HAT-P-5b

Last updated
HAT-P-5b / Kráľomoc
Exoplanet Comparison HAT-P-5 b.png
Size comparison of HAT-P-5b with Jupiter.
Discovery
Discovered by Bakos et al.
Discovery dateOctober 9, 2007
transit
Orbital characteristics
0.04075 ± 0.00076 AU (6,096,000 ± 114,000 km)
Eccentricity 0
2.788491 ± 2.5e-5 d
Inclination 86.75 ± 0.44
Star HAT-P-5
Physical characteristics
Mean radius
1.204±0.017 RJ [1]
Mass 0.989±0.053 MJ [1]
Mean density
660 ± 110  kg/m3 (1,110 ± 190  lb/cu yd)
Temperature 1485+109
−118 [2]

    HAT-P-5b is a transiting extrasolar planet located approximately 1000 light-years away in the constellation of Lyra, orbiting the star HAT-P-5. It is a hot Jupiter with a mass 6% greater than Jupiter and a radius 26% greater than Jupiter, corresponding to a density of 0.66 g/cm3, which is less than water. This planet was found by Bakos et al. on October 9, 2007. [3]

    Contents

    The planet HAT-P-5b is named Kráľomoc. The name was selected in the NameExoWorlds campaign by Slovakia, during the 100th anniversary of the IAU. Kráľomoc is an ancient Slovak term for the planet Jupiter. [4] [5]

    Physical properties

    The measured temperature on the planetary dayside is 1485+109
    −118     K. [2]

    See also

    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.

    <span class="mw-page-title-main">HAT-P-2b</span> Extrasolar planet

    HAT-P-2b is an extrasolar planet detected by the HATNet Project in May 2007. It orbits a class F star HAT-P-2,, located about 420 light-years away in the constellation Hercules.

    The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

    <span class="mw-page-title-main">HAT-P-4b</span> Exoplanet orbiting HAT-P-4b in the constellation Boötes

    HAT-P-4b is a confirmed extrasolar planet orbiting the star HAT-P-4 over 1000 light years away in Boötes constellation. It was discovered by transit on October 2, 2007, which looks for slight dimming of stars caused by planets that passed in front of them. It is the fourth planet discovered by the HATNet Project. It is also called BD+36 2593b, TYC 2569-01599-1b, 2MASS J15195792+3613467b, SAO 64638b.

    HAT-P-5 is a 12th magnitude star in the constellation Lyra, approximately 1,000 light years away from Earth. It is a spectral type G star, about 1.16 solar masses and radii greater than the Sun, and only 200 kelvins hotter. It is estimated to be 2.6 billion years old.

    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.

    <span class="mw-page-title-main">HAT-P-8b</span> Extrasolar planet in the constellation Pegasus

    HAT-P-8b is an extrasolar planet located approximately 720 light years away in the constellation of Pegasus, orbiting the 10th magnitude star GSC 02757-01152. This planet was discovered by transit on December 5, 2008. Despite the designation as HAT-P-8b, it is the 11th planet discovered by the HATNet Project. The mass of the planet is 50% more than Jupiter while the radius is also 50% more than Jupiter. The mass of this planet is exact since the inclination of the orbit is known, typical for transiting planets. This is a so-called “hot Jupiter” because this Jupiter-like gas giant planet orbits in a really close torch orbit around the star, making this planet extremely hot. The distance from the star is roughly 20 times smaller than that of Earth from the Sun, which places the planet roughly 8 times closer to its star than Mercury is from the Sun. The “year” on this planet lasts only 3 days, 1 hour, 49 minutes, and 54 seconds, compared with Earth's 365 days, 6 hours, 9 minutes, and 10 seconds in a sidereal year.

    GSC 03089-00929 is a magnitude 12 star located approximately 760 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.

    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.

    <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.

    WASP-37 is a yellow main sequence star in the constellation of Virgo.

    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.

    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.

    References

    1. 1 2 Wang, Xian-Yu; et al. (1 July 2021). "Transiting Exoplanet Monitoring Project (TEMP). VI. The Homogeneous Refinement of System Parameters for 39 Transiting Hot Jupiters with 127 New Light Curves". The Astrophysical Journal Supplement Series. 255 (1). 15. arXiv: 2105.14851 . Bibcode:2021ApJS..255...15W. doi: 10.3847/1538-4365/ac0835 . S2CID   235253975.
    2. 1 2 Wallack, Nicole L.; Knutson, Heather A.; Deming, Drake (2021), "Trends in Spitzer Secondary Eclipses", The Astronomical Journal, 162 (1): 36, arXiv: 2103.15833 , Bibcode:2021AJ....162...36W, doi: 10.3847/1538-3881/abdbb2 , S2CID   232417602
    3. ↑ Bakos, G. Á.; et al. (2007). "HAT-P-5b: A Jupiter-like Hot Jupiter Transiting a Bright Star". The Astrophysical Journal Letters. 671 (2): L173–L176. arXiv: 0710.1841 . Bibcode: 2007ApJ...671L.173B . doi: 10.1086/525022 . S2CID   15514048.
    4. ↑ "Approved names". NameExoworlds. Retrieved 2020-01-02.
    5. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.

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