HAT-P-3b

Last updated
HAT-P-3b / Teberda
Exoplanet Comparison HAT-P-3 b.png
Size comparison of HAT-P-3b (Teberda) with Jupiter
Discovery
Discovered by HATNet Project
Discovery date28 July 2007
Transit
Orbital characteristics
0.03899+0.00062
−0.00065 AU
Eccentricity <0.0100 [1]
2.8997360±0.0000020 [2] d
Inclination 87.24
2454218.7598 ± 0.0029
Semi-amplitude 89.1 ± 2.0
Star HAT-P-3
Physical characteristics
Mean radius
0.890 ± 0.046 [3] RJ
Mass 0.609+0.021
−0.022 [1] MJ
Mean density
1,060 ± 170  kg/m3 (1,790 ± 290  lb/cu yd) [3]
12.3  m/s2 (40  ft/s2)

    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. [3]

    Contents

    The planet HAT-P-3b is named Teberda. The name was selected in the NameExoWorlds campaign by Russia, during the 100th anniversary of the IAU. Teberda is a mountain river in Dombay region (name of HAT-P-3). [4] [5]

    In 2013, this planet was photometrically observed by Spitzer Space Telescope which characterized its near-zero eccentricity and low albedo. [6]

    Discovery

    In 2007 the HATNet Project reported the discovery of HAT-P-3b transiting the metal-rich early K dwarf star HAT-P-3 with an orbital period of 2.9 days. It was found with the 11 cm aperture HAT-5 telescope, located at the Fred Lawrence Whipple Observatory on Mount Hopkins in Arizona. Follow up radial velocity observations to confirm the planet were made with the 1.5 m Tillinghast reflector in order to rule out the possibility that the observed decrease in brightness was caused by an eclipsing binary. Final confirmation was made at the W. M. Keck Observatory using the HIRES spectrograph to measure the mass and orbital parameters of the planet. [3]

    Related Research Articles

    <span class="mw-page-title-main">HAT-P-1b</span> Hot Jupiter orbiting HAT-P-1

    HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located roughly 521 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.

    <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.

    HD 147506 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. There is one known transiting extrasolar planet.

    <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-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.

    <span class="mw-page-title-main">HAT-P-6b</span> Extrasolar planet in the Andromeda constellation

    HAT-P-6b is a transiting extrasolar planet discovered by Noyes et al. on October 15, 2007. It is located approximately 910 light-years away in the constellation of Andromeda, orbiting the star HAT-P-6. This hot Jupiter planet orbits with a semi-major axis of about 7.832 gigameters, and takes 92 hours, 28 minutes, 17 seconds and 9 deciseconds to orbit the star. 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.

    <span class="mw-page-title-main">XO-5b</span> Exoplanet in the constellation Lynx

    XO-5b "Makropulos" is an extrasolar planet approximately 910 light years away in the constellation of Lynx. This planet was found by the transit method using the XO Telescope and announced in May 2008. It was also independently discovered by the HATNet Project. The planet has a mass and radius just slightly larger than that of Jupiter. This planet orbits very close to the G-type parent star, as it is typical for transiting planets, classing this as Hot Jupiter. It takes only 4.188 days to orbit at an orbital distance of 0.0488 AU).

    HAT-P-9 is a magnitude 12 F star approximately 1500 light years away in the constellation Auriga. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.

    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.

    HAT-P-8 is a magnitude 10 star located 700 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of 0.22 M☉. The second is even less massive, at 0.18 M☉, and its spectral type is M6V.

    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.

    <span class="mw-page-title-main">HAT-P-12b</span> Extrasolar planet in constellation Canes Venatici

    HAT-P-12b, formally named Puli, 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-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.

    HAT-P-24 is an F8 dwarf star about 400 parsecs away. A planet was discovered with the transit method by the HATNet Project in 2010. HAT-P-24b, is a typical hot Jupiter orbiting in only 3 days.

    HAT-P-24b is an extrasolar planet discovered by the HATNet Project in 2010 orbiting the F8 dwarf star HAT-P-24. It is a hot Jupiter, with a mass three quarters that of Jupiter and a radius 20% larger.

    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.

    References

    1. 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. S2CID   118923163.
    2. ↑ Chan, Tucker; et al. (2011). "The Transit Light-curve Project. XIV. Confirmation of Anomalous Radii for the Exoplanets TrES-4b, HAT-P-3b, and WASP-12b". The Astronomical Journal. 141 (6). 179. arXiv: 1103.3078 . Bibcode:2011AJ....141..179C. doi:10.1088/0004-6256/141/6/179. S2CID   56378813.
    3. 1 2 3 4 Torres, G.; et al. (2007). "HAT-P-3b: A Heavy-Element-rich Planet Transiting a K Dwarf Star". The Astrophysical Journal Letters. 666 (2): L121–L124. arXiv: 0707.4268 . Bibcode: 2007ApJ...666L.121T . doi: 10.1086/521792 . S2CID   16549542.
    4. ↑ "Approved names". NameExoworlds. Archived from the original on 2019-12-19. Retrieved 2020-01-02.
    5. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
    6. ↑ Todorov, Kamen O.; et al. (2013). "Warm Spitzer Photometry of Three Hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b". The Astrophysical Journal. 770 (2). 102. arXiv: 1305.0833 . Bibcode:2013ApJ...770..102T. doi:10.1088/0004-637X/770/2/102. S2CID   51509956.

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