השוואת שיטות

	פוטומטריית מעברים	אסטרומטריה (היסט)	ספקטרוסקופיית מעבר של אקזופלנטות
תחום	אסטרונומיה	אסטרונומיה	אסטרונומיה
משפחה	Process / pipeline	Process / pipeline	Process / pipeline
שנת המקור	1984	1838	2002
הוגה השיטה	William Borucki	Friedrich Wilhelm Bessel	David Charbonneau
סוג	Observational photometric pipeline	Astrometric distance measurement	Spectroscopic observational method
מקור מכונן	Borucki, W. J., & Summers, A. L. (1984). The photometric method of detecting other planetary systems. Astrophysical Journal, 281, 537-553.	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	Charbonneau, D., Brown, T. M., Noyes, R. W., & Gilliland, R. L. (2002). Detection of an atmospheric trace constituent in the transmission spectrum of a distant extrasolar planet. Astrophysical Journal, 568(1), 377-384.
כינויים	Photometric Transit Method, Planetary Transit Detection	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Transmission Spectrum, Atmospheric Spectroscopy, Transit Spectroscopy
קשורות	3	3	3
תקציר	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.	Transmission spectroscopy is a technique for studying the atmospheres of exoplanets by analyzing the light passing through the planetary atmosphere during transit. Pioneered by David Charbonneau in 2002 with the detection of sodium in HD 209458b's atmosphere, this method has become the primary tool for characterizing exoplanet atmospheres and searching for biosignatures.