Vertaile menetelmiä
Tarkastele valitsemiasi menetelmiä rinnakkain; eroavat rivit korostetaan.
| Gravitaatiolinssi-ilmiö× | Vahva gravitaatiolinssi-ilmiö× | |
|---|---|---|
| Tieteenala | Tähtitiede | Tähtitiede |
| Menetelmäperhe | Process / pipeline | Process / pipeline |
| Syntyvuosi≠ | 1986 | 1964 |
| Kehittäjä≠ | Bohdan Paczynski | Sjur Refsdal |
| Tyyppi≠ | Observational detection method | Observational measurement method |
| Alkuperäislähde≠ | Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5. DOI ↗ | Refsdal, S. (1964). On the possibility of determining Hubble's parameter and the masses of galaxies from the gravitational lens effect. Monthly Notices of the Royal Astronomical Society, 128(4), 307-311. DOI ↗ |
| Rinnakkaisnimet≠ | Microlensing, Gravitational Lensing Method | Strong Lensing, Gravitational Lens, Einstein Ring |
| Liittyvät | 3 | 3 |
| Tiivistelmä≠ | 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. | Strong gravitational lensing occurs when massive objects (clusters, galaxies) bend light so strongly that multiple images of distant sources appear, or complete rings (Einstein rings) form. Proposed by Sjur Refsdal in 1964 and first observed in 0957+561 in 1979, strong lensing provides direct measurements of lens masses and cosmic distances independent of the distance ladder. |
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