Astronomy:HD 134060
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| 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]
Planetary system
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 | — | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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, doi:10.1051/0004-6361/201629512, Bibcode: 2016A&A...595A...2G.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 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, doi:10.1051/0004-6361/201629270, A117, Bibcode: 2017A&A...601A.117G.
- ↑ 3.0 3.1 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, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 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, doi:10.1093/mnras/stv1441, Bibcode: 2015MNRAS.452.2745S
- ↑ 6.0 6.1 6.2 6.3 6.4 Delgado Mena, E. et al. (April 2015), "Li abundances in F stars: planets, rotation, and Galactic evolution", Astronomy & Astrophysics 576: 24, doi:10.1051/0004-6361/201425433, A69, Bibcode: 2015A&A...576A..69D.
- ↑ "HD 134060". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+134060.
- ↑ 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. https://academic.oup.com/mnras/article/450/3/3127/1063872. 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, doi:10.1051/0004-6361/201526215, A72, Bibcode: 2017A&A...601A..72I.
- ↑ "The Extrasolar Planet Encyclopaedia — HD 134060 B". http://voparis-exoplanet-new.obspm.fr/catalog/hd_134060_b/.
External links
- Planet HD 134060 b, https://exoplanet.eu/catalog/hd_134060_b--963/, retrieved 2018-07-13.
- Planet HD 134060 c, https://exoplanet.eu/catalog/hd_134060_c--964/, retrieved 2018-07-13.
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