TrES-4b

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TrES-4b
TrES-4.jpg
Size comparison of TrES-4 with Jupiter
Discovery
Discovered by Mandushev et al [1]
Discovery date2006–2007
Transit
Orbital characteristics
0.05091 ± 0.00071 AU (7.616 ± 0.106 million km) [2]
Eccentricity 0
3.553945 ± 0.000075 d
Inclination 82.86 ± 0.33 [2]
Semi-amplitude 86.1
Star GSC 02620-00648 A [2]
Physical characteristics
1.838+0.240
−0.238  RJ [3]
Mass 0.78±0.19  MJ [3]
Mean density
0.156+0.072
−0.071  g/cm3 [3]
7.04 ± 1.12  m/s2 (23.1 ± 3.7  ft/s2)
0.718 ± 0.114 g
Temperature 1,782±29  K (1,509 °C; 2,748 °F, equilibrium) [2]

    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]

    Contents

    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°. [4]

    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. 1 2 3 4 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. 1 2 3 4 5 6 7 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. 1 2 3 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. ↑ 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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