WASP-72
(Redirected from WASP-72b)
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Fornax[1] |
| Right ascension | 02h 44m 09.60960s[2] |
| Declination | −30° 10′ 08.5637″[2] |
| Apparent magnitude (V) | 10.96[3] |
| Characteristics | |
| Spectral type | F7[4] |
| Apparent magnitude (B) | 11.454[3] |
| Apparent magnitude (R) | 10.47[3] |
| Apparent magnitude (I) | 10.428[3] |
| Astrometry | |
| Radial velocity (Rv) | 36.20±0.31[2] km/s |
| Proper motion (μ) | RA: +7.614 mas/yr[2] Dec.: −7.673 mas/yr[2] |
| Parallax (π) | 2.3889±0.0252 mas[2] |
| Distance | 1,370 ± 10 ly (419 ± 4 pc) |
| Orbit[5] | |
| Primary | WASP-72 |
| Name | WASP-72B |
| Semi-major axis (a) | 0.639±0.003" (281 AU) |
| Details[6] | |
| WASP-72 | |
| Mass | 1.386±0.055 M☉ |
| Radius | 1.98±0.24 R☉ |
| Luminosity | 5.3+1.5 −1.3 L☉ |
| Surface gravity (log g) | 4.08±0.13 cgs |
| Temperature | 6250±100 K |
| Metallicity [Fe/H] | −0.06±0.09 dex |
| Rotational velocity (v sin i) | 6.0±0.7 km/s |
| Age | 3.55±0.82[5] Gyr |
| WASP-72B | |
| Mass | 0.66±0.02[5] M☉ |
| Temperature | 4234+80 −81[5] K |
| Other designations | |
| Diya, CD−30 1019, TOI-264, TIC 122612091, WASP-72, TYC 7011-487-1, 2MASS J02440959-3010085[3] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
WASP-72 (also known as CD-30 1019 and officially named Diya) is the primary of a binary star system. It is an F7 class dwarf star, with an internal structure just on the verge of the Kraft break.[7] It is orbited by a planet, WASP-72b. The age of WASP-72 is younger than the Sun at 3.55±0.82 billion years.[5]
The primary seems to have UV-opaque matter in the line-of-sight, which may originate from atmosphere escaping from WASP-72b or from an unknown object in the interstellar medium.[8] WASP-72 was named Diya in 2019.[9]
A faint stellar companion WASP-72B was discovered in 2020 at a projected separation of 281 AU. It may still be a false positive, with a probability of 0.02%.[5]
Planetary system
[edit]The transiting hot Jupiter exoplanet orbiting WASP-72 was discovered by WASP in 2012.[6] The planetary orbit is well aligned to the equatorial plane of the star, with misalignment equal to −7°+11°
−12°.[7] Despite the close proximity of the planet to the parent star, orbital decay was not detected as of 2020.[10] The planetary equilibrium temperature is 2210+120
−130 K,[6] compatible with the measured dayside temperature of 2098+335
−364 K.[11]
WASP-72b was named "Cuptor" in 2019 by Mauritian amateur astronomers as part of the NameExoWorlds contest.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b / Cuptor | 1.446+0.054 −0.053 MJ |
0.03711+0.00048 −0.00051 |
2.2167421(81) | <0.017 | 79.9+1.6 −1.3[4] |
1.24±0.15[4] RJ |
References
[edit]- ↑ 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.
- 1 2 3 4 5 6 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.
- 1 2 3 4 5 "CD-30 1019". SIMBAD. Centre de données astronomiques de Strasbourg.
- 1 2 3 Wong, Ian; Shporer, Avi; Daylan, Tansu; Benneke, Björn; Fetherolf, Tara; Kane, Stephen R.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Winn, Joshua N.; Jenkins, Jon M.; Boyd, Patricia T.; Glidden, Ana; Goeke, Robert F.; Sha, Lizhou; Ting, Eric B.; Yahalomi, Daniel (2020), "Systematic phase curve study of known transiting systems from year one of the TESS mission", The Astronomical Journal, 160 (4): 155, arXiv:2003.06407, Bibcode:2020AJ....160..155W, doi:10.3847/1538-3881/ababad, S2CID 212717799
- 1 2 3 4 5 6 Bohn, A. J.; Southworth, J.; Ginski, C.; Kenworthy, M. A.; Maxted, P. F. L.; Evans, D. F. (2020), "A multiplicity study of transiting exoplanet host stars. I. High-contrast imaging with VLT/SPHERE", Astronomy & Astrophysics, 635: A73, arXiv:2001.08224, Bibcode:2020A&A...635A..73B, doi:10.1051/0004-6361/201937127, S2CID 210861118
- 1 2 3 Gillon, M.; Anderson, D. R.; Collier-Cameron, A.; Doyle, A. P.; Fumel, A.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Montalban, J.; Pepe, F.; Pollacco, D.; Queloz, D.; Segransan, D.; Smith, A. M. S.; Smalley, B.; Southworth, J.; Triaud, A. H. M. J.; Udry, S.; West, R. G. (2012), "WASP-64b and WASP-72b: two new transiting highly irradiated giant planets", Astronomy & Astrophysics, 552: A82, arXiv:1210.4257, Bibcode:2013A&A...552A..82G, doi:10.1051/0004-6361/201220561, S2CID 53687206
- 1 2 Addison, B. C.; Wang, Songhu; Johnson, M. C.; Tinney, C. G.; Wright, D. J.; Bayliss, D. (2018), "Stellar Obliquities and Planetary Alignments (SOPA). I. Spin-orbit measurements of three transiting hot Jupiters: WASP-72b, WASP-100b, and WASP-109b", The Astronomical Journal, 156 (5): 197, arXiv:1809.00314, Bibcode:2018AJ....156..197A, doi:10.3847/1538-3881/aade91, S2CID 67819738
- ↑ SALT observations of the chromosphere activity of transiting planet hosts: mass-loss and star–planet interactions
- 1 2 "Methodology | IAU100 Name ExoWorlds - An IAU100 Global Event". Name Exoworlds. International Astronomical Union. Retrieved 2020-11-10.
- ↑ Patra, Kishore C.; Winn, Joshua N.; Holman, Matthew J.; Gillon, Michael; Burdanov, Artem; Jehin, Emmanuel; Delrez, Laetitia; Pozuelos, Francisco J.; Barkaoui, Khalid; Benkhaldoun, Zouhair; Narita, Norio; Fukui, Akihiko; Kusakabe, Nobuhiko; Kawauchi, Kiyoe; Terada, Yuka; Bouma, L. G.; Weinberg, Nevin N.; Broome, Madelyn (2020), "The continuing search for evidence of tidal orbital decay of hot Jupiters", The Astronomical Journal, 159 (4): 150, arXiv:2002.02606, Bibcode:2020AJ....159..150P, doi:10.3847/1538-3881/ab7374, S2CID 211066260
- ↑ Wallack, Nicole L.; Knutson, Heather A.; Deming, Drake (2021), "Trends in Spitzer Secondary Eclipses", The Astronomical Journal, 162 (1): 36, arXiv:2103.15833, Bibcode:2021AJ....162...36W, doi:10.3847/1538-3881/abdbb2, S2CID 232417602
- ↑ 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.
