HD 40307 b

Last updated
HD 40307 b
Discovery
Discovered by Mayor et al.
Discovery site La Silla Observatory, Chile
Discovery date18 June 2008
radial velocity, using HARPS
Orbital characteristics
0.0468+0.0492
−0.0445 [1] AU
Eccentricity 0.20+0.25
−0.04 [1]
4.3115 ± 0.0006 [2] d
Semi-amplitude 1.94+2.25
−1.67 [1]
Star HD 40307

    HD 40307 b is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus, in June 2008. It is the second smallest of the planets orbiting the star, after HD 40307 e. [1] The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

    Contents

    Discovery

    As with many other extrasolar planets, HD 40307 b was discovered by measuring variations in the radial velocity of the star it orbits. These measurements were made by the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph at the Chile-based La Silla Observatory. The discovery was announced at the astrophysics conference that took place in Nantes, France between 16 and 18 June 2008. [3] HD 40307 b was one of three found here at the time. [4]

    Orbit and mass

    HD 40307 b is the second lightest planet discovered in the system, with at least 4.2 times the mass of the Earth. [1] The planet orbits the star HD 40307 every 4.3 Earth days, [4] corresponding of its location at approximately 0.047 astronomical units from the star. [5] The eccentricity of the planet's orbit was found to not differ significantly from zero, meaning that there is insufficient data to distinguish the orbit from an entirely circular one. [2]

    The star around which HD 40307 b orbits has a low metallicity, compared to other planet-bearing stars. This supports a hypothesis concerning the possibility that the metallicity of stars during their births may determine whether a protostar's accretion disk forms gas giants or terrestrial planets. [2]

    The Arizonan astronomer Rory Barnes's mathematical model, in 2009, found that "Planet b’s orbit must be more than 15◦ from face-on"; [6] however it cannot be much more. [1]

    Characteristics

    A Trio of Super-Earths (artist's impression).jpg
    A Trio of Super-Earths (artist's impression).jpg
    HD 40307 b. Artist impression

    HD 40307 b does not transit [1] and has not been imaged. More specific characteristics, such as its radius, composition, and possible surface temperature cannot be determined. [7]

    With a lower mass bound of 4.2 times the mass of the Earth, HD 40307 b is presumably too small to be a jovian planet. [4] This concept was challenged in a 2009 study, which stated that if HD 40307 b is terrestrial, the planet would be highly unstable and would be affected by tidal heating in a manner greater than Io, a volcanic satellite of planet Jupiter; restrictions that seem to bind terrestrial planets, however, do not restrict ice giant planets like Neptune or Uranus. [6]

    As strong tidal forces often result in the destruction of larger natural satellites in planets orbiting close to a star, it is unlikely that HD 40307 b hosts any satellites. [8]

    HD 40307 b, c, and d are presumed to have migrated into their present orbits. [6]

    Trivia

    The planet was named "Good Planet" in the Xkcd strip "Exoplanet Names" in August, 2013. [9]

    See also

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    <span class="mw-page-title-main">HD 40307</span> Star in the constellation Pictor

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    HD 40307 c is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the HARPS apparatus, in June 2008. Of the six proposed planets in the HD 40307 star system, it is the third-largest, and has the second-closest orbit from the star. The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

    HD 40307 d is an extrasolar planet orbiting the star HD 40307, located 42 light-years from Earth in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the HARPS apparatus in June 2008. It is the most massive of the six proposed planets in the system. The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

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    <span class="mw-page-title-main">HD 40307 g</span> Exoplanet candidate in the constellation of Pictor

    HD 40307 g is an exoplanet candidate suspected to be orbiting in the habitable zone of HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany.

    HD 40307 e is an extrasolar planet candidate suspected to be orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany.

    HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Göttingen, Germany. The existence of planet was confirmed in 2015.

    References

    1. 1 2 3 4 5 6 7 Tuomi, Mikko; Anglada-Escudé, Guillem; Gerlach, Enrico; Jones, Hugh R. A.; Reiners, Ansgar; Rivera, Eugenio J.; Vogt, Steven S.; Butler, R. Paul (17 December 2012). "Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307". Astronomy & Astrophysics. 549: A48. arXiv: 1211.1617 . Bibcode:2013A&A...549A..48T. doi:10.1051/0004-6361/201220268. S2CID   7424216.
    2. 1 2 3 M. Mayor; S. Udry; C. Lovis; F. Pepe; D. Queloz; W. Benz; et al. (2009). "The HARPS search for southern extra-solar planets. XIII. A planetary system with 3 Super-Earths (4.2, 6.9, & 9.2 Earth masses)". Astronomy and Astrophysics. 493 (2): 639–644. arXiv: 0806.4587 . Bibcode:2009A&A...493..639M. doi:10.1051/0004-6361:200810451. S2CID   116365802.
    3. ↑ Mayor; et al. (2008-06-16). "Trio of 'super-Earths' discovered". BBC News. Retrieved 2008-06-16.
    4. 1 2 3 Bryner, Jeanna (June 16, 2008). "3 super-Earths found around one star". NBC News. Retrieved 2008-10-30.
    5. ↑ "Notes for Planet HD 40307 b". Extrasolar Planets Encyclopaedia. Paris Observatory. 2008. Retrieved 2008-10-30.
    6. 1 2 3 Barnes, R.; Jackson, B.; Raymond, S.; West, A.; Greenberg, R. (2009). "The HD 40307 Planetary System: Super-Earths or Mini-Neptunes?". The Astrophysical Journal . 695 (2): 1006–1011. arXiv: 0901.1698 . Bibcode:2009ApJ...695.1006B. doi:10.1088/0004-637X/695/2/1006. S2CID   18849636.
    7. ↑ Characterizing Extrasolar Planets, Timothy M. Brown, chapter 3, Extrasolar Planets: XVI Canary Islands Winter School of Astrophysics, edited by Hans Deeg, Juan Antonio Belmonte, and Antonio Aparicio, Cambridge, UK: Cambridge University Press, 2007, ISBN   0-521-86808-4.
    8. ↑ 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.
    9. ↑ "Exoplanet Names".

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