方法证据记录
Radial Velocity Method
The radial velocity method detects exoplanets by measuring the Doppler shift of a star's spectral lines caused by gravitational tugging from orbiting planets. When a planet orbits a star, the star wobbles slightly toward and away from Earth, creating periodic shifts in its light spectrum. First proposed by Friedrich Wilhelm Bessel in the 19th century and successfully applied to exoplanet detection in 1995, this method has discovered nearly half of all known exoplanets.
源记录
引文逐字复制自方法源记录。这些引文不代表任何层级的验证。
Radial Velocity Exoplanet Detection Method
分类方法记录 · process-pipeline / applied-physics
- Mayor, M., & Queloz, D. (1995). A Jupiter-mass companion to a solar-type star. Nature, 378(6555), 355-359. · DOI 10.1038/378355a0
- Campbell, B., Walker, G. A., & Yang, S. (1988). A Search for Substellar Companions to Solar-type Stars. The Astrophysical Journal, 331, 902. · DOI 10.1086/166608
- Pepe, F., et al. (2014). Exoplanet research with the HARPS-N spectrograph at the Telescopio Nazionale Galileo. Astronomy & Astrophysics, 534, A58. · URL
精选声明
声明已持久化到证据分类账中，每个声明都有自己的评估。
尚无精选声明
当分类账中没有声明时，此视图不会自行创建声明评估。
相关方法
从方法图中生成，显示为机器建议的关系 — 不推断任何证据声明。