WASP-17

WASP-17 is an F-type main sequence star approximately 1,300 light-years away in the constellation Scorpius.[4][1][5] As of 2009, an extrasolar planet has been confirmed to orbit the star. The planet is thought to orbit in a retrograde orbit (in the opposite direction to the star's rotation).

WASP-17
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Scorpius
Right ascension  15h 59m 50.9473s[1]
Declination −28° 03′ 42.327″[1]
Apparent magnitude (V) 11.500[2]
Characteristics
Spectral type F6V
Astrometry
Proper motion (μ) RA: −6.600±1.557[1] mas/yr
Dec.: −8.485±0.774[1] mas/yr
Parallax (π)2.4366 ± 0.0518[1] mas
Distance1,340 ± 30 ly
(410 ± 9 pc)
Details
Mass1.2 M☉
Radius1.38 R☉
Surface gravity (log g)4.14 ± 0.03[3] cgs
Temperature6509 ± 86[3] K
Metallicity [Fe/H]–0.02 ± 0.09[3] dex
Rotational velocity (v sin i)10.6 ± 1.3[3] km/s
Age3 Gyr
Other designations
Dìwö, 1SWASP J155950.94−280342.3,
USNO-B1.0 0619-0419495,
2MASS J15595095-2803422,
TYC2 6787-1927-1, Gaia DR2 6042793005779654656
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

WASP-17 is named Dìwö. The name was selected in the NameExoWorlds campaign by Costa Rica, during the 100th anniversary of the IAU. Dìwö in Bribri language means the sun.[6][7]

Planetary system
Main article: WASP-17b

The star is unusual in that it has an orbiting exoplanet, WASP-17b,[8][9] which is believed to orbit in the opposite direction to the star's spin and is said to be twice the size of Jupiter, but half its mass. It is subject to intensive photo-evaporation, and may be completely destroyed within one billion years from now.[10]

The planet was discovered by the SuperWASP project, hence the name.


The WASP-17 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.486 (± 0.032) MJ 0.0515 (± 0.00034) 3.735438 (± 6.8e-06) 0.028 +0.018
−0.015		 — —
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References
  1. Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.Gaia Data Release 1 catalog entry
  2. Maxted, P. F. L.; et al. (2011). "UBV(RI)C photometry of transiting planet hosting stars". Monthly Notices of the Royal Astronomical Society. 418 (2): 1039–1042. arXiv:1108.0349. Bibcode:2011MNRAS.418.1039M. doi:10.1111/j.1365-2966.2011.19554.x.
  3. 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.
  4. Anderson, D. R.; et al. (2010). "WASP-17b: An Ultra-Low Density Planet in a Probable Retrograde Orbit". The Astrophysical Journal. 709 (1): 159–167. arXiv:0908.1553. Bibcode:2010ApJ...709..159A. doi:10.1088/0004-637X/709/1/159.
  5. http://www.space.com/scienceastronomy/090812-backward-planet.html
  6. "Approved names". NameExoworlds. Retrieved 2020-01-02.
  7. "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  8. BBC NEWS | Science & Environment |
  9. New-found Planet Orbits Backward
  10. D. Ehrenreich and J.-M. Désert, "Mass-loss rates for transiting exoplanets", 2011
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