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 mas[1] |
Distance | 1,340 ± 30 ly (410 ± 9 pc) |
Details | |
Mass | 1.2 M☉ |
Radius | 1.38 R☉ |
Surface gravity (log g) | 4.14 ± 0.03[3] cgs |
Temperature | 6509 ± 86[3] K |
Metallicity [Fe/H] | –0.02 ± 0.09[3] dex |
Rotational velocity (v sin i) | 10.6 ± 1.3[3] km/s |
Age | 3 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 | |
SIMBAD | data |
Exoplanet Archive | data |
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 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
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.
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 |
— | — |
References
- ^ a b c d e f 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. S2CID 1828208.Gaia Data Release 1 catalog entry
- ^ 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. S2CID 117056033.
{{cite journal}}
: CS1 maint: unflagged free DOI (link) - ^ a b c d 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.
- ^ 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. S2CID 53628741.
- ^ http://www.space.com/scienceastronomy/090812-backward-planet.html
- ^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
- ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
- ^ BBC NEWS | Science & Environment |
- ^ New-found Planet Orbits Backward
- ^ D. Ehrenreich and J.-M. Désert, "Mass-loss rates for transiting exoplanets", 2011