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TrES-4b

Coordinates:Sky map17h 53m 13s, +37° 12′ 42″
From Wikipedia, the free encyclopedia
Hot Jupiter exoplanet orbiting a Sun-like star
TrES-4b
Size comparison of TrES-4 with Jupiter
Discovery
Discovered byMandushevet al[1]
Discovery date2006–2007
Transit
Orbital characteristics
0.05091 ± 0.00071 AU (7.616 ± 0.106 million km)[2]
Eccentricity0
3.553945 ± 0.000075d
Inclination82.86 ± 0.33[2]
Semi-amplitude86.1
StarGSC 02620-00648 A[2]
Physical characteristics
1.838+0.240
−0.238
 RJ
[3]
Mass0.78±0.19 MJ[3]
0.156+0.072
−0.071
 g/cm3
[3]
7.04 ± 1.12 m/s2 (23.1 ± 3.7 ft/s2)
0.718 ± 0.114g
Temperature1,782±29 K (1,509 °C; 2,748 °F,equilibrium)[2]

TrES-4b is anexoplanet, one of thelargest exoplanets ever found. It was discovered in 2006, and announced in 2007, by theTrans-Atlantic Exoplanet Survey, using thetransit method. It is approximately 1,400light-years (430 pc) away orbiting the starGSC 02620-00648, in the constellationHercules.[1]

Orbit

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

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

The study in 2012, utilizing aRossiter–McLaughlin effect, have determined the planetary orbit is probably aligned with the equatorial plane of the star, misalignment equal to6.3±4.7°.[4]

Physical characteristics

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The planet is slightly less massive thanJupiter (0.919 ± 0.073MJ) 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 asSaturn's moonMethone. At the time of its discovery in 2007, TrES-4 was both the largest-known planet and the planet with the lowest-known density.[2][1]

TrES-4b's orbital radius is 0.05091AU, 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 theSun as well as theinternal heat within the planet.[2][1]

See also

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References

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  1. ^abcdMandushev, 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. ^abcdefgDaemgen, 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. ^abcJohns, 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.

External links

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Media related toTrES-4 at Wikimedia Commons


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