54 Piscium b

Last updated
54 Piscium b
Discovery [1]
Discovered by Fischer et al.
Discovery site Lick Observatory and Keck Observatory
Discovery date2003
Doppler spectroscopy
Orbital characteristics [2]
0.295±0.029  AU
Eccentricity 0.645±0.02
62.250±0.004 d
243±3 º
Semi-amplitude 16.6±0.6  m/s
Star 54 Piscium A
Physical characteristics [2]
Mass ≥0.228±0.011  MJ

    54 Piscium b (HD 3651 b), occasionally catalogued as 54 Piscium Ab to differentiate from the brown dwarf in the system, is an extrasolar planet [3] [1] approximately 36 light-years away [4] in the constellation of Pisces. It was discovered orbiting the orange dwarf star 54 Piscium. Its minimum mass is one-fifth that of Jupiter, and it orbits the star in a very eccentric orbit about every two months.

    Contents

    Discovery

    On January 16, 2003, a team of astronomers (led by Geoff Marcy) announced the discovery of an extrasolar planet around 54 Piscium using the radial velocity method, [1] a process utilizing the "wobbling" effect that a star may experience if something is tugging on it. The planet has been estimated to have a mass of only 20 percent that of Jupiter (making the planet around the same size and mass of Saturn).

    Orbit and mass

    An artist's impression of the brown dwarf (54 Piscium B) and the planet closer to its sun (54 Piscium b). LuhmanTStarCompanion (54 Psc).jpg
    An artist's impression of the brown dwarf (54 Piscium B) and the planet closer to its sun (54 Piscium b).

    The planet orbits its sun at a distance of 0.28 astronomical units (which would be within the orbit of Mercury), which takes approximately 62 days to complete. The planet has a high eccentricity of about 0.63. The highly elliptical orbit, however, suggested that the gravity of an unseen object farther away from the star was pulling the planet outward. The eccentric orbit became clear with the discovery of the brown dwarf within the system.

    Perturbation

    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 near the known planet’s apastron distance, near the 1:2 mean-motion resonance". Also, observation has ruled out Neptune-class or heavier planets with a period of one year or less; which still allows for Earth-sized planets at 0.6 AU or more. [6]

    See also

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    References

    1. 1 2 3 Fischer, Debra A.; et al. (2003). "A Sub-Saturn Mass Planet Orbiting HD 3651". The Astrophysical Journal. 590 (2): 1081–1087. Bibcode: 2003ApJ...590.1081F . doi: 10.1086/375027 .
    2. 1 2 Wittenmyer, Robert A.; et al. (2019). "Truly eccentric – I. Revisiting eight single-eccentric planetary systems". Monthly Notices of the Royal Astronomical Society. 484 (4): 5859–5867. arXiv: 1901.08471 . Bibcode:2019MNRAS.484.5859W. doi:10.1093/mnras/stz290.
    3. ↑ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv: astro-ph/0607493 . Bibcode: 2006ApJ...646..505B . doi: 10.1086/504701 .
    4. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
    5. ↑ square root of luminosity
    6. ↑ Wittenmyer, Robert A.; et al. (2007). "Dynamical and Observational Constraints on Additional Planets in Highly Eccentric Planetary Systems". The Astronomical Journal. 134 (3): 1276–1284. arXiv: 0706.1962 . Bibcode: 2007AJ....134.1276W . doi: 10.1086/520880 .
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