WASP-24

Last updated
WASP-24
Observation data
Epoch J2000       Equinox J2000
Constellation Virgo [1]
Right ascension 15h 08m 51.7367s [2]
Declination +02° 20′ 35.9644″ [2]
Apparent magnitude  (V)11.3 [3]
Characteristics
Spectral type F8/9 [4]
Astrometry
Proper motion (μ)RA: −16.713±0.062 [2]   mas/yr
Dec.: −8.702±0.065 [2]   mas/yr
Parallax (π)3.0764 ± 0.0424  mas [2]
Distance 1,060 ± 10  ly
(325 ± 4  pc)
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
USNO-B1.0 0923-0348089, 2MASS J15085174+0220358, TYC 339-329-1, GAIA DR2 1153682508388170112 [3]
Database references
SIMBAD data

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.

Contents

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 325 parsecs, or 1,060 light years, away. [2] 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 a 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]

The WASP-24 planetary system [8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.091 ± 0.025  MJ 0.03619 ± 0.000272.3412132 ± 0.0000018<0.038883.30 ± 0.30° 1.383 ± 0.039  RJ

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<span class="mw-page-title-main">WASP-4b</span> Extrasolar planet in the constellation Phoenix

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<span class="mw-page-title-main">WASP-13b</span> Extrasolar planet in the orbit of the star WASP-13

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<span class="mw-page-title-main">WASP-15b</span> Extrasolar planet orbiting WASP-15

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WASP-24b is a Hot Jupiter detected in the orbit of the F-type star WASP-24. The planet is approximately the same size and mass of Jupiter, but it orbits at approximately 4% of the mean distance between the Earth and the Sun every two days. WASP-24b was observed by SuperWASP starting in 2008; after two years of observations, follow-ups led to the collection of the information that led to the planet's discovery.

WASP-44b is a closely orbiting Jupiter-sized planet found in the orbit of the sunlike star WASP-44 by the SuperWASP program, which searches for transiting planets that cross in front of their host stars as seen from Earth. After follow-up observations using radial velocity, the planet was confirmed. Use of another telescope at the same observatory detected WASP-44 transiting its star. The planet completes an orbit around its star every two and a half days, and orbits at roughly 0.03 AU from its host star. WASP-44b's discovery was reported by the Royal Astronomical Society in May 2011.

WASP-44 is a G-type star in the constellation Cetus that is orbited by the Jupiter-size planet WASP-44b. The star is slightly less massive and slightly smaller than the Sun; it is also slightly cooler, but is more metal-rich. The star was observed by SuperWASP, an organization searching for exoplanets, starting in 2009; manual follow-up observations used WASP-44's spectrum and measurements of its radial velocity led to the discovery of the transiting planet WASP-44b. The planet and its star were presented along with WASP-45b and WASP-46b on May 17, 2011 by a team of scientists testing the idea that hot Jupiters tend to have circular orbits, an assumption that is made when the orbital eccentricity of such planets are not well-constrained.

HAT-P-32b is a planet orbiting the G-type or F-type star HAT-P-32, which is approximately 950 light years away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searching HATNet Project in 2004, although difficulties in measuring its radial velocity prevented astronomers from verifying the planet until after three years of observation. The Blendanal program helped to rule out most of the alternatives that could explain what HAT-P-32b was, leading astronomers to determine that HAT-P-32b was most likely a planet. The discovery of HAT-P-32b and of HAT-P-33b was submitted to a journal on 6 June 2011.

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HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

References

  1. ↑ 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
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  3. 1 2 3 4 Jean Schneider (2010). "Notes on star WASP-24". Extrasolar Planets Encyclopaedia . Archived from the original on April 21, 2010. Retrieved 30 May 2011.
  4. 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. hdl: 10211.3/172030 . S2CID   6745500.
  5. 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. S2CID   16580774.
  6. ↑ 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. S2CID   46522188.
  7. ↑ Jean Schneider (2011). "Interactive Extra-solar Planets Catalogue - Candidates detected by radial velocity or astrometry". Extrasolar Planets Encyclopaedia . Retrieved 30 May 2011.
  8. ↑ 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. S2CID   55700178.
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