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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