HD 40307 d is an extrasolar planet orbiting the starHD 40307, located 42 light-years from Earth in the direction of the southern constellationPictor. 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.[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.
HD 40307 d has a mass of at least 9.2 times Earth's; assuming that all planets in the system have coplanar orbits, it is the most massive planet known in the system.[1] The planet orbits approximately 0.135 astronomical units from its primary star, as compared to Earth's orbit at approximately one astronomical unit away from the Sun. As a result, one year on HD 40307 d constitutes approximately 20.45 Earth days. 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.[3]
The star around which HD 40307 d orbits has an unusually low metallicity compared to that of 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.[3]
Characteristics
The planet has not been found to transit and, further, it is not likely to.[1] It has also not been imaged. More specific physical characteristics such as radius, composition, and average surface temperature cannot be observed.[4]
A dynamical study of planets b, c, and d showed tidal effects at least on b and c, to the extent that b had to be a sub-Neptune. All the planets from b to at least f must have migrated inward. That study implied that d was a sub-Neptune as well.[5]
As such 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 d hosts any satellites.[6]
^ abcdefTuomi, 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. S2CID7424216.
^ abM. 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:0806.4587. Bibcode:2009A&A...493..639M. doi:10.1051/0004-6361:200810451. S2CID116365802.
^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, ISBN0-521-86808-4.
