WASP-16
In this article we will delve into the fascinating world of WASP-16, a topic that has captured the attention of experts and the curious alike. WASP-16 is a topic that has generated interest in various spheres, from politics to science, including popular culture and history. Over the years, WASP-16 has been the subject of debate and analysis, and its importance and relevance has continued to grow. In this article, we will dive into the different facets of WASP-16, exploring its impact on society and its evolution over time.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Virgo[1] |
| Right ascension | 14h 18m 43.9225s[2] |
| Declination | −20° 16′ 31.844″[2] |
| Apparent magnitude (V) | 11.309[3] |
| Characteristics | |
| Spectral type | G3V[4] |
| Apparent magnitude (B) | 12.51±0.32[5] |
| Apparent magnitude (R) | ~11.00[5] |
| Apparent magnitude (I) | 10.49±0.02[5] |
| Apparent magnitude (J) | 9.984±0.024[5] |
| Apparent magnitude (H) | 9.659±0.022[5] |
| Apparent magnitude (K) | 9.589±0.023[5] |
| Astrometry | |
| Radial velocity (Rv) | −1.34±0.61[2] km/s |
| Proper motion (μ) | RA: 0.088(27) mas/yr[2] Dec.: 17.350(21) mas/yr[2] |
| Parallax (π) | 5.1912±0.0262 mas[2] |
| Distance | 628 ± 3 ly (192.6 ± 1.0 pc) |
| Details | |
| Mass | 1.022±0.101[4] M☉ |
| Radius | 0.946±0.054[4] R☉ |
| Surface gravity (log g) | 4.5±0.2[4] cgs |
| Temperature | 5700±150[4] K |
| Metallicity | 0.01±0.10[4] dex |
| Rotational velocity (v sin i) | 3.0±1.0[4] km/s |
| Age | 5+3.1 −0[4][6] Gyr |
| Other designations | |
| TOI-818, TIC 46096489, WASP-16, TYC 6147-229-1, GSC 06147-00229, 2MASS J14184392-2016317, SDSS J141843.92-201631.8[5] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-16 is a magnitude 11 yellow dwarf main sequence star, with characteristics similar to the Sun,[5] located 628 light-years away in the Virgo constellation.[1]
Planetary system
In 2009, a planet of the star was announced by the SuperWASP project. It is another hot Jupiter type exoplanet.[4]
In 2024, a candidate mini-neptune was detected, also using the transit method. Further observations are needed to confirm its existence. The planet takes ten days to fully orbit WASP-16 and has an equilibrium temperature of 810 K (537 °C).[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.908+0.045 −0.071 MJ |
0.0422+0.0010 −0.0017 |
3.1186068(12) | <0.018 | 85.22+0.27 −0.43° |
1.008+0.083 −0.060 RJ |
| c (unconfirmed) | — | — | 10.457+0.018 −0.028 |
— | — | 2.2±0.23 R🜨 |
References
- ^ a b Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ 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.
- ^ a b c d e f g h i Lister, T. A.; et al. (2009). "WASP-16b: A New Jupiter-Like Planet Transiting a Southern Solar Analog". The Astrophysical Journal. 703 (1): 752–756. arXiv:0908.0297. Bibcode:2009ApJ...703..752L. doi:10.1088/0004-637X/703/1/752. S2CID 15203701.
- ^ a b c d e f g h "TYC 6147-229-1 -- Star". Centre de Données astronomiques de Strasbourg. Retrieved 2009-08-20.
- ^ Brown, D. J. A.; Cameron, A. Collier; Anderson, D. R.; Enoch, B.; Hellier, C.; Maxted, P. F. L.; Miller, G. R. M.; Pollacco, D.; Queloz, D.; Simpson, E.; Smalley, B.; Triaud, A. H. M. J.; Boisse, I.; Bouchy, F.; Gillon, M.; Hébrard, G. (2012). "Rossiter-Mc Laughlin effect measurements for WASP-16, WASP-25 and WASP-31★". Monthly Notices of the Royal Astronomical Society. 423 (2): 1503–1520. arXiv:1203.4971. Bibcode:2012MNRAS.423.1503B. doi:10.1111/j.1365-2966.2012.20973.x. S2CID 53445367.
- ^ a b Dévora-Pajares, Martín; Pozuelos, Francisco J.; Thuillier, Antoine; Timmermans, Mathilde; Van Grootel, Valérie; Bonidie, Victoria; Mota, Luis Cerdeño; Suárez, Juan C. (2024). "The SHERLOCK pipeline: new exoplanet candidates in the WASP-16, HAT-P-27, HAT-P-26, and TOI-2411 systems". Monthly Notices of the Royal Astronomical Society. 532 (4): 4752–4773. arXiv:2407.14602. doi:10.1093/mnras/stae1740.
- ^ Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics. 602: A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID 118923163.
External links
- SuperWASP Homepage
- "WASP-16". Exoplanets. Archived from the original on 2016-03-03. Retrieved 2009-08-28.
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