HAT-P-7b
Size comparison of HAT-P-7b (gray) with Jupiter.
Discovery[1]
Discovered byHATNet Project
Discovery siteHAT-7 telescope at Fred Lawrence Whipple Observatory and HAT-8 at Mauna Kea Observatory
Discovery dateMarch 5, 2008
Transit
Designations
Kepler-2b, KOI-2.01[2]
Orbital characteristics
0.03813±0.00036 AU
Eccentricity<0.0040[3]
2.204737±0.000017[4] d
Inclination85.7+3.5
−3.1
StarHAT-P-7
Physical characteristics
Mean radius
1.64±0.11 RJ[5]
Mass1.806±0.036[3] MJ
Mean density
0.54 g cm−3
17.36 m/s2 (57.0 ft/s2)
1.77 g
Temperature2730+150
−100 K

    HAT-P-7b (or Kepler-2b) is an extrasolar planet discovered in 2008. It orbits very close to its host star and is larger and more massive than Jupiter. Due to the extreme heat that it receives from its star, the dayside temperature is predicted to be 2,630–2,880 K (4,270–4,720 °F; 2,360–2,610 °C) K, while nightside temperatures are 2,211–2,238 K (3,520–3,569 °F; 1,938–1,965 °C).[6] HAT-P-7b is also one of the darkest planets ever observed, with an albedo of less than 0.03—meaning it absorbs more than 97% of the visible light that strikes it.[7]

    Discovery

    The HATNet Project telescopes HAT-7, located at the Smithsonian Astrophysical Observatory's Fred Lawrence Whipple Observatory in Arizona, and HAT-8, installed on the rooftop of Smithsonian Astrophysical Observatory's Submillimeter Array building atop Mauna Kea, Hawaii, observed 33,000 stars in HATNet field G154, on nearly every night from late May to early August 2004. The light curves resulting from the 5140 exposures obtained were searched for transit signals and a very significant periodic drop in brightness was detected in the star GSC 03547–01402 (HAT-P-7), with a depth of approximately 7.0 millimagnitude, a period of 2.2047 days, and a duration of 4.1 hours.[1]

    Fortunately HAT-P-7 was located in the overlapping area between fields G154 and G155 allowing the transit to be independently confirmed by the HAT-6 (Arizona) and HAT-9 (Hawaii) telescopes which observed the neighboring field G155. Field G155 was observed from late July 2004 to late September 2005 gathering an additional 11,480 exposures for a total of 16,620 data points.[1]

    History

    The GSC 03547-01402 system was within the initial field of view of the Kepler Mission spacecraft,[1] which confirmed the transit and orbital properties of the planet with significantly improved confidence and observed occultation and light curve characteristics consistent with a strongly absorbing atmosphere with limited advection to the night side. In testing itself on HAT-P-7b, Kepler proved it was sensitive enough to detect Earth-like exoplanets.[8]

    On July 4, 2011, HAT-P-7b was the subject of the Hubble Space Telescope's one millionth scientific observation.[9]

    Physical characteristics

    In August 2009, it was announced that HAT-P-7b may have a retrograde orbit, based upon measurements of the Rossiter–McLaughlin effect.[10][11][12] This announcement came only a day after the announcement of the first planet discovered with such an orbit, WASP-17b. A study in 2012, utilizing the Rossiter–McLaughlin effect, determined the planetary orbit inclination with respect to the rotational axis of the star, equal to 155±37°.[13]

    In January 2010, it was announced that ellipsoidal light variations were detected for HAT-P-7b, the first detection of such kind. This method analyses the brightness variation caused by the rotation of a star as its shape is tidally distorted by the planet.[14]

    Weather

    In December 2016, a letter published in Nature Astronomy by Dr. David Armstrong and his colleagues described evidence of strong wind jets of variable speed on HAT-P-7b.[15] High variation in wind speed would explain similar variations in light reflected from HAT-P-7b's atmosphere. In particular, the brightest point on the planet shifts its phase or position on a timescale of only tens to hundreds of days, suggesting high variation in global wind speeds and cloud coverage. Condensation models of HAT-P-7b predict precipitation of Al2O3 (corundum) on the night side of the planet's atmosphere. The clouds themselves are likely made up of corundum, the mineral which forms rubies and sapphires.[15][16]

    See also

    References

    1. 1 2 3 4 Pál, A.; et al. (2008). "HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field". The Astrophysical Journal. 680 (2): 1450–1456. arXiv:0803.0746. Bibcode:2008ApJ...680.1450P. doi:10.1086/588010.
    2. ↑ "HAT-P-7b". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-24.
    3. 1 2 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.
    4. ↑ Morris, Brett M.; et al. (2013). "Kepler's Optical Secondary Eclipse of HAT-P-7b and Probable Detection of Planet-induced Stellar Gravity Darkening". The Astrophysical Journal Letters. 764 (2). L22. arXiv:1301.4503. Bibcode:2013ApJ...764L..22M. doi:10.1088/2041-8205/764/2/L22.
    5. ↑ Rhodes, Michael D.; Puskullu, Caglar; Budding, Edwin; Banks, Timothy S. (2020). "Exoplanet system Kepler-2 with comparisons to Kepler-1 and 13". Astrophysics and Space Science. 365 (4): 77. arXiv:2004.07971. Bibcode:2020Ap&SS.365...77R. doi:10.1007/s10509-020-03789-3. S2CID 215814387.
    6. ↑ A Comprehensive Study of Kepler Phase Curves and Secondary Eclipses:Temperatures and Albedos of Confirmed Kepler Giant Planets
    7. ↑ WASP-104b is Darker Than Charcoal
    8. ↑ Borucki, W. J.; et al. (2009-08-07). "Kepler's Optical Phase Curve of the Exoplanet HAT-P-7b". Science. 325 (5941): 709. Bibcode:2009Sci...325..709B. doi:10.1126/science.1178312. PMID 19661420. S2CID 206522122.
    9. ↑ NASA'S Hubble Makes One Millionth Science Observation
    10. ↑ Second backwards planet found, a day after the first
    11. ↑ Winn, Joshua N.; et al. (2009). "HAT-P-7: A Retrograde or Polar Orbit, and a Third Body". The Astrophysical Journal Letters. 703 (2): L99–L103. arXiv:0908.1672. Bibcode:2009ApJ...703L..99W. doi:10.1088/0004-637X/703/2/L99.
    12. ↑ Narita, Norio; et al. (2009). "First Evidence of a Retrograde Orbit of a Transiting Exoplanet HAT-P-7b". Publications of the Astronomical Society of Japan. 61 (5): L35–L40. arXiv:0908.1673. Bibcode:2009PASJ...61L..35N. doi:10.1093/pasj/61.5.L35.
    13. ↑ 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
    14. ↑ Welsh, William F.; et al. (2010). "The Discovery of Ellipsoidal Variations in the Kepler Light Curve of HAT-P-7". The Astrophysical Journal Letters. 713 (2): L145–L149. arXiv:1001.0413. Bibcode:2010ApJ...713L.145W. doi:10.1088/2041-8205/713/2/L145.
    15. 1 2 Armstrong, D. J.; et al. (2016). "Variability in the atmosphere of the hot giant planet HAT-P-7 b". Nature Astronomy. 1 (1). 0004. arXiv:1612.04225. Bibcode:2016NatAs...1E...4A. doi:10.1038/s41550-016-0004. S2CID 36668489.
    16. ↑ Pat Brennan (December 11, 2016). "Winds of rubies and sapphires strike the sky of giant planet". Exoplanets.nasa.gov. NASA. Retrieved May 22, 2019.
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