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TrES-4b is an exoplanet. It was discovered in 2006, and announced in 2007, by the Trans-Atlantic Exoplanet Survey, using the transit method. At the time of its discovery TrES-4 was the largest confirmed exoplanet ever found; now more than 10 larger planets have been discovered. It is approximately 1,400 light-years (430 pc) away orbiting the star GSC 02620-00648, in the constellation Hercules.[1]

Orbit

TrES-4 orbits its primary star every 3.543 days and eclipses it when viewed from Earth.

A 2008 study concluded that the GSC 02620-00648 system (among others) is a binary star system allowing even more accurate determination of stellar and planetary parameters.[2]

The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is probably aligned with the equatorial plane of the star, misalignment equal to 6.3±4.7°.[5]

Physical characteristics

The planet is slightly less massive than Jupiter (0.919 ± 0.073 MJ) but its diameter is 84% larger. This give TrES-4 an average density of only about a third of a gram per cubic centimetre, approximately the same as Saturn‘s moon Methone. At the time of its discovery in 2007, TrES-4 was described as both the largest known planet and the planet with the lowest known density.[2][1]

TrES-4b’s orbital radius is 0.05091 AU, giving it a predicted surface temperature of about 1,782 K (1,509 °C; 2,748 °F). This by itself is not enough to explain the planet’s low density, however. It is not currently known why TrES-4b is so large. The probable causes are the proximity to a parent star that is three to four times more luminous than the Sun as well as the internal heat within the planet.[2][1]

See also

References

  1. ^ a b c d Mandushev, Georgi; et al. (2007). “TrES-4: A Transiting Hot Jupiter of Very Low Density”. The Astrophysical Journal Letters. 667 (2): L195–L198. arXiv:0708.0834. Bibcode:2007ApJ…667L.195M. doi:10.1086/522115. S2CID 6087170.
  2. ^ a b c d e f g Daemgen, S.; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T. (2009). “Binarity of transit host stars – Implications for planetary parameters” (PDF). Astronomy and Astrophysics. 498 (2): 567–574. arXiv:0902.2179. Bibcode:2009A&A…498..567D. doi:10.1051/0004-6361/200810988. S2CID 9893376.
  3. ^ a b Johns, Daniel; Marti, Connor; Huff, Madison; McCann, Jacob; Wittenmyer, Robert A.; Horner, Jonathan; Wright, Duncan J. (2018-11-01). “Revised Exoplanet Radii and Habitability Using Gaia Data Release 2”. The Astrophysical Journal Supplement Series. 239 (1): 14. arXiv:1808.04533. Bibcode:2018ApJS..239…14J. doi:10.3847/1538-4365/aae5fb. ISSN 0067-0049.
  4. ^ Sozzetti, A.; Bonomo, A. S.; Biazzo, K.; Mancini, L.; Damasso, M.; Desidera, S.; Gratton, R.; Lanza, A. F.; Poretti, E.; Rainer, M.; Malavolta, L.; Affer, L.; Barbieri, M.; Bedin, L. R.; Boccato, C.; Bonavita, M.; Borsa, F.; Ciceri, S.; Claudi, R. U.; Gandolfi, D.; Giacobbe, P.; Henning, T.; Knapic, C.; Latham, D. W.; Lodato, G.; Maggio, A.; Maldonado, J.; Marzari, F.; Fiorenzano, A. F.; Micela, G.; Molinari, E.; Mordasini, C.; Nascimbeni, V.; Pagano, I.; Pedani, M.; Pepe, F.; Piotto, G.; Santos, N.; Scandariato, G.; Shkolnik, E.; Southworth, J. Martinez (2015). “The GAPS programme with HARPS-N at TNG VI. The curious case of TrES-4b”. Astronomy & Astrophysics. 575 L15(2015): 1–10. doi:10.1051/0004-6361/201425570.
  5. ^ 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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