TrES-1b

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TrES-1b
Exoplanet Comparison TrES-1 b.png
Size comparison of TrES-1 with Jupiter.
Discovery [1] [2]
Discovered by TrES
Discovery site Teide Observatory, Lowell Observatory, Palomar Observatory
Discovery date24 August 2004
Transit
Orbital characteristics
0.03926+0.00058
−0.00060 AU
Eccentricity <0.012 [3]
3.03006973±0.00000018 [4] d
Inclination 88.2 ± 1
Semi-amplitude 106.7+2.9
−2.8 [3]
Star GSC 02652-01324
Physical characteristics
Mean radius
1.081+0.18−0.04 RJ
Mass 0.697+0.028
−0.027 [3] MJ
Mean density
642  kg/m3 (1,082  lb/cu yd)
0.52 g
Temperature 1,060 ± 50

    TrES-1b is an extrasolar planet approximately 523 light-years away in the constellation of Lyra (the Lyre). The planet's mass and radius indicate that it is a Jovian planet with a similar bulk composition to Jupiter. Unlike Jupiter, but similar to many other planets detected around other stars, TrES-1 is located very close to its star, and belongs to the class of planets known as hot Jupiters. The planet was discovered orbiting around GSC 02652-01324 (an orange dwarf star).

    Contents

    Detection and discovery

    TrES-1b was discovered by the Trans-Atlantic Exoplanet Survey by detecting the transit of the planet across its parent star using a 4-inch-diameter (100 mm) telescope. The discovery was confirmed by the Keck Observatory using the radial velocity method, which allowed its mass to be determined. [2]

    Transit

    On March 22, 2005, Astronomers using NASA's Spitzer Space Telescope took advantage of this fact to directly capture the infrared light of two previously detected planets orbiting outside our solar system. Their findings revealed the temperatures and orbits of the planets.

    Eclipse of TrES-1 in visible and infrared light (artist's conception) Ssc2005-09b.jpg
    Eclipse of TrES-1 in visible and infrared light (artist's conception)

    Upcoming Spitzer observations using a variety of infrared wavelengths may provide more information about the planets' winds and atmospheric compositions. It enabled determination of TrES-1's temperature, which is in excess of 1000 K (1340 °F). The planet's Bond albedo was found to be 0.31 ± 0.14. [5]

    In the infrared panel, the colors reflect what our eyes might see if we could retune them to the invisible, infrared portion of the light spectrum. The hot star is less bright in infrared light than in visible and appears fainter. The warm planet peaks in infrared light, so is shown brighter. Their hues represent relative differences in temperature. Because the star is hotter than the planet, and because hotter objects give off more blue light than red, the star is depicted in blue, and the planet, red.

    The overall look of the planet is inspired by theoretical models of hot, gas giant planets. These "hot Jupiters" are similar to Jupiter in composition and mass, but are expected to look quite different at such high temperatures.

    Radial velocity

    The transit light-curve signature in the course of the TrES multi-site transiting planet survey, and confirmed the planetary nature of the companion via multicolor photometry and precise radial velocity measurements. [1] [2] With this, the planet has an orbital period similar to that of HD 209458 b, but about twice as long as those of the Optical Gravitational Lensing Experiment (OGLE) transiting planets. Its mass is similar to that of HD 209458 b, but its radius is significantly smaller and fits the theoretical models without the need for an additional source of heat deep in the atmosphere, as has been invoked by some investigators for HD 209458 b.

    Rotation

    The spin-orbit angle using the Rossiter–McLaughlin effect [6] was measured to be +30±21° in 2007, [7] and measurement was not updated by 2012 [8]

    Physical characteristics

    Hubble might find water in TrES-1, and it would give a much more precise measurement of the planet's size, and even allow us to search for moons. A satellite is unlikely however, given the likely history and current orbital configuration for the planet, the research team concluded.

    There are only 11 exomoon candidates around 8 exoplanets, but some researchers have considered that such satellites would be logical places for life to exist around giant gaseous worlds that otherwise could not be expected to support biology.

    Models indicate that TrES-1 has undergone significant tidal heating in the past due to its eccentric orbit, but this does not appear to have inflated the planet's radius. [9]

    See also

    Related Research Articles

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    References

    1. 1 2 "Keck confirms transit planet" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. August 24, 2004. Retrieved August 14, 2019.
    2. 1 2 3 Alonso, Roi; et al. (2004). "TrES-1: The Transiting Planet of a Bright K0V Star". The Astrophysical Journal Letters. 613 (2): L153–L156. arXiv: astro-ph/0408421 . Bibcode:2004ApJ...613L.153A. doi:10.1086/425256. S2CID   8940599.
    3. 1 2 3 Bonomo, A. S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG . XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy and Astrophysics. 602. A107. arXiv: 1704.00373 . Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID   118923163.
    4. ↑ Baluev, Roman V.; et al. (2015). "Benchmarking the power of amateur observatories for TTV exoplanets detection". Monthly Notices of the Royal Astronomical Society. 450 (3): 3101–3113. arXiv: 1501.06748 . Bibcode:2015MNRAS.450.3101B. doi:10.1093/mnras/stv788. S2CID   15420110.
    5. ↑ Charbonneau; Allen, Lori E.; Megeath, S. Thomas; Torres, Guillermo; Alonso, Roi; Brown, Timothy M.; Gilliland, Ronald L.; Latham, David W.; et al. (2005). "Detection of Thermal Emission from an Extrasolar Planet". The Astrophysical Journal. 626 (1): 523–529. arXiv: astro-ph/0503457 . Bibcode:2005ApJ...626..523C. doi:10.1086/429991. S2CID   13296966.
    6. ↑ Joshua N. Winn (2008). "Measuring accurate transit parameters". Proceedings of the International Astronomical Union. 4: 99–109. arXiv: 0807.4929 . Bibcode:2009IAUS..253...99W. doi:10.1017/S174392130802629X. S2CID   34144676.
    7. ↑ Narita; et al. (August 25, 2007). "Measurement of the Rossiter-McLaughlin Effect in the Transiting Exoplanetary System TrES-1" (PDF). Publications of the Astronomical Society of Japan . 59 (4): 763–770. arXiv: astro-ph/0702707 . Bibcode:2007PASJ...59..763N. doi:10.1093/pasj/59.4.763. S2CID   15033371.
    8. ↑ 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
    9. ↑ Jackson; Greenberg, Richard; Barnes, Rory (July 10, 2008). "Tidal Heating of Extra-Solar Planets". The Astrophysical Journal. 681 (2): 1631–1638. arXiv: 0803.0026 . Bibcode:2008ApJ...681.1631J. doi:10.1086/587641. S2CID   42315630.

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