HD 40307 c

HD 40307 c
Exoplanet List of exoplanets
Parent star
Star HD 40307
Constellation Pictor
Right ascension (α) 05h 54m 04.2409s[1]
Declination (δ) −60° 01′ 24.498″[1]
Apparent magnitude (mV) 7.17[1]
Distance41.8 ± 0.3 ly
(12.83 ± 0.09[1] pc)
Spectral type K2.5V[1]
Mass (m) 0.75+0.03
−0.04[2] M☉
Radius (r) 0.716 ± 0.010[3] R☉
Temperature (T) 4977 ± 59[4] K
Metallicity [Fe/H] −0.31 ± 0.03[4]
Age 1.2 (≥ 0.2)[2] Gyr
Orbital elements
Semi-major axis(a) 0.07990.07590.0839[5] AU
Eccentricity (e) 0.0500.13[5]
Orbital period(P) 9.61849.61359.6234[5] d
Semi-amplitude (K) 2.452.172.75[5] m/s
Physical characteristics
Minimum mass(m sin i)6.65.67.7[5] M⊕
Discovery information
Discovery date June 16, 2008
Discoverer(s) Mayor et al.
Discovery method radial velocity, using HARPS
Discovery site La Silla Observatory, Chile
Discovery status Confirmed[5]
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

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.[5] 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.

Discovery

Like the other two exoplanets, HD 40307 b and HD 40307 d, orbiting the star HD 40307, HD 40307 c was discovered by measuring variations in the radial velocity of HD 40307 caused by the star's orbit around the center of mass of the planetary system. These measurements were made by the High Accuracy Radial Velocity Planet Searcher spectrograph apparatus (HARPS) at the La Silla Observatory in Chile's Atacama Desert.[6] The discovery of planets in the HD 40307 system was announced in an astrophysics convention that took place in Nantes, France in mid-June 2008.[6]

Orbit and mass

HD 40307 c is the third-most massive planet in the system, with a lower mass bound 6.8 times the mass of the Earth.[5] The planet orbits HD 40307 at about 0.08 astronomical units (AU), as compared to the Earth's distance from the Sun at 1 AU; as a result, one year on the planet constitutes approximately 9.6 Earth days. Analysis of the radial velocity data used to detect the planet does not yield a statistically significant deviation from a circular orbit.[4]

The star around which the planet HD 40307 orbits has a low metallicity, unusual when 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.[4]

Characteristics

HD 40307 c has not been observed directly and likely does not transit.[5] More specific characteristics (such as surface temperature, composition and radius) cannot be determined.[7]

HD 40307 c has a small mass of at least 6.9 times Earth's, so it was first assumed terrestrial. Later in 2009 a study stated that if HD 40307 c is terrestrial, tidal heating would destabilise it, in a manner greater than this process crushes the Jovian moon Io. Such restrictions as bind terrestrial planets would not restrict ice giant planets like Neptune or Uranus. HD 40307 c might be a sub-Neptune.[8]

Since the same tides are predicted to result in the destruction of larger natural satellites of planets located close to their parent star,[9] it is unlikely that HD 40307 c hosts any satellites.

See also

References

  1. 1 2 3 4 5 "HD 40307". SIMBAD. Centre de Données astronomiques de Strasbourg. 2008. Retrieved 18 June 2008.
  2. 1 2 HD 40307, database entry, Geneva-Copenhagen Survey of Solar neighbourhood, J. Holmberg et al., 2007, CDS database V/117A, accessed November 19, 2008; described in The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14 000 F and G dwarfs, B. Nordström, M. Mayor, J. Andersen, J. Holmberg, F. Pont, B. R. Jørgensen, E. H. Olsen, S. Udry, and N. Mowlavi, Astronomy and Astrophysics 418 (May 2004), pp. 989–1019, Bibcode: 2004A&A...418..989N, doi:10.1051/0004-6361:20035959.
  3. ↑ HD 40307, entry, CDS database J/A+A/450/735; described in Effective temperature scale and bolometric corrections from 2MASS photometry, E. Masana, C. Jordi, and I. Ribas, Astronomy and Astrophysics 450, #2 (May 2006), pp. 735–746. Bibcode: 2006A&A...450..735M. doi:10.1051/0004-6361:20054021.
  4. 1 2 3 4 M. Mayor; S. Udry; C. Lovis; F. Pepe; D. Queloz; W. Benz; J.-L. Bertaux; F. Bouchy; C. Mordasini; D. Segransan (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:0806.4587Freely accessible. Bibcode:2009A&A...493..639M. doi:10.1051/0004-6361:200810451.
  5. 1 2 3 4 5 6 7 8 9 Tuomi, Mikko; Anglada-Escude, Guillem; Gerlach, Enrico; Jones, Hugh R. R.; Reiners, Ansgar; Rivera, Eugenio J.; Vogt, Steven S.; Butler, R. Paul (2012). "Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307". arXiv:1211.1617v1Freely accessible [astro-ph].
  6. 1 2 Mayor; et al. (2008-06-16). "Trio of 'super-Earths' discovered". BBC news. Retrieved 2008-06-16.
  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, 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. arXiv:0901.1698Freely accessible. Bibcode:2009ApJ...695.1006B. doi:10.1088/0004-637X/695/2/1006.
  9. ↑ 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/0205035Freely accessible. Bibcode:2002ApJ...575.1087B. doi:10.1086/341477.

External links

Coordinates: 05h 54m 04.2409s, −60° 01′ 24.498″

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