HAT-P-3b

HAT-P-3b / Teberda
	Size comparison of HAT-P-3b (Teberda) with Jupiter
Discovery
Discovered by	HATNet Project
Discovery date	28 July 2007
Detection method	Transit
Orbital characteristics
Semi-major axis	0.03899+0.00062; −0.00065 AU
Eccentricity	<0.0100
Orbital period (sidereal)	2.8997360±0.0000020 d
Inclination	87.24
Time of periastron	2454218.7598 ± 0.0029
Semi-amplitude	89.1 ± 2.0
Star	HAT-P-3
Physical characteristics
Mean radius	0.890 ± 0.046 RJ
Mass	0.609+0.021; −0.022 MJ
Mean density	1.06 ± 0.17 g/cm3
Surface gravity	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]

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]

References

^ ^a ^b 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.
^ 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.
^ ^a ^b ^c ^d 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.
^ "Approved names". NameExoworlds. Archived from the original on 2019-12-19. Retrieved 2020-01-02.
^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
^ 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.