WASP-24
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo[1] |
| Right ascension | 15h 08m 51.7367s[2] |
| Declination | +02° 20′ 35.962″[2] |
| Apparent magnitude (V) | 11.3[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | F8/9[3] |
| Astrometry | |
| Radial velocity (Rv) | −17.46±0.58[2] km/s |
| Proper motion (μ) | RA: −16.741 mas/yr[2] Dec.: −8.556 mas/yr[2] |
| Parallax (π) | 3.0330±0.0208 mas[2] |
| Distance | 1,075 ± 7 ly (330 ± 2 pc) |
| Details | |
| Mass | 1.184±0.027[3] M☉ |
| Radius | 1.331±0.032[3] R☉ |
| Surface gravity (log g) | 4.26 ± 0.02[4] cgs |
| Temperature | 6107 ± 77[4] K |
| Metallicity [Fe/H] | –0.02 ± 0.10[4] dex |
| Rotational velocity (v sin i) | 7.32 ± 0.88[5] km/s |
| Age | 3.8+1.3 −1.2[3] Gyr |
| Other designations | |
| TOI-5685, TIC 460396820, WASP-24, TYC 339-329-1, 2MASS J15085174+0220358, USNO-B1.0 0923-0348089[6] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-24 is an F-type star with the hot Jupiter planet WASP-24b in orbit, about 1,075 light-years away in the constellation Virgo. WASP-24 is slightly larger and more massive than the Sun, it also has a similar metallicity and is hotter than the Sun. WASP-24 was first observed by the SuperWASP planet-searching organization, which flagged it as a potential host to a planet before following up with radial velocity and spectral measurements. Analysis of these confirmed the planetary nature of WASP-24b, which was later released to the public on the SuperWASP website.
An eclipsing binary pair of companion stars were identified by a 2019 study using Gaia DR2 data. They are separated by 21.8 arcseconds from the primary star, corresponding to a distance of 7097 AU.[7]
Between March 2008 and April 2009, the northern and southern portions of the SuperWASP Consortium observed the night sky in WASP-24's vicinity. The star, in particular, was flagged as a host to a planetary candidate. After accumulating over 9,750 datapoints for a light curve on WASP-24, all information on the star that had been previously catalogued was collected alongside the new data, and the star was set aside for manual follow-up observations.[3]
The 2.56m Nordic Optical Telescope (NOT) at the Canary Islands' Roque de los Muchachos Observatory was used to collected radial velocity measurements. The Fibre-Fed Echelle Spectrograph, or FIES, was the instrument that collected these observations between December 2008 and April 2009; also used was the CORALIE spectrograph on the Leonhard Euler Telescope at Chile's La Silla Observatory, which collected additional radial velocity and spectral measurements. Analysis of WASP-24's spectrum ruled out the possibility that WASP-24 is a rapidly rotating star, which could make confirmation of a planet difficult, or that it is a spectroscopic binary star system. Use of a span bisector analysis revealed that the star is not very active.[3] WASP-24 was then observed using Hawaii's Faulkes Telescope North and Australia's Faulkes Telescope South, searching for a period at which the discovered planet WASP-24b might transit, or cross in front of, its star, over various days in 2009 and 2010.[3]
Using information collected by NOT, WASP-24's temperature, metallicity, and other characteristics were derived. Detected levels of lithium and the star's surface gravity suggests that the star does not follow the main sequence.[3] These stellar characteristics were later used to derive its planet's characteristics.[3]
WASP-24 and, specifically, the discovery of orbiting hot Jupiter WASP-24b were first reported on SuperWASP's website in April 2010,[8] followed by its formal publication in September 2010.[3]
