| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 01 57 03.204 |
| Declination | 00° 45′ 31.88″ |
| Apparent magnitude (V) | 10.56 |
| Characteristics | |
| Spectral type | F8 |
| B−V color index | 0.896 |
| Astrometry | |
| Radial velocity (Rv) | 7.690±0.004 km/s |
| Proper motion (μ) | RA: 23.418 mas/yr Dec.: −6.844 mas/yr |
| Parallax (π) | 2.8158 ± 0.0265 mas |
| Distance | 1,160 ± 10 ly (355 ± 3 pc) |
| Details | |
| Mass | 1.53 −0.06 M☉ |
| Radius | 2.17 −0.10 R☉ |
| Surface gravity (log g) | 3.944 −0.050 cgs |
| Temperature | 6,050±100 K |
| Metallicity | 0.15±0.07 dex |
| Rotational velocity (v sin i) | 7.8±0.3 km/s |
| Age | 3.6 −1.0 Gyr |
| Other designations | |
| Mpingo, BD+00 316, Gaia DR2 2507901914613005056, WASP-71, TYC 30-116-1, 2MASS J01570320+0045318 | |
| Database references | |
| SIMBAD | 436 data |
BD+00 316 is an ordinary star with a close-orbiting planetary companion in the equatorial constellation of Cetus. It is also known as WASP-71 since 2019; BD+00 316 is the stellar identifier from the Bonner Durchmusterung catalogue. With an apparent visual magnitude of 10.56, 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.
This is classified as an F-type star with a stellar classification of F8. 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, yet is already evolving away from the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron. Imaging surveys in 2015 and 2020 failed to find any stellar companions for BD+00 316.
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.
Planetary system
In 2012 a transiting superjovian planet, designated component b, was detected on a tight, circular orbit. The planetary orbit is well aligned with the equatorial plane of the star, the misalignment angle being equal to −1.9
−7.5°. Its equilibrium temperature is 2,016.1
−52.5 K.
The planet was named Tanzanite by Tanzanian amateur astronomers in 2020 as part of the NameExoWorlds contest, after the mineral also known as tanzanite.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Tanzanite) | 2.14±0.08 MJ | 0.0460±0.0006 | 2.903676±0.000008 | <0.019 | 85.8 −2.1° |
1.35 −0.07 RJ |
References
- ^ 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.
- ^ 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.
- ^ 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
- ^ 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.
- ^ 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
- "BD+00 316". SIMBAD. Centre de données astronomiques de Strasbourg.
- 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
- 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
- ^ The IAU announces names for WASP exoplanets
- 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
