Astronomy:WASP-72
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Fornax |
| Right ascension | 02h 44m 09.6098s[1] |
| Declination | −30° 10′ 08.5614″[1] |
| Apparent magnitude (V) | 10.96[1] |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | F7[2] |
| Apparent magnitude (B) | 11.54 [1] |
| Apparent magnitude (G) | 10.8378 [1] |
| Apparent magnitude (R) | 10.47 [1] |
| Astrometry | |
| Radial velocity (Rv) | 37.36 km/s |
| Proper motion (μ) | RA: 7.447[3] mas/yr Dec.: -7.817[3] mas/yr |
| Parallax (π) | 2.2718 ± 0.0440[3] mas |
| Distance | 1,440 ± 30 ly (440 ± 9 pc) |
| Orbit[4] | |
| Primary | WASP-72 |
| Companion | WASP-72B |
| Semi-major axis (a) | 0.639±0.003" (281 AU) |
| Details[4] | |
| WASP-72 | |
| Mass | 1.386 M☉ |
| Radius | 1.98 R☉ |
| Temperature | 6250 K |
| Rotational velocity (v sin i) | 6.0±2.1[5] km/s |
| Age | 3.55±0.82 Gyr |
| WASP-72B | |
| Mass | 0.66±0.02 M☉ |
| Temperature | 4234+80−81 K |
| Other designations | |
| Database references | |
| SIMBAD | 1019 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.[5] 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.[4]
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.[6] WASP-72 was named Diya in 2019.[7]
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%.[4]
Planetary system
The transiting hot Jupiter exoplanet orbiting WASP-72 was discovered by WASP in 2012.[8] The planetary orbit is well aligned to the equatorial plane of the star, with misalignment equal to −7°+11°
−12°.[5] Despite the close proximity of the planet to the parent star, orbital decay was not detected as of 2020.[9] The planetary equilibrium temperature is 2210+120−130 K,[8] compatible with the measured dayside temperature of 2098+335−364 K.[10]
WASP-72b was named "Cuptor" in 2019 by Mauritian amateur astronomers as part of the NameExoWorlds contest.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b / Cuptor | — | 0.0344±0.0046 | 2.216789+0.000041−0.000054 | 0 | 79.9+1.6−1.3° | 1.24±0.15 RJ |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "CD-30 1019". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=CD-30+1019.
- ↑ 2.0 2.1 Wong, Ian; Shporer, Avi; Daylan, Tansu; Benneke, Björn; Fetherolf, Tara; Kane, Stephen R.; Ricker, George R.; Vanderspek, Roland et al. (2020), "Systematic phase curve study of known transiting systems from year one of the TESS mission", The Astronomical Journal 160 (4): 155, doi:10.3847/1538-3881/ababad, Bibcode: 2020AJ....160..155W
- ↑ 3.0 3.1 3.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 4.0 4.1 4.2 4.3 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, doi:10.1051/0004-6361/201937127, Bibcode: 2020A&A...635A..73B
- ↑ 5.0 5.1 5.2 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, doi:10.3847/1538-3881/aade91, Bibcode: 2018AJ....156..197A
- ↑ SALT observations of the chromosphere activity of transiting planet hosts: mass-loss and star–planet interactions
- ↑ 7.0 7.1 "Methodology | IAU100 Name ExoWorlds - An IAU100 Global Event" (in en). International Astronomical Union. http://www.nameexoworlds.iau.org/methodology.
- ↑ 8.0 8.1 Gillon, M.; Anderson, D. R.; Collier-Cameron, A.; Doyle, A. P.; Fumel, A.; Hellier, C.; Jehin, E.; Lendl, M. et al. (2012), "WASP-64b and WASP-72b: two new transiting highly irradiated giant planets", Astronomy & Astrophysics 552: A82, doi:10.1051/0004-6361/201220561, Bibcode: 2013A&A...552A..82G
- ↑ Patra, Kishore C.; Winn, Joshua N.; Holman, Matthew J.; Gillon, Michael; Burdanov, Artem; Jehin, Emmanuel; Delrez, Laetitia; Pozuelos, Francisco J. et al. (2020), "The continuing search for evidence of tidal orbital decay of hot Jupiters", The Astronomical Journal 159 (4): 150, doi:10.3847/1538-3881/ab7374, Bibcode: 2020AJ....159..150P
- ↑ Wallack, Nicole L.; Knutson, Heather A.; Deming, Drake (2021), "Trends in Spitzer Secondary Eclipses", The Astronomical Journal 162 (1): 36, doi:10.3847/1538-3881/abdbb2, Bibcode: 2021AJ....162...36W
Coordinates: 
02h 44m 09.6098s, −30° 10′ 08.5614″
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