HD 134606
Observation data
Epoch J2000      Equinox J2000
Constellation Apus
Right ascension 15h 15m 15.04429s[1]
Declination −70° 31′ 10.6439″[1]
Apparent magnitude (V) 6.86[2]
Characteristics
Spectral type G6 IV[3]
B−V color index 0.740±0.001[2]
Astrometry
Radial velocity (Rv)+2.30±1.21[4] km/s
Proper motion (μ) RA: −177.748[1] mas/yr
Dec.: −164.774[1] mas/yr
Parallax (π)37.2972 ± 0.0283 mas[1]
Distance87.45 ± 0.07 ly
(26.81 ± 0.02 pc)
Absolute magnitude (MV)4.74[2]
Details[5]
Mass0.998±0.024 M☉
Luminosity1.25[2] L☉
Surface gravity (log g)4.30±0.08 cgs
Temperature5,614±34 K
Metallicity [Fe/H]+0.27±0.03 dex
Age4.349±2.399 Gyr
Other designations
CD−70° 1258, GC 20455, HD 134606, HIP 74653, SAO 257257, LTT 6064, 2MASS J15151504-7031105[6]
Database references
SIMBADdata

HD 134606 is a yellow-hued star with a planetary system, positioned in the southern constellation of Apus. It is below the nominal limit for visibility with the naked eye, having an apparent visual magnitude of 6.86.[2] Based upon an annual parallax shift of 37.3 mas,[1] it is located 87.45 light years away. The star appears to be moving further from the Earth with a heliocentric radial velocity of +2.3 km/s.[4]

This is an evolving G-type subgiant star with a stellar classification of G6 IV[3] and is not considered active, having a chromospheric activity index of −5.04.[7] It has about the same[5] mass as the Sun but is 25% more luminous.[2] The photosphere is radiating energy at an effective temperature of 5,614 K.[5] It has a higher than solar metallicity rating – a term astronomers use to describe the abundance of elements other than hydrogen and helium.[5]

Planetary system

The discovery of a planetary system orbiting HD 134606 was announced in 2011 following an eight-year survey carried out at the La Silla Observatory in Chile. The detection was made via the radial velocity method using the HARPS instrument. Applying a Keplerian fit to the data suggests the presence of three planets in moderately eccentric orbits.[8] The planets are successively larger the further away they are from the star.[9] None of the planetary orbits displays a mean motion resonance with the others.[10]

The HD 134606 planetary system[11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥ 9.28±0.95 M🜨 0.1023±0.0017 12.083±0.0096 0.15±0.1 — —
c ≥ 12.14±1.52 M🜨 0.2962±0.0049 59.519±0.1746 0.29±0.2 — —
d ≥ 38.45±4.13 M🜨 1.1567±0.0241 459.26±8.3238 0.46±0.09 — —

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. 1 2 Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61
  5. 1 2 3 4 Tsantaki, M.; et al. (July 2013). "Deriving precise parameters for cool solar-type stars. Optimizing the iron line list". Astronomy & Astrophysics. 555: A150. arXiv:1304.6639. Bibcode:2013A&A...555A.150T. doi:10.1051/0004-6361/201321103. S2CID 118388752.
  6. ↑ "HD 134606". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 20, 2018.
  7. ↑ Jenkins, J. S.; et al. (October 2006), "An activity catalogue of southern stars", Monthly Notices of the Royal Astronomical Society, 372 (1): 163–173, arXiv:astro-ph/0607336, Bibcode:2006MNRAS.372..163J, doi:10.1111/j.1365-2966.2006.10811.x, S2CID 17524675.
  8. ↑ Mayor, M.; Marmier, M.; Lovis, C.; Udry, S.; Ségransan, D.; Pepe, F.; Benz, W.; Bertaux, J.-L.; Bouchy, F.; Dumusque, X.; Lo Curto, G.; Mordasini, C.; Queloz, D.; Santos, N. C. (September 13, 2011), The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets, arXiv:1109.2497
  9. ↑ Schlaufman, Kevin C. (2014). "Tests of in situ Formation Scenarios for Compact Multiplanet Systems". The Astrophysical Journal. 790 (2): 11. arXiv:1402.7075. Bibcode:2014ApJ...790...91S. doi:10.1088/0004-637X/790/2/91. S2CID 8130257. 91.
  10. ↑ Giuppone, C. A.; et al. (December 2013), "A semi-empirical stability criterion for real planetary systems with eccentric orbits", Monthly Notices of the Royal Astronomical Society, 436 (4): 3547–3556, arXiv:1309.6861, Bibcode:2013MNRAS.436.3547G, doi:10.1093/mnras/stt1831
  11. ↑ "HD 134606", Extrasolar Planets Encyclopaedia, retrieved 2015-09-20
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