Transit Photometry
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.
Rekodi ya chanzo
Nukuu zimehamishwa kwa uhalisi kutoka kwa rekodi ya chanzo cha mbinu. Hakuna uthibitisho wa kiwango cha dai unaodokezwa kutoka kwao.
- Borucki, W. J., & Summers, A. L. (1984). The photometric method of detecting other planetary systems. Astrophysical Journal, 281, 537-553. · DOI 10.1016/0019-1035(84)90102-7
- Fressin, F., et al. (2013). The false positive rate for Kepler and the validation of Kepler objects of interest. Astrophysical Journal, 766(2), 81. · URL
- Charbonneau, D., Brown, T. M., Latham, D. W., & Mayor, M. (2000). Detection of planetary transits across a sun-like star. Astrophysical Journal, 529(1), L45-L48. · DOI 10.1086/312457
Madai yaliyotunzwa
Madai yamehifadhiwa katika daftari la ushahidi, kila moja ikiwa na tathmini yake.
Mwonekano huu haubuni tathmini ya dai wakati daftari haina yoyote.
Mbinu zinazohusiana
Zilizotengenezwa kutoka kwa grafu ya mbinu na kuonyeshwa kama uhusiano uliopendekezwa na mashine — hakuna dai la ushahidi linalodokezwa.