HAT-P-6b

Last updated
HAT-P-6b / Nachtwacht
Exoplanet Comparison HAT-P-6 b.png
Size comparison of HAT-P-6b with Jupiter.
Discovery
Discovered by Noyes et al.
Discovery dateOctober 15, 2007
transit
Orbital characteristics
0.05239+0.00080
−0.00082 AU [1]
Eccentricity <0.044 [1]
3.852985±0.000005 [2] d
Inclination 166±10 ° [3]
Star HAT-P-6
Physical characteristics
Mean radius
1.33 ± 0.06 RJ [2]
Mass 1.106+0.039
−0.040 [1] MJ
Mean density
583  kg/m3 (983  lb/cu yd) [1]

    HAT-P-6b is a transiting extrasolar planet discovered by Noyes et al. on October 15, 2007. [2] It is located approximately 910 light-years away [4] in the constellation of Andromeda, orbiting the star HAT-P-6. This hot Jupiter planet orbits with a semi-major axis of about 0.05 AU, and takes 92 hours, 28 minutes, 17 seconds to orbit the star. [2] It has true mass of 5.7% greater than Jupiter and a radius 33% greater than Jupiter, corresponding to a density of 0.583 g/cm3, which is less than water. [1]

    The planet HAT-P-6b is named Nachtwacht. The name was selected in the NameExoWorlds campaign by the Netherlands, during the 100th anniversary of the IAU, after Rembrandt's painting The Night Watch. [5] [6]

    The sky projected angle between stellar and orbital axis is roughly 166°, making it one of the few planets that is in a retrograde orbit around its parent star. [3] Observations made by Spitzer Space Telescope shows that the planet atmosphere has a weak temperature inversion, or no inversion at all, depending on how strong is the stellar chromospheric activity. [7]

    Artist's impression of Hat-P-6b orbiting its host star with an aurora on its south pole. Artistic impression HAT-P-6b.png
    Artist's impression of Hat-P-6b orbiting its host star with an aurora on its south pole.

    Related Research Articles

    HD 147506, also known as HAT-P-2 and formally named Hunor, is a magnitude 8.7 F8 dwarf star that is somewhat larger and hotter than the Sun. The star is approximately 419 light-years from Earth and is positioned near the keystone of Hercules. It is estimated to be 2 to 3 billion years old, towards the end of its main sequence life. There is one known transiting exoplanet, and a second planet not observed to transit.

    HAT-P-6 also named Sterrennacht is a star in the constellation Andromeda, located approximately 895 light years or 274 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than the Sun. The apparent magnitude of the star is +10.54, which means that it can only be visible through the telescope. The absolute magnitude of +3.36 is brighter than the Sun's +4.83, meaning that the star itself is brighter than the Sun. A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative.

    HD 118203 is a star with an orbiting exoplanet located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.

    <span class="mw-page-title-main">WASP-8b</span> Planet orbiting a star in a binary system in the constellation of Sculptor

    WASP-8b is an exoplanet orbiting the star WASP-8A in the constellation of Sculptor. The star is similar to the Sun and forms a binary star with a red dwarf star (WASP-8B) of half the Sun's mass that orbits WASP-8A 4.5 arcseconds away. The system is 294 light-years away and is therefore located closer to Earth than many other star systems that are known to feature planets similar to WASP-8b. The planet and its parent star were discovered in the SuperWASP batch -6b to -15b. On 1 April 2008, Dr. Don Pollacco of Queen's University Belfast announced them at the RAS National Astronomy Meeting.

    HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593.

    XO-4 is a star located approximately 896 light-years away from Earth in the Lynx constellation. It has a magnitude of about 11 and cannot be seen with the naked eye but is visible through a small telescope. A search for a binary companion star using adaptive optics at MMT Observatory was negative.

    CoRoT-6 is a magnitude 13.9 star located in the Ophiuchus constellation.

    <span class="mw-page-title-main">HAT-P-14b</span> Exoplanet in the constellation of Hercules

    HAT-P-14b, officially named Sissi also known as WASP-27b, is an extrasolar planet located approximately 224.2 ± 0.6 parsecs (731.2 ± 2.0 ly) away in the constellation of Hercules, orbiting the 10th magnitude F-type main-sequence star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project.

    <span class="mw-page-title-main">HD 15082</span> Star in the constellation Andromeda

    HD 15082 is a star located roughly 399 light years away in the northern constellation of Andromeda. The star is a Delta Scuti variable and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.

    HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

    HAT-P-29, also known as Muspelheim since 2019, is a star about 1,040 light-years away. It is a G-type main-sequence star. The star's age of 2.2±1.0 billion years is less than half that of the Sun. HAT-P-29 is slightly enriched in heavy elements, having 35% more iron than the Sun.

    BD+00 316 is an ordinary star with a close-orbiting planetary companion in the equatorial constellation of Cetus. It is also known as WASP-71 since 2019; BD+00 316 is the stellar identifier from the Bonner Durchmusterung catalogue. With an apparent visual magnitude of 10.56, it is too faint to be visible to the naked eye. This star is located at a distance of 1,160 light-years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 7.7 km/s.

    WASP-60 is a F-type main-sequence star about 1420 light-years away. The stars age is much younger than the Sun's at 1.7±0.5 billion years. WASP-60 is enriched in heavy elements, having 180% of the solar abundance of iron. The star does not have noticeable starspot activity, an unexpected observation for a relatively young star. The age of WASP-60 determined by different methods is highly discrepant though, and it may actually be an old star which experienced an episode of spin-up in the past.

    WASP-54, also known as BD+00 3088, is a binary star system about 825 light-years away. The primary, WASP-54A, is a F-type main-sequence star, accompanied by the red dwarf WASP-54B on a wide orbit. WASP-54 is depleted in heavy elements, having 55% of the solar abundance of iron. The age of WASP-54 is slightly older than the Sun's at 6.9+1.0
    −1.9     billion years.

    WASP-69, also named Wouri, is a K-type main-sequence star 164 light-years away. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.

    HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K. compared to the Sun, HAT-P-41 is enriched in heavy elements, with a metallicity Fe/H index of 0.21±0.10, but is much younger at an age of 2.2±0.4 billion years.

    References

    1. 1 2 3 4 5 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.
    2. 1 2 3 4 Noyes, R. W.; et al. (2008). "HAT-P-6b: A Hot Jupiter Transiting a Bright F Star". The Astrophysical Journal Letters. 673 (1): L79–L82. arXiv: 0710.2894 . Bibcode:2008ApJ...673L..79N. doi:10.1086/527358. S2CID   2301387.
    3. 1 2 Hébrard, Guillaume; Ehrenreich, David; Bouchy, François; Delfosse, Xavier; Moutou, Claire; Arnold, Luc; Boisse, Isabelle; Bonfils, Xavier; Díaz, Rodrigo F.; Eggenberger, Anne; Forveille, Thierry; Lagrange, Anne-Marie; Lovis, Christophe; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Santerne, Alexandre; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Vidal-Madjar, Alfred (2011). "The retrograde orbit of the HAT-P-6b exoplanet". Astronomy and Astrophysics. 527: L11. arXiv: 1101.5009 . Bibcode:2011A&A...527L..11H. doi:10.1051/0004-6361/201016331. S2CID   56130884.
    4. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
    5. ↑ "Approved names". NameExoworlds. Retrieved 2020-01-02.
    6. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
    7. ↑ Todorov, Kamen O.; Deming, Drake; Knutson, Heather A.; Burrows, Adam; Sada, Pedro V.; Cowan, Nicolas B.; Agol, Eric; Desert, Jean-Michel; Fortney, Jonathan J.; Charbonneau, David; Laughlin, Gregory; Langton, Jonathan; Showman, Adam P.; Lewis, Nikole K.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2012). "Warm Spitzer Observations of Three Hot Exoplanets: XO-4b, HAT-P-6b, and HAT-P-8b". The Astrophysical Journal. 746 (1): 111. arXiv: 1111.5858 . Bibcode:2012ApJ...746..111T. doi:10.1088/0004-637X/746/1/111. S2CID   119200344.

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