Vertaile menetelmiä
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| Astrometria (paralleksi)× | Kinemaattinen etäisyys× | |
|---|---|---|
| Tieteenala | Tähtitiede | Tähtitiede |
| Menetelmäperhe | Process / pipeline | Process / pipeline |
| Syntyvuosi≠ | 1838 | 1957 |
| Kehittäjä≠ | Friedrich Wilhelm Bessel | Bert Westerhout |
| Tyyppi≠ | Astrometric distance measurement | Kinematic measurement method |
| Alkuperäislähde≠ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ | 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 ↗ |
| Rinnakkaisnimet | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax |
| Liittyvät | 3 | 3 |
| Tiivistelmä≠ | 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. | 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. |
| ScholarGateAineisto ↗ |
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