WASP-71

Last updated
WASP-71
Observation data
Epoch J2000       Equinox J2000
Constellation Cetus [1]
Right ascension 01h 57m 03.204s [2]
Declination +00° 45′ 31.88″ [2]
Apparent magnitude  (V)10.56 [3]
Characteristics
Evolutionary stage main sequence [2]
Spectral type F8 [4]
B−V color index 0.896 [3]
Astrometry
Radial velocity (Rv)7.690±0.004 [5] km/s
Proper motion (μ)RA: 23.418 mas/yr [2]
Dec.: −6.844 mas/yr [2]
Parallax (π)2.8158±0.0265  mas [2]
Distance 1,160 ± 10  ly
(355 ± 3  pc)
Details [6]
Mass 1.53+0.07
−0.06  M☉
Radius 2.17+0.18
−0.10  R☉
Surface gravity (log g)3.944+0.036
−0.050  cgs
Temperature 6,050±100  K
Metallicity [Fe/H]0.15±0.07  dex
Rotational velocity (v sin i)7.8±0.3 km/s
Age 3.6+1.6
−1.0  Gyr
Other designations
Mpingo, BD+00 316, TOI-388, TIC 422655579, WASP-71, TYC 30-116-1, 2MASS J01570320+0045318 [7]
Database references
SIMBAD data
Exoplanet Archive data

WASP-71, also named Mpingo, is an ordinary star with a close-orbiting planetary companion in the equatorial constellation of Cetus. With an apparent visual magnitude of 10.56, [3] it is too faint to be visible to the naked eye. This star is located at a distance of 1,160 light-years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 7.7 km/s. [5]

Contents

This is classified as an F-type star with a stellar classification of F8. [4] It is more than double the diameter of the Sun with 1.5 times the Sun's mass. The star is younger than the Sun at about 3.6 billion years, [6] yet is already evolving away from the main sequence. [4] BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron. [6] Imaging surveys in 2015 and 2020 failed to find any stellar companions for BD+00 316. [8] [9]

Nomenclature

The designation WASP-71 comes from the Wide Angle Search for Planets and has been used since 2012; [4] BD+00 316 is the stellar identifier from the Bonner Durchmusterung catalogue. [7]

The star was named Mpingo by Tanzanian amateur astronomers in 2020 as part of the NameExoWorlds contest, after the mpingo tree ( Dalbergia melanoxylon ) whose wood is a type of ebony used in musical instruments. [10]

Planetary system

In 2012 a transiting superjovian planet, designated WASP-71b, was detected on a tight, circular orbit. [4] The planetary orbit is well aligned with the equatorial plane of the star, the misalignment angle being equal to −1.9+7.1
−7.5°. [6] Its equilibrium temperature is 2,016.1+67.0
−52.5 K. [6]

The planet was named Tanzanite by Tanzanian amateur astronomers in 2020 as part of the NameExoWorlds contest, after the mineral also known as tanzanite. [10]

The WASP-71 planetary system [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Tanzanite)2.14±0.08  MJ 0.0460±0.00062.903676±0.000008<0.019 [11] 85.8+2.4
−2.1 ° 		1.35+0.13
−0.07  RJ

References

  1. ↑ 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.
  2. 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.
  3. 1 2 3 Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN   978-0333750889.
  4. 1 2 3 4 5 Smith, A. M. S.; Anderson, D. R.; Bouchy, F.; Collier Cameron, A.; Doyle, A. P.; Fumel, A.; Gillon, M.; Hébrard, G.; Hellier, C.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Moutou, C.; Pepe, F.; Pollacco, D.; Queloz, D.; Santerne, A.; Segransan, D.; Smalley, B.; Southworth, J.; Triaud, A. H. M. J.; Udry, S.; West, R. G. (2013), "WASP-71b: a bloated hot Jupiter in a 2.9-day, prograde orbit around an evolved F8 star", Astronomy & Astrophysics, 552: A120, arXiv: 1211.3045 , Bibcode:2013A&A...552A.120S, doi:10.1051/0004-6361/201220727, S2CID   118575479
  5. 1 2 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.
  6. 1 2 3 4 5 6 Brown, D. J. A.; Triaud, A. H. M. J.; Doyle, A. P.; Gillon, M.; Lendl, M.; Anderson, D. R.; Collier Cameron, A.; Hébrard, G.; Hellier, C.; Lovis, C.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Smalley, B. (2016), "Rossiter–McLaughlin models and their effect on estimates of stellar rotation, illustrated using six WASP systems", Monthly Notices of the Royal Astronomical Society, 464 (1): 810–839, arXiv: 1610.00600 , Bibcode:2017MNRAS.464..810B, doi: 10.1093/mnras/stw2316 , S2CID   53497449
  7. 1 2 "BD+00 316". SIMBAD . Centre de données astronomiques de Strasbourg.
  8. ↑ Wöllert, Maria; Brandner, Wolfgang (2015), "A Lucky Imaging search for stellar sources near 74 transit hosts", Astronomy & Astrophysics, 579: A129, arXiv: 1506.05456 , Bibcode:2015A&A...579A.129W, doi:10.1051/0004-6361/201526525, S2CID   118903879
  9. ↑ 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
  10. 1 2 The IAU announces names for WASP exoplanets
  11. ↑ Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2017), "The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics, A107: 602, arXiv: 1704.00373 , Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID   118923163
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