WASP-2

Last updated
WASP-2
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Delphinus
A [1]
Right ascension 20h 30m 54.1279s [2]
Declination +06° 25′ 46.338″ [2]
Apparent magnitude  (V)+11.98 [3]
C [a 1]
Right ascension ~20h 30m 54s [1]
Declination ~+06° 25′ 46″ [1]
Apparent magnitude  (V)15.38 [1]
Orbit [4]
PrimaryWASP-2A
CompanionWASP-2B
Semi-major axis (a)106″
Characteristics
Spectral type K1.5V + K2-M3 [5]
Apparent magnitude  (B)~13 [3]
Apparent magnitude  (V)~11.98 [3]
Apparent magnitude  (J)10.166±0.027 [3]
Apparent magnitude  (H)9.752±0.026 [3]
Apparent magnitude  (K)9.632±0.024 [3]
Astrometry
Proper motion (μ)RA: 5.936±0.101 [2]   mas/yr
Dec.: −48.279±0.082 [2]   mas/yr
Parallax (π)6.4980 ± 0.0686  mas [2]
Distance 502 ± 5  ly
(154 ± 2  pc)
Details [6]
WASP-2A
Mass 0.843±0.033  M☉
Radius 0.821±0.013  R☉
Temperature 5170±60  K
Age 7.6+2.5
−3.3  Gyr
WASP-2B
Mass 0.48 [1]   M☉
Temperature 3523+28
−19  K
Other designations
GSC 00522-01199, 1SWASP J203054.12+062546.4, USNO-B1.0 0964-00543604, 2MASS J20305413+0625463, UCAC2 34018636, Gaia DR2 1748596020745038208, V357 Del
Database references
SIMBAD data
Extrasolar Planets
Encyclopaedia 		data

WASP-2 is a binary star system in the Delphinus constellation located about 500 light-years away. [3] The primary is magnitude 12 orange dwarf star, orbited by red dwarf star on wide orbit. [4] [7] The star system shows an infrared excess noise of unknown origin. [8]

Contents

Planetary system

This star has one extrasolar planet WASP-2b, detected by the SuperWASP project in 2006. [9]

The WASP-2 planetary system [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.882±0.027  MJ 0.0308±0.00042.15222144 (± 4e-07)0—1.06±0.024  RJ

Binary star

In 2008 a study was undertaken of fourteen stars with exoplanets that were originally discovered using the transit method through relatively small telescopes. These systems were re-examined with the 2.2 m (87 in) reflector telescope at the Calar Alto Observatory in Spain. This star system, along with two others, was determined to be a previously unknown binary star system. The previously unknown secondary star is a dim magnitude 15 M-type star separated by about 111 AU from the primary, appearing offset from the primary by about one arc second in the images. This discovery resulted in a recalculation of parameters for both the planet and the primary star. [1]

The re-examination of the WASP-2 spectrum in 2015, have resulted in the measurement of stellar companion temperature equal to 3513±28 K, and angular separation of 0.73 arc second. [10]

See also

Notes

  1. ↑ The secondary star is identified with a "C" suffix so as to not confuse it with the planetary designation suffix "b". [1]

Related Research Articles

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<span class="mw-page-title-main">HD 15082</span> Star in the constellation Andromeda

HD 15082 is a star located roughly 399 light years away in the northern constellation of Andromeda. The star is a Delta Scuti variable and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.

<span class="mw-page-title-main">HAT-P-27</span> Star in the constellation Virgo

HAT-P-27, also known as WASP-40, is the primary of a binary star system about 650 light-years away. It is a G-type main-sequence star. The star's age is similar to the Sun's at 4.4 billion years. HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

Kepler-102 is a star 353 light-years away in the constellation of Lyra. Kepler-102 is less luminous than the Sun. The star system does not contain any observable amount of dust. Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU.

EQ Pegasi is a nearby binary system of two red dwarfs. Both components are flare stars, with spectral types of M4Ve and M6Ve respectively, and a current separation between the components of 5.8 arcseconds. The system is at a distance of 20.4 light-years, and is 950 million years old. The primary star is orbited by one known exoplanet.

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HD 233731, or HAT-P-22, is a suspected multiple star system in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye, having an apparent visual magnitude of 9.732. This system is located at a distance of 267 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s.

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BD+00 316, also known as WASP-71 since 2019, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.

WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.

WASP-58 is a binary star system comprising a G-type main-sequence star and a red dwarf about 955 light-years away. WASP-58 is slightly depleted in heavy elements, having 80% of the solar abundance of iron. WASP-58 is much older than the Sun at 12.80+0.20
−2.10 billion years.

WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

HD 175289 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

References

  1. 1 2 3 4 5 6 7 Daemgen; et al. (2009). "Binarity of transit host stars - Implications for planetary parameters" (PDF). Astronomy and Astrophysics . 498 (2): 567–574. arXiv: 0902.2179 . Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988. S2CID   9893376.
  2. 1 2 3 4 5 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 5 6 7 "WASP-2". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-05-04.
  4. 1 2 Quarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020), "Orbital stability of circumstellar planets in binary systems", The Astronomical Journal, 159 (3): 80, arXiv: 1912.11019 , Bibcode:2020AJ....159...80Q, doi: 10.3847/1538-3881/ab64fa , S2CID   209444271
  5. ↑ Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics, 575: A23, arXiv: 1507.01938 , Bibcode:2015A&A...575A..23W, doi:10.1051/0004-6361/201424091, S2CID   119250579
  6. 1 2 Southworth, J.; Bohn, A. J.; Kenworthy, M. A.; Ginski, C.; Mancini, L. (2020), "A multiplicity study of transiting exoplanet host stars. II.Revised properties of transiting planetary systems with companions", Astronomy & Astrophysics, A74: 635, arXiv: 2001.08225 , Bibcode:2020A&A...635A..74S, doi:10.1051/0004-6361/201937334, S2CID   210860775
  7. ↑ Precise Differential Analysis of Stellar Metallicities: Application to Solar Analogs Including 16 Cyg A and B
  8. ↑ Sada, Pedro V.; Deming, Drake; Jennings, Donald E.; Jackson, Brian k.; Hamilton, Catrina M.; Fraine, Jonathan; Peterson, Steven W.; Haase, Flynn; Bays, Kevin; Lunsford, Allen; o'Gorman, Eamon (2012), "Extrasolar Planet Transits Observed at Kitt Peak National Observatory", Publications of the Astronomical Society of the Pacific, 124 (913): 212–229, arXiv: 1202.2799 , Bibcode:2012PASP..124..212S, doi:10.1086/665043, S2CID   29665395
  9. ↑ Cameron, A. Collier; et al. (2007). "WASP-1b and WASP-2b: two new transiting exoplanets detected with SuperWASP and SOPHIE". Monthly Notices of the Royal Astronomical Society . 375 (3): 951–957. arXiv: astro-ph/0609688 . Bibcode:2007MNRAS.375..951C. doi:10.1111/j.1365-2966.2006.11350.x. S2CID   735515.
  10. ↑ Piskorz, Danielle; Knutson, Heather A.; Ngo, Henry; Muirhead, Philip S.; Batygin, Konstantin; Crepp, Justin R.; Hinkley, Sasha; Morton, Timothy D. (2015), "Friends of Hot Jupiters. III. An Infrared Spectroscopic Search for Low-Mass Stellar Companions", The Astrophysical Journal, 814 (2): 148, arXiv: 1510.08062 , Bibcode:2015ApJ...814..148P, doi:10.1088/0004-637X/814/2/148, S2CID   11525988
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