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]
Based upon an 8-year survey using the HARPS spectrograph at La Silla Observatory, in 2011 the detection of a pair of planets orbiting this star were announced. The inner planet, HD 134060 b, is in a tight, eccentric orbit around the star with a period of just over three days. The second object, HD 134060 c, has a more leisurely period of around 3.2 years and a high orbital eccentricity. [9]
The star was observed for a few hours by the Spitzer Space Telescope in the hopes of observing a transit by the inner planet, but none was detected. [2] HD 134060 displays an infrared excess at a wavelength of 18μm, making it a warm debris disk candidate. [10]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 0.0351±0.0021 MJ | 0.0441±0.0010 [6] | 3.269555+0.000092 −0.000080 [6] |
0.480±0.034 [6] | — | — |
c | 0.1507±0.071 MJ | 2.2263±0.0507 | 1,160.9±27.046 | 0.75±0.19 | — | — |
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]
Based upon an 8-year survey using the HARPS spectrograph at La Silla Observatory, in 2011 the detection of a pair of planets orbiting this star were announced. The inner planet, HD 134060 b, is in a tight, eccentric orbit around the star with a period of just over three days. The second object, HD 134060 c, has a more leisurely period of around 3.2 years and a high orbital eccentricity. [9]
The star was observed for a few hours by the Spitzer Space Telescope in the hopes of observing a transit by the inner planet, but none was detected. [2] HD 134060 displays an infrared excess at a wavelength of 18μm, making it a warm debris disk candidate. [10]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 0.0351±0.0021 MJ | 0.0441±0.0010 [6] | 3.269555+0.000092 −0.000080 [6] |
0.480±0.034 [6] | — | — |
c | 0.1507±0.071 MJ | 2.2263±0.0507 | 1,160.9±27.046 | 0.75±0.19 | — | — |