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  • 21 Aug, 2019

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WASP-14b

WASP-14b is an extrasolar planet discovered in 2008 by SuperWASP using the transit method. Follow-up radial velocity measurements showed that the mass of WASP-14b is almost eight times larger than that of Jupiter. The radius found by the transit observations show that it has a radius 25% larger than Jupiter. This makes WASP-14b one of the densest exoplanets known. Its radius best fits the model of Jonathan Fortney.

Orbit

First calculation of WASP-14b's Rossiter–McLaughlin effect and so spin-orbit angle was −14 ± 17 degrees. It is too eccentric for its age and so is possibly pulled into its orbit by another planet. The study in 2012 has updated spin-orbit angle to 33.1±7.4°.

References

  1. ^ Joshi, Y. C.; et al. (2008). "WASP-14b: A 7.7 Mjup transiting exoplanet in an eccentric orbit". Monthly Notices of the Royal Astronomical Society. 392 (4): 1532–1538. arXiv:0806.1478. Bibcode:2009MNRAS.392.1532J. doi:10.1111/j.1365-2966.2008.14178.x. S2CID 7775011.
  2. ^ Fortney; Marley, M. S.; Barnes, J. W. (2007). "Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits". The Astrophysical Journal. 659 (2): 1661–1672. arXiv:astro-ph/0612671. Bibcode:2007ApJ...659.1661F. doi:10.1086/512120. S2CID 3039909.
  3. ^ Winn, Joshua N. (2008). "Measuring accurate transit parameters". Proceedings of the International Astronomical Union. 4: 99–109. arXiv:0807.4929v2. Bibcode:2009IAUS..253...99W. doi:10.1017/S174392130802629X. S2CID 34144676.
  4. ^ Albrecht, Simon; Winn, Joshua N.; Johnson, John A.; Howard, Andrew W.; Marcy, Geoffrey W.; Butler, R. Paul; Arriagada, Pamela; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B.; Hirano, Teruyuki; Bakos, Gaspar; Hartman, Joel D. (2012), "Obliquities of Hot Jupiter Host Stars: Evidence for Tidal Interactions and Primordial Misalignments", The Astrophysical Journal, 757 (1): 18, arXiv:1206.6105, Bibcode:2012ApJ...757...18A, doi:10.1088/0004-637X/757/1/18, S2CID 17174530

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