| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| 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 mas[3] |
| 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]
- ^ a b c d e f g Cite error: The named reference
simbadwas invoked but never defined (see the help page). - ^ Cite error: The named reference
Wong2020was invoked but never defined (see the help page). - ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d 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
- ^ a b Cite error: The named reference
Addison2018was invoked but never defined (see the help page). - ^ SALT observations of the chromosphere activity of transiting planet hosts: mass-loss and star–planet interactions
- ^ Cite error: The named reference
Methodologywas invoked but never defined (see the help page).