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| Paralaksa astrometryczna (Paralaksa)× | Analiza krzywej rotacji× | |
|---|---|---|
| Dziedzina | Astronomia | Astronomia |
| Rodzina | Process / pipeline | Process / pipeline |
| Rok powstania≠ | 1838 | 1970 |
| Twórca≠ | Friedrich Wilhelm Bessel | Vera Rubin |
| Typ≠ | Astrometric distance measurement | Observational kinematic method |
| Źródło pierwotne≠ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ | 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 ↗ |
| Inne nazwy | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis |
| Pokrewne | 3 | 3 |
| Podsumowanie≠ | 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. | 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. |
| ScholarGateZbiór danych ↗ |
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