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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.[3][1]

HAT-P-24b
Discovery
Discovered byHATNet Project
Discovery date2010
Detection method
Transit
Orbital characteristics
Semi-major axis
0.04651+0.00055
−0.00056 AU
Eccentricity<0.038[1]
Orbital period (sidereal)
3.3552479±0.0000062[2] d
StarHAT-P-24
Physical characteristics
Mean radius
1.243 +0.072
−0.061 RJ
Mass0.723+0.031
−0.030[1] MJ
Mean density
0.467+0.089
−0.070 g cm−3
Surface gravity
10.9 ± 1.1 m/s2 (35.8 ± 3.6 ft/s2)

    The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is probably aligned with the equatorial plane of the star, misalignment equal to 20±16°.[4]


    References


    1. 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.
    2. Wang, Xiao-Bin; et al. (2013). "The refined physical parameters of transiting exoplanet system HAT-P-24" (PDF). Research in Astronomy and Astrophysics. 13 (5): 593–603. Bibcode:2013RAA....13..593W. doi:10.1088/1674-4527/13/5/010.
    3. Kipping, D. M.; et al. (2011). "HAT-P-24b: An Inflated Hot Jupiter on a 3.36 Day Period Transiting a Hot, Metal-poor Star". The Astrophysical Journal. 725 (2): 2017–2028. arXiv:1008.3389. Bibcode:2010ApJ...725.2017K. doi:10.1088/0004-637X/725/2/2017.
    4. Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments, 2012, arXiv:1206.6105




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