WASP-72

WASP-72 / Diya
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]
Distance1,440 ± 30 ly
(440 ± 9 pc)
Orbit[4]
PrimaryWASP-72
CompanionWASP-72B
Semi-major axis (a)0.639±0.003"
(281 AU)
Details[4]
WASP-72
Mass1.386 M☉
Radius1.98 R☉
Temperature6250 K
Rotational velocity (v sin i)6.0±2.1[5] km/s
Age3.55±0.82 Gyr
WASP-72B
Mass0.66±0.02 M☉
Temperature4234+80
−81 K
Other designations
Diya, CD−30 1019, Gaia DR2 5065640460769428224, TYC 7011-487-1, 2MASS J02440959-3010085[1]
Database references
SIMBAD1019 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]

  1. ^ a b c d e f g Cite error: The named reference simbad was invoked but never defined (see the help page).
  2. ^ Cite error: The named reference Wong2020 was invoked but never defined (see the help page).
  3. ^ 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.
  4. ^ 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
  5. ^ a b Cite error: The named reference Addison2018 was invoked but never defined (see the help page).
  6. ^ SALT observations of the chromosphere activity of transiting planet hosts: mass-loss and star–planet interactions
  7. ^ Cite error: The named reference Methodology was invoked but never defined (see the help page).