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[1] mas |
| Distance | 87.45 ± 0.07 ly (26.81 ± 0.02 pc) |
| Absolute magnitude (MV) | 4.74[2] |
| Details[5] | |
| Mass | 0.998±0.024 M☉ |
| Luminosity | 1.25[2] L☉ |
| Surface gravity (log g) | 4.30±0.08 cgs |
| Temperature | 5,614±34 K |
| Metallicity [Fe/H] | +0.27±0.03 dex |
| Age | 4.349±2.399 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥ 9.28±0.95 M
|