| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Circinus |
| Right ascension | 15h 10m 44.74390s[1] |
| Declination | –61° 25′ 20.3469″[1] |
| Apparent magnitude (V) | 6.29±0.01[2] |
| Characteristics | |
| Spectral type | G0 V Fe+0.4[3] or G3 IV[2] |
| B−V color index | 0.623±0.003[4] |
| Astrometry | |
| Radial velocity (Rv) | 43.50±0.74[4] km/s |
| Proper motion (μ) | RA: −185.615[1] mas/yr Dec.: −12.184[1] mas/yr |
| Parallax (π) | 41.59 ± 0.23 mas[1] |
| Distance | 78.4 ± 0.4 ly (24.0 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.37[4] |
| Details[2] | |
| Mass | 1.07±0.07 M☉ |
| Radius | 1.15±0.02 R☉ |
| Luminosity | 1.63[4] L☉ |
| Surface gravity (log g) | 4.35±0.04 cgs |
| Temperature | 5,965±50 K |
| Metallicity [Fe/H] | +0.14±0.01 dex |
| Rotation | 21.2±1.1 d[5] |
| Rotational velocity (v sin i) | 3.21[6] km/s |
| Age | 1.75[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 134060, also known by its Gould designation of 38 G. Circini, is a star in the southern constellation of Circinus. It is near the lower limit of stars visible to the naked eye, having an apparent visual magnitude of 6.29.[2] The distance to HD 134060, as determined using an annual parallax shift measurement of 41.59 mas,[1] is 78.4 light years. It is moving further away with a heliocentric radial velocity of 43.5 km/s, having come within 34.6 ly some 439,000 years ago.[4]
During the NStars project, Grey et al. (2006) found a stellar classification of G0 V Fe+0.4 for this star,[3] matching a Sun-like G-type main-sequence star with an overabundance of iron in its outer atmosphere. However, an older classification of G3 IV[2] is still used, which would suggest it is instead a more evolved subgiant star. HD 134060 has an estimated 1.07 times the mass of the Sun and 1.15 times the Sun's radius.[2] It is radiating 1.63[4] times the Sun's luminosity from its photosphere at an effective temperature of about 5,965 K.[2]
The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 22 to 163 astronomical units.[8]
- ^ a b c d e f Cite error: The named reference
dr1was invoked but never defined (see the help page). - ^ a b c d e f g Cite error: The named reference
Gillon2017was invoked but never defined (see the help page). - ^ a b Cite error: The named reference
Gray2006was invoked but never defined (see the help page). - ^ a b c d e f Cite error: The named reference
Anderson2012was invoked but never defined (see the help page). - ^ Suárez Mascareño, A.; Rebolo, R.; González Hernández, J. I.; Esposito, M. (2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society, 452 (3): 2745–2756, arXiv:1506.08039, Bibcode:2015MNRAS.452.2745S, doi:10.1093/mnras/stv1441
- ^ a b Cite error: The named reference
Delgado_Mena2015was invoked but never defined (see the help page). - ^ Cite error: The named reference
SIMBADwas invoked but never defined (see the help page). - ^ Mugrauer, M.; Ginski, C. (12 May 2015). "High-contrast imaging search for stellar and substellar companions of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 450 (3): 3127–3136. doi:10.1093/mnras/stv771. hdl:1887/49340. Retrieved 19 June 2020.