HAT-P-12b

Last updated
HAT-P-12b / Puli
Exoplanet Comparison HAT-P-12 b.png
Size comparison of HAT-P-12b with Jupiter.
Discovery [1]
Discovered by Hartman et al.
Discovery site Cambridge, Massachusetts
Discovery dateApril 29, 2009
Transit
Designations
Puli [2]
Orbital characteristics
0.0384 ± 0.0003 AU (5,745,000 ± 45,000 km) [1]
Eccentricity 0 (assumed) [1]
3.2130598 ± 0.0000021 [1] d
Inclination 89.0 ± 0.4 [1]
Star HAT-P-12
Physical characteristics
Mean radius
0.959 ± 0.029 [1] RJ
Mass 0.211 ± 0.012 [1] MJ
Mean density
295 ± 25  kg/m3 (497 ± 42  lb/cu yd) [1]

    HAT-P-12b, formally named Puli, [2] is an extrasolar planet approximately 468 light years away from Earth, orbiting the 13th magnitude K-type star HAT-P-12, which is located in Canes Venatici constellation. It is a transiting hot Jupiter that was discovered by the HATNet Project on April 29, 2009.

    HAT-P-12b is a H/He-dominated gas giant planet with a core mass of 11.3+2.6
    −2.1     M🜨 and is moderately irradiated by its low-metallicity host star. [3] Therefore, HAT-P-12b is most likely an H/He-dominated planet with a core of perhaps ~10 M🜨, and a total metal fraction of ~15%. This makes HAT-P-12b the least massive H/He-dominated gas giant planet found to date; the previous record holder was Saturn. [1]

    In 2020, the obtained transmission spectra have revealed that the atmosphere of HAT-P-12b is cloudy, [4] with haze above cloud tops. Water was detected. [5] The prevalence of clouds and hazes in planetary atmosphere was disputed in 2021 though. [6]

    In August 2022, this planet and its host star were included among 20 systems to be named by the third NameExoWorlds project. [7] The approved names, proposed by a team from Hungary, were announced in June 2023. HAT-P-12b is named Puli and its host star is named Komondor, after the Hungarian Puli and Komondor dog breeds. [2]

    Comparison of "hot Jupiter" exoplanets (artist concept). From top left to lower right: WASP-12b, WASP-6b, WASP-31b, WASP-39b, HD 189733b, HAT-P-12b, WASP-17b, WASP-19b, HAT-P-1b and HD 209458b. Clear to cloudy hot Jupiters.jpg
    Comparison of "hot Jupiter" exoplanets (artist concept).
    From top left to lower right: WASP-12b, WASP-6b, WASP-31b, WASP-39b, HD 189733b, HAT-P-12b, WASP-17b, WASP-19b, HAT-P-1b and HD 209458b.

    Related Research Articles

    <span class="mw-page-title-main">Gliese 436 b</span> Hot Neptune exoplanet orbiting Gliese 436

    Gliese 436 b is a Neptune-sized exoplanet orbiting the red dwarf Gliese 436. It was the first hot Neptune discovered with certainty and was among the smallest-known transiting planets in mass and radius, until the much smaller Kepler exoplanet discoveries began circa 2010.

    <span class="mw-page-title-main">HAT-P-3b</span> Jovian-sized exoplanet orbiting HAT-P-3

    HAT-P-3b, also named Teberda, is an extrasolar planet that orbits the star HAT-P-3 approximately 450 light-years away in the constellation of Ursa Major. It was discovered by the HATNet Project via the transit method and confirmed with Doppler spectroscopy, so both its mass and radius are known quite precisely. Based on these figures it is predicted that the planet has about 75 Earth masses' worth of heavy elements in its core, making it similar to the planet HD 149026 b.

    <span class="mw-page-title-main">WASP-6b</span> Extrasolar planet

    WASP-6b, also named Boinayel, is an extrasolar planet approximately 600 light years away in the constellation Aquarius. It was discovered in 2008, by the WASP survey, by astronomical transit across its parent star WASP-6. This planet orbits only 4% that of Earth-Sun distance. The planet has mass half that of Jupiter, but its insolation has forced a thermal expansion of its radius over that of Jupiter. The planet is an inflated Hot Jupiter. Starspots on the host star WASP-6 helped to refine the measurements of the mass and the radius of the planet.

    HAT-P-3, is a metal-rich K5 dwarf star located about 441 light-years away in the constellation Ursa Major. At a magnitude of about 11.5 it is not visible to the naked eye but is visible in a small to medium-sized amateur telescope. It is believed to be a relatively young star and has a slightly enhanced level of chromospheric activity.

    HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

    WASP-19, formally named Wattle, is a magnitude 12.3 star about 869 light-years away, located in the Vela constellation of the southern hemisphere. This star has been found to host a transiting hot Jupiter-type planet in tight orbit.

    <span class="mw-page-title-main">WASP-19b</span> Extrasolar planet in the constellation Vela

    WASP-19b, formally named Banksia, is an exoplanet, notable for possessing one of the shortest orbital periods of any known planetary body: 0.7888399 days or approximately 18.932 hours. It has a mass close to that of Jupiter, but by comparison has a much larger radius ; making it nearly the size of a low-mass star. It orbits the star WASP-19 in the Vela constellation. At the time of discovery it was the shortest period hot Jupiter discovered as planets with shorter orbital periods had a rocky, or metallic composition.

    <span class="mw-page-title-main">GJ 1214</span> Star in the constellation Ophiuchus

    GJ 1214 is a dim M4.5 red dwarf star in the constellation Ophiuchus with an apparent magnitude of 14.7. It is located at a distance of 47.8 light-years from Earth. GJ 1214 hosts one known exoplanet.

    <span class="mw-page-title-main">WASP-43b</span> Extrasolar planet in the constellation Sextans

    WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

    <span class="mw-page-title-main">GJ 3470 b</span> Hot Neptune orbiting GJ 3470

    GJ 3470 b is an exoplanet orbiting the star GJ 3470, located in the constellation Cancer. With a mass of just under 14 Earth-masses and a radius approximately 4.3 times that of Earth's, it is likely something akin to Neptune despite the initially strong belief that the planet was not covered in clouds like the gas giants in the Solar System.

    <span class="mw-page-title-main">WASP-121b</span> Hot Jupiter exoplanet orbiting WASP-121

    WASP-121b, formally named Tylos, is an exoplanet orbiting the star WASP-121. WASP-121b is the first exoplanet found to contain water in an extrasolar planetary stratosphere. WASP-121b is in the constellation Puppis, and is about 858 light-years from Earth.

    WASP-121, also known as CD-38 3220, is a magnitude 10.4 star located approximately 858 light-years away in the constellation Puppis. WASP-121 has a mass and radius similar to the Sun's. It hosts one known exoplanet.

    HAT-P-26 is a K-type main-sequence star about 466 light-years away. A survey in 2015 did not find any stellar companions in orbit around it, although a red dwarf companion with a temperature 4000+100
    −350     K is suspected on wide orbit.

    GJ 3470 is a red dwarf star located in the constellation of Cancer, 96 light-years away from Earth. With a faint apparent magnitude of 12.3, it is not visible to the naked eye. It hosts one known exoplanet.

    HAT-P-18 is a K-type main-sequence star about 530 light-years away. The star is very old and has a concentration of heavy elements similar to solar abundance. A survey in 2015 detected very strong starspot activity on HAT-P-18.

    WASP-62, formally named Naledi, is a single star about 573 light-years away. It is an F class main-sequence star, orbited by a planet, WASP-62b. The age of WASP-62 is much younger than the Sun at 0.8±0.6 billion years, and it has a metal abundance similar to the Sun.

    WASP-63 or Kosjenka, also known as CD-38 2551, is a single star with an exoplanetary companion in the southern constellation of Columba. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 11.1. The distance to this system is approximately 942 light-years based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.

    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.

    <span class="mw-page-title-main">Gliese 486</span> Star in constellation of Virgo

    Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years away in the constellation Virgo. It hosts one known exoplanet.

    LHS 3844 is a red dwarf star located 48.5 light-years away from the Solar System in the constellation of Indus. The star has about 15% the mass and 19% the radius of the Sun. It is a relatively inactive red dwarf with a slow rotation period of about 128 days, though UV flares have been observed. LHS 3844 is orbited by one known exoplanet.

    References

    1. 1 2 3 4 5 6 7 8 9 Hartman, J. D.; et al. (2009). "HAT-P-12b: A Low-density sub-Saturn mass planet transiting a metal-poor K dwarf". The Astrophysical Journal. 706 (1): 785–796. arXiv: 0904.4704 . Bibcode:2009ApJ...706..785H. doi:10.1088/0004-637X/706/1/785. S2CID   14540643.
    2. 1 2 3 "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
    3. ↑ Lee, Jae Woo; Youn, Jae-Hyuck; Kim, Seung-Lee; Lee, Chung-Uk; Hinse, Tobias Cornelius (2012). "THE SUB-SATURN MASS TRANSITING PLANET HAT-P-12b". The Astronomical Journal. 143 (4): 95. arXiv: 1201.6419 . Bibcode:2012AJ....143...95L. doi:10.1088/0004-6256/143/4/95. S2CID   118610109.
    4. ↑ Yan, F.; Espinoza, N.; Molaverdikhani, K.; Henning, Th.; Mancini, L.; Mallonn, M.; Rackham, B. V.; Apai, D.; Jordán, A.; Mollière, P.; Chen, G.; Carone, L.; Reiners, Ansgar (2020), "LBT transmission spectroscopy of HAT-P-12b: confirmation of a cloudy atmosphere with no significant alkali features", Astronomy & Astrophysics, A98: 642, arXiv: 2007.15485 , Bibcode:2020A&A...642A..98Y, doi:10.1051/0004-6361/201937265, S2CID   220870755
    5. ↑ Wong, Ian; Benneke, Björn; Gao, Peter; Knutson, Heather A.; Chachan, Yayaati; Henry, Gregory W.; Deming, Drake; Kataria, Tiffany; Lee, Graham K. H.; Nikolov, Nikolay; Sing, David K.; Ballester, Gilda E.; Baskin, Nathaniel J.; Wakeford, Hannah R.; Williamson, Michael H. (2020). "Optical to near-infrared transmission spectrum of the warm sub-Saturn HAT-P-12b". The Astronomical Journal. 159 (5): 234. arXiv: 2004.03551 . Bibcode:2020AJ....159..234W. doi: 10.3847/1538-3881/ab880d . S2CID   215238620.
    6. ↑ Jiang, C.; Chen, G.; Pallé, E.; Murgas, F.; Parviainen, H.; Yan, F.; Ma, Y. (2021), "Evidence for stellar contamination in the transmission spectra of HAT-P-12b", Astronomy & Astrophysics, 656: A114, arXiv: 2109.11235 , Bibcode:2021A&A...656A.114J, doi:10.1051/0004-6361/202141824, S2CID   237604976
    7. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.

    Commons-logo.svg Media related to HAT-P-12b at Wikimedia Commons

    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.