55 Cancri b

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55 Cancri b / Galileo
Jkv.55 Cnc b.png
Artist's impression of 55 Cancri b.
Discovery
Discovered by Butler, Marcy
Discovery site California, USA
Discovery dateApril 12, 1996
Radial velocity
Orbital characteristics
Apastron 0.116 AU (17,400,000 km)
Periastron 0.113 AU (16,900,000 km)
0.115 ± 0.0000011 AU (17,203,760 ± 160 km) [1]
Eccentricity 0.014 ± 0.008 [1]
14.65162 ± 0.0007 [1] d
0.04011325 y
Inclination ~85 [2] [3]
2,450,002.94749 ± 1.2 [1]
131.94 ± 30 [1]
Semi-amplitude 71.32 ± 0.41 [1]
Star 55 Cancri A
Physical characteristics
Mass 0.824 ± 0.007 [1] [2] MJ

    55 Cancri b (abbreviated 55 Cnc b), occasionally designated 55 Cancri Ab (to distinguish it from the star 55 Cancri B), also named Galileo, is an exoplanet orbiting the Sun-like star 55 Cancri A every 14.65 days. It is the second planet in order of distance from its star, and is an example of a hot Jupiter, or possibly rather "warm Jupiter". [4]

    Contents

    In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. [5] The process involved public nomination and voting for the new names. [6] In December 2015, the IAU announced the winning name was Galileo for this planet. [7] The winning name was submitted by the Royal Netherlands Association for Meteorology and Astronomy of the Netherlands. It honors early-17th century astronomer and physicist Galileo Galilei. [8]

    Discovery

    The radial velocity trend of 55 Cancri caused by the presence of 55 Cancri b. 55 Cnc b rv.pdf
    The radial velocity trend of 55 Cancri caused by the presence of 55 Cancri b.

    55 Cancri b was discovered in 1996 by Geoffrey Marcy and R. Paul Butler. It was the fourth known extrasolar planet, excluding pulsar planets. It was discovered by detecting variations in its star's radial velocity caused by the planet's gravity. By making sensitive measurements of the Doppler shift of the spectrum of 55 Cancri A, a 15-day periodicity was detected. The planet was announced in 1996, together with the planet of Tau Boötis and the innermost planet of Upsilon Andromedae. [9]

    Even when this inner planet, with a mass at least 78% times that of Jupiter was accounted for, the star still showed a drift in its radial velocity. This eventually led to the discovery of the outer planet 55 Cancri d in 2002.

    Orbit and mass

    55 Cancri b is in a short-period orbit, though not so extreme as that of the previously detected hot Jupiter 51 Pegasi b. The orbital period indicates that the planet is located close to a 1:3 mean motion resonance with 55 Cancri c, however investigations of the planetary parameters in a Newtonian simulation indicate that while the orbital periods are close to this ratio, the planets are not actually in the resonance. [1]

    In 2012, b's upper atmosphere was observed transiting the star; so its inclination is about 85 degrees, coplanar with 55 Cancri e. This helped to constrain the mass of the planet but the inclination was too low to constrain its radius. [2]

    The mass is about 0.85 that of Jupiter. [2]

    Characteristics

    55 Cancri b is a gas giant with no solid surface. The atmospheric transit has demonstrated hydrogen in the upper atmosphere. [2]

    That transit is so tangential, that properties such as its radius, density, and temperature are unknown. Assuming a composition similar to that of Jupiter and that its environment is close to chemical equilibrium, 55 Cancri b's upper atmosphere is predicted to be cloudless with a spectrum dominated by alkali metal absorption. [10]

    The atmosphere's transit indicates that it is slowly evaporating under the sun's heat. The evaporation is slower than that for previously studied (hotter) hot Jupiters. [4]

    The planet is unlikely to have large moons, since tidal forces would either eject them from orbit or destroy them on short timescales relative to the age of the system. [11]

    See also

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    References

    1. 1 2 3 4 5 6 7 8 DA Fischer; et al. (March 2008). "Five Planets Orbiting 55 Cancri". Astrophysical Journal. 675 (675): 790–801. arXiv: 0712.3917 . Bibcode:2008ApJ...675..790F. doi:10.1086/525512. S2CID   17083836.
    2. 1 2 3 4 5 Ehrenreich, David; Bourrier, Vincent; Bonfils, Xavier; Lecavelier des Étangs, Alain; Hébrard, Guillaume; Sing, David K.; Wheatley, Peter J.; Vidal-Madjar, Alfred; Delfosse, Xavier; Udry, Stéphane; Forveille, Thierry (2012-11-01). "Hint of a transiting extended atmosphere on 55 Cancri b". Astronomy & Astrophysics. 547: A18. arXiv: 1210.0531 . Bibcode:2012A&A...547A..18E. doi: 10.1051/0004-6361/201219981 . ISSN   0004-6361.
    3. ↑ D. Dragomir, 2012-08-27, referred to in Ehrenreich
    4. 1 2 "Astrophile: First puffy, 'warm Jupiter' spotted - space - 12 October 2012". New Scientist. Retrieved 2012-11-09.
    5. ↑ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
    6. ↑ "NameExoWorlds The Process". Archived from the original on 2015-08-15. Retrieved 2015-09-05.
    7. ↑ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
    8. ↑ "NameExoWorlds The Approved Names". Archived from the original on 2018-02-01. Retrieved 2015-12-27.
    9. ↑ Butler; Marcy, Geoffrey W.; Williams, Eric; Hauser, Heather; Shirts, Phil; et al. (1997). "Three New 51 Pegasi-Type Planets". The Astrophysical Journal. 474 (2): L115–L118. Bibcode:1997ApJ...474L.115B. doi: 10.1086/310444 .
    10. ↑ Sudarsky, D.; et al. (2003). "Theoretical Spectra and Atmospheres of Extrasolar Giant Planets". The Astrophysical Journal . 588 (2): 1121–1148. arXiv: astro-ph/0210216 . Bibcode:2003ApJ...588.1121S. doi:10.1086/374331. S2CID   16004653.
    11. ↑ Barnes, J.; O'Brien, D. (2002). "Stability of Satellites around Close-in Extrasolar Giant Planets". The Astrophysical Journal . 575 (2): 1087–1093. arXiv: astro-ph/0205035 . Bibcode:2002ApJ...575.1087B. doi:10.1086/341477. S2CID   14508244.
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