Сравнение методов
Просматривайте выбранные методы рядом; строки с различиями подсвечены.
| Гравитационное микролинзирование× | Слабое гравитационное линзирование× | |
|---|---|---|
| Область | Астрономия | Астрономия |
| Семейство | Process / pipeline | Process / pipeline |
| Год появления≠ | 1986 | 1992 |
| Автор метода≠ | Bohdan Paczynski | Nick Kaiser |
| Тип≠ | Observational detection method | Observational measurement method |
| Основополагающий источник≠ | Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5. DOI ↗ | Kaiser, N. (1992). Weak gravitational lensing of distant galaxies. Astrophysical Journal, 388, 272-286. DOI ↗ |
| Другие названия≠ | Microlensing, Gravitational Lensing Method | Weak Lensing, Cosmic Shear, Lensing Distortion |
| Связанные | 3 | 3 |
| Сводка≠ | 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. | Weak gravitational lensing occurs when light from distant sources bends slightly as it travels through the universe, passing through the gravitational fields of matter concentrations. Proposed theoretically by Nick Kaiser in 1992, this subtle effect has become one of the most powerful cosmological probes, directly revealing the distribution of all matter (dark and luminous) across cosmic distances. |
| ScholarGateНабор данных ↗ |
|
|