Σύγκριση μεθόδων
Εξετάστε τις επιλεγμένες μεθόδους δίπλα-δίπλα· οι γραμμές που διαφέρουν επισημαίνονται.
| Αστρομετρία (Παράλλαξη)× | Βαρυτική Μικροεστίαση× | |
|---|---|---|
| Πεδίο | Αστρονομία | Αστρονομία |
| Οικογένεια | Process / pipeline | Process / pipeline |
| Έτος προέλευσης≠ | 1838 | 1986 |
| Δημιουργός≠ | Friedrich Wilhelm Bessel | Bohdan Paczynski |
| Τύπος≠ | Astrometric distance measurement | Observational detection method |
| Θεμελιώδης πηγή≠ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ | Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5. DOI ↗ |
| Εναλλακτικές ονομασίες≠ | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | Microlensing, Gravitational Lensing Method |
| Συναφείς | 3 | 3 |
| Σύνοψη≠ | Astrometric parallax is the foundational geometric method for measuring distances to nearby stars, based on observing the apparent shift in a star's position as Earth orbits the Sun. First successfully demonstrated by Friedrich Wilhelm Bessel in 1838 for the star 61 Cygni, parallax remains the most direct and reliable distance measurement in astronomy, anchoring the entire cosmic distance ladder. | 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. |
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