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]
| 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 |
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]
Planetary system
editBased 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 | — | — |
References
edit- ^ a b c d e f Gaia Collaboration; Brown, A. G. A.; Vallenari, A.; Prusti, T.; De Bruijne, J. H. J.; Mignard, F.; Drimmel, R.; et al. (2016), "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties", Astronomy & Astrophysics, 595: A2, arXiv:1609.04172, Bibcode:2016A&A...595A...2G, doi:10.1051/0004-6361/201629512, S2CID 1828208.
- ^ a b c d e f g h Gillon, M.; et al. (May 2017), "The Spitzer search for the transits of HARPS low-mass planets. II. Null results for 19 planets", Astronomy & Astrophysics, 601: 23, arXiv:1701.01303, Bibcode:2017A&A...601A.117G, doi:10.1051/0004-6361/201629270, S2CID 86862862, A117.
- ^ a b Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (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.
- ^ a b c d e f 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.
- ^ 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 c d e Delgado Mena, E.; et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics, 576: 24, arXiv:1412.4618, Bibcode:2015A&A...576A..69D, doi:10.1051/0004-6361/201425433, S2CID 56051637, A69.
- ^ "HD 134060". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-12.
- ^ 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.
- ^ Mayor, M.; et al. (September 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 [astro-ph.EP]
- ^ Ishihara, Daisuke; et al. (May 2017), "Faint warm debris disks around nearby bright stars explored by AKARI and IRSF", Astronomy & Astrophysics, 601: 18, arXiv:1608.04480, Bibcode:2017A&A...601A..72I, doi:10.1051/0004-6361/201526215, S2CID 55234482, A72.
- ^ "The Extrasolar Planet Encyclopaedia — HD 134060 B". Archived from the original on 2014-02-02. Retrieved 2013-01-31.
External links
edit- "Planet HD 134060 b", Extrasolar Planets Encyclopaedia, retrieved 2018-07-13.
- "Planet HD 134060 c", Extrasolar Planets Encyclopaedia, retrieved 2018-07-13.