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Doppler spectroscopy (also known as the radial-velocity method, or colloquially, the wobble method) is an indirect method for finding extrasolar planets and brown dwarfs from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star. As of November 2022, about 19.5% of known extrasolar planets ...
Minimum mass is a widely cited statistic for extrasolar planets detected by the radial velocity method or Doppler spectroscopy, and is determined using the binary mass function. This method reveals planets by measuring changes in the movement of stars in the line-of-sight , so the real orbital inclinations and true masses of the planets are ...
Download as PDF; Printable version; ... Doppler spectroscopy: Orbital characteristics; Semi-major axis ... Orbital period (sidereal) 219 d: Time of periastron. 1189.3 ...
Download as PDF; Printable version; ... Doppler Spectroscopy: Orbital characteristics; Apastron: ... It is believed to have almost no orbital eccentricity. [1] See also
Download as PDF; Printable version; In other projects Wikidata item; Appearance. ... Doppler Spectroscopy: Orbital characteristics [1] Apastron: 1.412 AU (211,200,000 km)
HD 65216 b is an extrasolar planet located approximately 115 light-years away [3] in the constellation of Carina, orbiting the star HD 65216.This planet was discovered by the Geneva Extrasolar Planet Search Team in 2003.
HD 111232 b is an extrasolar planet that orbits at almost 2 AU with a minimum mass of 6.8 times that of Jupiter.This planet was discovered in the La Silla Observatory by Michel Mayor using the CORALIE spectrograph on 30 June 2003, along with six other planets, including HD 41004 Ab, HD 65216 b, HD 169830 c, HD 216770 b, HD 10647 b, and HD 142415 b.
HD 168443 b is a planet with a minimum mass seven times as that of Jupiter.Given the high mass, this planet is likely to be a gas giant, or possibly a small brown dwarf depending on the orbital inclination.