WASP-24
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo[1] |
| Right ascension | 15h 08m 51.738s[2] |
| Declination | +02° 20′ 35.99″[2] |
| Apparent magnitude (V) | 11.3[3] |
| Characteristics | |
| Spectral type | F8/9[4] |
| Astrometry | |
| Proper motion (μ) | RA: –15.5 ± 0.5[2] mas/yr Dec.: –8.7 ± 1.4[2] mas/yr |
| Details | |
| Mass | 1.129 +0.027 −0.025[3] M☉ |
| Radius | 1.147 +0.044 −0.048 R☉ |
| Surface gravity (log g) | 4.26 ± 0.02[5] cgs |
| Temperature | 6107 ± 77[5] K |
| Metallicity [Fe/H] | –0.02 ± 0.10[5] dex |
| Rotational velocity (v sin i) | 7.32 ± 0.88[6] km/s |
| Age | 3.8+1.3 −1.2[4] Gyr |
| Other designations | |
WASP-24 is an F-type star with the Hot Jupiter planet WASP-24b in orbit. WASP-24 is slightly larger and more massive than the Sun, it is 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.
Observational history
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.[4]
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.[4] 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.[4]
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.[4] These stellar characteristics were later used to derive its planet's characteristics.[4]
WASP-24 and, specifically, the discovery of orbiting Hot Jupiter WASP-24b were first reported on SuperWASP's website.[7]
Characteristics
WASP-24 is an F-type star that lies 330 parsecs, or 1,076 light years, away. With an apparent magnitude of 11.3, the star is invisible to the naked eye from the Earth's perspective. WASP-24 is 1.129 solar masses and 1.147 solar radii, making it just slightly larger and more massive than the Sun. It is also hotter, with an effective temperature of 6100 K. The star has an metallicity similar to that of the sun, which means that it has the same amount of metals (elements heavier than He) as found in the Sun .[5] The best fit for WASP-24's age is 3.8 billion years, although this is not well-constrained, and its actual age may lie anywhere between 2.6 and 5.1 billion years.[4]
The star's surface gravity, logg = 4.15, and its low levels of lithium helped derive the star's age, and revealed that it most likely evolved away from the zero age main sequence.[4]
Planetary system
WASP-24b is a Hot Jupiter that is 1.091 Jupiter masses and 1.383 Jupiter radii. Thus, the planet is larger and slightly more massive than Jupiter is. WASP-24b orbits at a distance of 0.03619 AU, roughly 3.5% of the mean distance between the Earth and Sun. It is the only planet yet discovered to orbit WASP-24.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.091 ± 0.025 MJ | 0.03619 ± 0.00027 | 2.3412132 ± 0.0000018 | <0.0388 | 83.30 ± 0.30° | 1.383 ± 0.039 RJ |
References
- ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Vizier query form
- 1 2 3 4 Zacharias, N.; et al. (2013). "The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". The Astronomical Journal. 145 (2). 44. arXiv:1212.6182
. Bibcode:2013AJ....145...44Z. doi:10.1088/0004-6256/145/2/44.Vizier catalog entry - 1 2 3 4 Jean Schneider (2010). "Notes on star WASP-24". Extrasolar Planets Encyclopaedia. Retrieved 30 May 2011.
- 1 2 3 4 5 6 7 8 9 Street, R. A. W.; et al. (2010). "WASP-24 b: A New Transiting Close-in Hot Jupiter Orbiting a Late F-star". The Astrophysical Journal. 720 (1): 337–343. Bibcode:2010ApJ...720..337S. doi:10.1088/0004-637X/720/1/337.
- 1 2 3 4 Torres, Guillermo; et al. (2012). "Improved Spectroscopic Parameters for Transiting Planet Hosts". The Astrophysical Journal. 757 (2). 161. arXiv:1208.1268. Bibcode:2012ApJ...757..161T. doi:10.1088/0004-637X/757/2/161.
- ↑ Simpson, E. K.; et al. (2011). "The spin-orbit angles of the transiting exoplanets WASP-1b, WASP-24b, WASP-38b and HAT-P-8b from Rossiter-McLaughlin observations". Monthly Notices of the Royal Astronomical Society. 414 (4): 3023–3035. arXiv:1011.5664. Bibcode:2011MNRAS.414.3023S. doi:10.1111/j.1365-2966.2011.18603.x.
- ↑ Jean Schneider (2011). "Interactive Extra-solar Planets Catalogue - Candidates detected by radial velocity or astrometry". Extrasolar Planets Encyclopaedia. Retrieved 30 May 2011.
- ↑ Smith, A. M. S.; et al. (2012). "Thermal emission from WASP-24b at 3.6 and 4.5 μm". Astronomy and Astrophysics. 545. A93. arXiv:1203.6017. Bibcode:2012A&A...545A..93S. doi:10.1051/0004-6361/201219294.