HD 133131
Observation data
Epoch J2000      Equinox J2000
Constellation Libra
Right ascension 15h 03m 35.80651s[1]
Declination −27° 50′ 27.5520″[1]
Apparent magnitude (V) 8.40 + 8.42[2]
Characteristics
Spectral type G2 + G2[2]
B−V color index 0.622[3]
Astrometry
Radial velocity (Rv)-16.30 km/s
Proper motion (μ) RA: 156.88 mas/yr
Dec.: -136.07 mas/yr
Parallax (π)19.4 ± 0.12 mas[4][5][6]
Distance168 ± 1 ly
(51.5 ± 0.3 pc)
Orbit[2]
Period (P)~4240 yr
Details[2]
HD 133131 A
Mass0.95 M☉
Surface gravity (log g)4.39 ± 0.050 cgs
Temperature5799 ± 19 K
Metallicity [Fe/H]−0.306 ± 0.016 dex
Age6.3[3] Gyr
HD 133131 B
Mass0.93 M☉
Surface gravity (log g)4.41 ± 0.045 cgs
Temperature5805 ± 15 K
Metallicity [Fe/H]−0.281 ± 0.013 dex
Age5.9[3] Gyr
Other designations
CPD−27° 5116, Gaia DR1 6224633979686194688, HD 133131, HIP 73674[4]
HD 133131 A: CD−27 10194A, Gaia DR2 6224633983987510528, SAO 183128, TYC 6756-1541-1, 2MASS J15033543-2750330[5]
HD 133131 B: CD−27 10194B, Gaia DR2 6224633983987511552, SAO 183129, TYC 6756-867-1, 2MASS J15033579-2750273[6]
Database references
SIMBADHD 133131
HD 133131 A
HD 133131 B

HD 133131 is a binary star in the constellation of Libra. It is roughly 168 light-years (51.5 parsecs) away from the Sun.[2] It consists of two G-type main-sequence stars;[2] neither are bright enough to be seen with the naked eye.

Both components, HD 133131 A and B, are very similar to the Sun but are far older, about 6 billion years old. They also have low metallicities (50% of solar abundance), and HD 133131 A is additionally depleted in heavy elements compared to HD 133131 B, indicating a possibly past planetary engulfment event for HD 133131 B.[7]

Planetary system

In 2016 two planets orbiting HD 133131 A and one planet orbiting HD 133131 B were discovered utilizing the radial velocity method.[2]

The HD 133131 A planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥1.43 MJ 1.44 649 0.32 — —
c ≥0.63 MJ 4.79 3925 0.20 — —
The HD 133131 B planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥2.50 MJ 6.40 6119 0.62 — —

References

  1. ^ a b van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c d e f g h i Teske, Johanna K; Shectman, Stephen A; Vogt, Steve S; Díaz, Matías; Butler, R. Paul; Crane, Jeffrey D; Thompson, Ian B; Arriagada, Pamela (2016). "The Magellan PFS Planet Search Program: Radial Velocity and Stellar Abundance Analyses of the 360 AU, Metal-Poor Binary "Twins" HD 133131A & B". The Astronomical Journal. 152 (6): 167. arXiv:1608.06216. Bibcode:2016AJ....152..167T. doi:10.3847/0004-6256/152/6/167. S2CID 118852162.
  3. ^ a b c Arriagada, Pamela (2011), "Chromospheric Activity of Southern Stars from the Magellan Planet Search Program", The Astrophysical Journal, 734 (1): 70, arXiv:1104.3186, Bibcode:2011ApJ...734...70A, doi:10.1088/0004-637X/734/1/70, S2CID 118384591
  4. ^ a b "HD 133131". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 September 2020.
  5. ^ a b "HD 133131 A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 September 2020.
  6. ^ a b "HD 133131 B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 September 2020.
  7. ^ Oh, Semyeong; Price-Whelan, Adrian M.; Brewer, John M.; Hogg, David W.; Spergel, David N.; Myles, Justin (2017), "Kronos and Krios: Evidence for Accretion of a Massive, Rocky Planetary System in a Comoving Pair of Solar-type Stars", The Astrophysical Journal, 854 (2): 138, arXiv:1709.05344, doi:10.3847/1538-4357/aaab4d, S2CID 119076217
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