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  2. Doppler spectroscopy - Wikipedia

    en.wikipedia.org/wiki/Doppler_spectroscopy

    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 ...

  3. Methods of detecting exoplanets - Wikipedia

    en.wikipedia.org/wiki/Methods_of_detecting_exo...

    Until around 2012, the radial-velocity method (also known as Doppler spectroscopy) was by far the most productive technique used by planet hunters. (After 2012, the transit method from the Kepler space telescope overtook it in number.)

  4. Minimum mass - Wikipedia

    en.wikipedia.org/wiki/Minimum_mass

    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 ...

  5. HD 154857 c - Wikipedia

    en.wikipedia.org/wiki/HD_154857_c

    The first signs of this planet were noticed on 9 February 2007 by O’Toole in Australia using the method Doppler spectroscopy, along with HD 23127 b and HD 159868 b. The orbit had not yet been completely observed, so the values quoted were lower limits. The previously unconstrained orbital period and minimum mass were constrained in January 2014.

  6. HD 102956 b - Wikipedia

    en.wikipedia.org/wiki/HD_102956_b

    HD 102956 b or Isagel is an extrasolar planet discovered in 2010 by a team of American astronomers led by John Johnson using Doppler spectroscopy and the Keck Observatory in Hawaii. HD 102956 b is in the orbit of host star HD 102956.

  7. HD 222582 b - Wikipedia

    en.wikipedia.org/wiki/HD_222582_b

    Doppler spectroscopy: Orbital characteristics; Semi-major axis. ... The orbital period is 572 days and orbits at a semimajor axis of 1.35 AU in one of the most ...

  8. 14 Andromedae b - Wikipedia

    en.wikipedia.org/wiki/14_Andromedae_b

    The preprint announcing 14 Andromedae b was submitted to the arXiv electronic repository on July 2, 2008, by Bun'ei Sato and collaborators, who discovered it using the Doppler Spectroscopy method, during the Okayama Planet Search radial velocity survey of G and K giants at Okayama Astrophysical Observatory.

  9. 54 Piscium Ab - Wikipedia

    en.wikipedia.org/wiki/54_Piscium_Ab

    The orbit of an Earth-like planet would need to be centered within 0.68 AU [5] (around the orbital distance of Venus), which in a Keplerian system means a 240-day orbital period. In a 2006 simulation with the brown dwarf, 54 Piscium b's orbit "sweeps clean" most test particles within 0.5 AU, leaving only asteroids "in low-eccentricity orbits ...