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TrES-2b / Kepler-1b
Exoplanet Comparison TrES-2 b.png
Size comparison of TrES-2b with Jupiter.
Discovered byO'Donovan et al.
Discovery siteCalifornia & Arizona, USA
Discovery dateAugust 21, 2006
confirmed September 8, 2006
Orbital characteristics
0.03556±0.00075 AU
2.47063±0.00001 d
StarGSC 03549-02811 A[2]
Physical characteristics
Mean radius
1.272±0.041[2] RJ
Mass1.199±0.052[2] MJ
3.284±0.016[2] g

TrES-2b (TrES-2 or Kepler-1b) is an extrasolar planet orbiting the star GSC 03549-02811 located 750 light years away from the Solar System. The planet has been identified in 2011 as the darkest known exoplanet, reflecting less than 1% of any light that hits it.[4] The planet's mass and radius indicate that it is a gas giant with a bulk composition similar to that of Jupiter. Unlike Jupiter, but similar to many planets detected around other stars, TrES-2b is located very close to its star, and belongs to the class of planets known as hot Jupiters. This system was within the field of view of the Kepler spacecraft.[1]

This planet continues to be studied by other projects and the parameters are being improved continuously. A 2007 study improved stellar and planetary parameters.[5] A 2008 study concluded that the TrES-2 system is a binary star system. This has a significant effect on the values for the stellar and the planetary parameters.[2]


The radial velocity of GSC 03549-02811 over time, caused by the presence of TrES-2 b.

TrES-2b was discovered on August 21, 2006 by the Trans-Atlantic Exoplanet Survey (TrES) by detecting the transit of the planet across its parent star using Sleuth (Palomar Observatory, California) and PSST (Lowell Observatory, Arizona), part of the TrES network of 10–cm telescopes. The discovery was confirmed by the W. M. Keck Observatory on September 8, 2006, by measuring the radial velocity of the star that hosts TrES-2b.[1]

Spin-orbit angle[edit]

In August 2008 more details of the relationship between the parent star and the orbit of the planet were published. The orbit was determined to be tilted by −9±12° from the stellar equator. The orbital direction was determined to be in the same direction as the star's rotation (prograde).[6]

The Kepler mission[edit]

NASA launched Kepler in March 2009. The spacecraft is dedicated to the discovery of extrasolar planets by the transit method from solar orbit. In April 2009 the project released the first light images from the spacecraft, and TrES-2b was one of two objects highlighted in these images. Although TrES-2b is not the only known exoplanet in the field of view of this spacecraft it is the only one identified in the first light images. This object is important for calibration and check-out.[7]

The GSC 03549-02811 system as seen from the Kepler spacecraft. (Celestial north is toward the lower left corner and the subject is in the center of the photograph as seen clearly in enlarged view.)

The Kepler mission also managed to detect the mass of the planet from Kepler data alone through the analysis of the light curve of the host star. In addition to detecting the planet directly, the planet was also detected by analysis of the star brightness caused by the gravitational tug of TrES-2b by shape distortion of the host star and by light variations due to Doppler beaming.[8]

Physical characteristics[edit]


An artist's impression of TrES-2b

The first important result from the Kepler Mission about TrES-2b is an extremely low geometric albedo measured in 2011, making it the darkest known exoplanet.[4] If the entire day–night contrast were due to geometric albedo, it would be 2.53%, but modeling suggests that much of this is dayside emission and the true albedo is much lower. It is estimated to be less than 1% and for best-fit model it is about 0.04%. This makes TrES-2b the darkest known exoplanet, reflecting less light than coal or black acrylic paint.[9] It is not clear why the planet is so dark. One reason could be an absence of reflective clouds such as those which make Jupiter so bright, due to TrES-2b's proximity to its parent star and the consequent high temperature. Another reason could be the presence in the atmosphere of light-absorbing chemicals such as vaporized sodium, potassium, or gaseous titanium oxide;[10] however, Kipping and Spiegel excluded heavy oxides of titanium and vanadium from their models, as it seems unrealistic that condensed, heavy compounds be present in the upper atmosphere. They also note that in general, hot Jupiters are expected to be dark, because "absorption due to the broad wings of the sodium and potassium D lines is thought to dominate their visible spectra", and, apart from that of Kepler-7b (38±12%), albedo measurements for hot Jupiters have generally given only upper limits.[4]


The planet is likely to be tidally locked to the parent star. In 2015, the planetary nightside temperature was estimated to be equal to 1885+51


  1. ^ a b c O'Donovan, Francis T.; et al. (2006). "TrES-2: The First Transiting Planet in the Kepler Field". The Astrophysical Journal Letters. 651 (1): L61–L64. arXiv:astro-ph/0609335. Bibcode:2006ApJ...651L..61O. doi:10.1086/509123.
  2. ^ a b c d e f 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.
  3. ^ a b A Comprehensive Study of Kepler Phase Curves and Secondary Eclipses:Temperatures and Albedos of Confirmed Kepler Giant Planets
  4. ^ a b c David M. Kipping & David S. Spiegel (2011). "Detection of visible light from the darkest world" (PDF). Monthly Notices of the Royal Astronomical Society. 417 (1): L88. arXiv:1108.2297. Bibcode:2011MNRAS.417L..88K. doi:10.1111/j.1745-3933.2011.01127.x. Archived from the original on March 17, 2012. Retrieved 2011-08-12.CS1 maint: unfit url (link)
  5. ^ Alessandro Sozzetti; Torres, Guillermo; Charbonneau, David; Latham, David W.; Holman, Matthew J.; Winn, Joshua N.; Laird, John B.; o’Donovan, Francis T. (August 1, 2007). "Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2". The Astrophysical Journal. 664 (2): 1190–1198. arXiv:0704.2938. Bibcode:2007ApJ...664.1190S. doi:10.1086/519214.
  6. ^ Winn, Joshua N.; Johnson, John Asher; Narita, Norio; Suto, Yasushi; Turner, Edwin L.; Fischer, Debra A.; Butler, R. Paul; Vogt, Steven S.; et al. (2008). "The Prograde Orbit of Exoplanet TrES-2b". The Astrophysical Journal. 682 (2): 1283–1288. arXiv:0804.2259. Bibcode:2008ApJ...682.1283W. doi:10.1086/589235.
  7. ^ "Kepler Eyes Cluster and Known Planet". NASA. 2009-04-16. Retrieved 2009-05-09.
  8. ^ Photometrically derived masses and radii of the planet and star in the TrES-2 system: Thomas Barclay, Daniel Huber, Jason F. Rowe, Jonathan J. Fortney, Caroline V. Morley, Elisa V. Quintana, Daniel C. Fabrycky, Geert Barentsen, Steven Bloemen, Jessie L. Christiansen, Brice-Olivier Demory, Benjamin J. Fulton, Jon M. Jenkins, Fergal Mullally, Darin Ragozzine, Shaun E. Seader, Avi Shporer, Peter Tenenbaum, Susan E. Thompson
  9. ^ Charles Q. Choi (2011-08-11). "Coal-Black Alien Planet Is Darkest Ever Seen". Archived from the original on 2012-06-10. Retrieved 2014-12-26.
  10. ^ Baldwin, Emily (2011-08-11). "Exoplanet blacker than coal". Astronomy Now. Archived from the original on 2011-09-18. Retrieved 2011-08-12.

External links[edit]

Coordinates: Sky map 19h 07m 14s, +49° 18′ 59″