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| Paralaksa astrometryczna (Paralaksa)× | Spektroskopia transmisyjna egzoplanet× | |
|---|---|---|
| Dziedzina | Astronomia | Astronomia |
| Rodzina | Process / pipeline | Process / pipeline |
| Rok powstania≠ | 1838 | 2002 |
| Twórca≠ | Friedrich Wilhelm Bessel | David Charbonneau |
| Typ≠ | Astrometric distance measurement | Spectroscopic observational method |
| Źródło pierwotne≠ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ | 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. DOI ↗ |
| Inne nazwy | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method | Transmission Spectrum, Atmospheric Spectroscopy, Transit Spectroscopy |
| Pokrewne | 3 | 3 |
| Podsumowanie≠ | 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. |
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