HAT-P-50b

Last updated
HAT-P-50b
Discovery
Discovery site Kepler Space Observatory
Discovery date2015
Primary transit
Orbital characteristics
0.0453+0.00058
−0.0014 AU
Eccentricity <0.115 [1]
3.12201 ± 0.0000065 [1] d
Inclination 83.65 ± 0.65 [1]
StarHAT-P-50
Physical characteristics
Mean radius
1.288 ± 0.64 [1] RJ
Mass 1.36 ± 0.075 [1] MJ

    HAT-P-50b is an exoplanet orbiting HAT-P-50 star located in the Gemini constellation. [1] [2] It was discovered in 2015. [3]

    Related Research Articles

    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-27</span> Star in the constellation Virgo

    HAT-P-27, also known as WASP-40, is the primary of a binary star system about 650 light-years away. It is a G-type main-sequence star. The star's age is similar to the Sun's at 4.4 billion years. HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

    WASP-36 is a yellow main sequence star in the Hydra constellation.

    HAT-P-26 is a K-type main-sequence star about 302 light-years away. Survey in 2015 did not find any stellar companions on orbit around it, although a red dwarf companion with a temperature 4000+100
    −350     K is suspected on wide orbit.

    HAT-P-25 is a G-type main-sequence star about 990 light-years away. It has a very low flare activity. The star is enriched in heavy elements, having about twice amount of metals compared to solar abundance.

    HAT-P-23 is a G-type main-sequence star about 1200 light-years away. It has a rapid rotation for its advanced age of 4 billion years, and exhibits a strong starspot activity. The star may be in the process of being spun up by the giant planet on close orbit. The star is enriched in heavy elements, having about 140% amount of metals compared to solar abundance.

    HAT-P-21 is a G-type main-sequence star about 910 light-years away. The star has amount of metals similar to solar abundance. The survey in 2015 has failed to detect any stellar companions. The star is rotating rapidly, being spun up by the tides of giant planet on close orbit.

    HAT-P-19 is a K-type main-sequence star about 650 light-years away. The star is old yet metal enriched, having amount of heavy elements 250% of solar abundance. The survey in 2012 have failed to find any stellar companions to HAT-P-19.

    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-16 is a F-type main-sequence star about 740 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58±0.08, close to Sun`s value of 0.55.

    HAT-P-15 is a G-type main-sequence star about 630 light-years away. The star is older than Sun yet has a concentration of heavy elements roughly 190% of solar abundance. The star has no noticeable starspot activity.

    HAT-P-28 is the primary of a binary star system about 1320 light-years away. It is a G-type main-sequence star. The star’s age is older than the Sun`s at 6.1+2.6
    −1.9     billion years. HAT-P-28 is slightly enriched in heavy elements, having a 130% concentration of iron compared to the Sun. Since 2014, the binary star system is suspected to be surrounded by a debris disk with a 6.1″(2500 AU) radius.

    References

    1. 1 2 3 4 5 6 "Planet HAT-P-50 b". exoplanet.eu. Retrieved 2018-04-25.
    2. ↑ "HAT-P-50". Universe Guide. Retrieved 2019-12-27.
    3. ↑ Hartman, J. D.; Bhatti, W.; Bakos, G. Á.; Bieryla, A.; Kovács, G.; Latham, D. W.; Csubry, Z.; De Val-Borro, M.; Penev, K.; Buchhave, L. A.; Torres, G.; Howard, A. W.; Marcy, G. W.; Johnson, J. A.; Isaacson, H.; Sato, B.; Boisse, I.; Falco, E.; Everett, M. E.; Szklenar, T.; Fulton, B. J.; Shporer, A.; Kovács, T.; Hansen, T.; Béky, B.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P. (2015), "HAT-P-50b, HAT-P-51b, HAT-P-52b, AND HAT-P-53b: THREE TRANSITING HOT JUPITERS AND a TRANSITING HOT SATURN FROM THE HATNET SURVEY", The Astronomical Journal, 150 (6): 168, arXiv: 1503.04149 , Bibcode:2015AJ....150..168H, doi:10.1088/0004-6256/150/6/168, S2CID   117960362
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