手法を比較
選択した手法を並べて確認できます。異なる行はハイライト表示されます。
| トランジット測光法× | 天体測量（年周視差）× | |
|---|---|---|
| 分野 | 天文学 | 天文学 |
| 系統 | Process / pipeline | Process / pipeline |
| 提唱年≠ | 1984 | 1838 |
| 提唱者≠ | William Borucki | Friedrich Wilhelm Bessel |
| 種類≠ | Observational photometric pipeline | Astrometric distance measurement |
| 原典≠ | Borucki, W. J., & Summers, A. L. (1984). The photometric method of detecting other planetary systems. Astrophysical Journal, 281, 537-553. DOI ↗ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ |
| 別名≠ | Photometric Transit Method, Planetary Transit Detection | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method |
| 関連 | 3 | 3 |
| 概要≠ | Transit photometry is an observational technique that detects exoplanets by monitoring the periodic dips in stellar brightness as planets cross in front of their host stars. First systematized by William Borucki in 1984, this method became the most successful exoplanet detection technique, with the Kepler space telescope discovering thousands of confirmed exoplanets using this approach. | 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. |
| ScholarGateデータセット ↗ |
|
|