Astronomy:HD 134060

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Short description: Star in the constellation Circinus
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
Distance78.4 ± 0.4 ly
(24.0 ± 0.1 pc)
Absolute magnitude (MV)4.37[4]
Details[2]
Mass1.07±0.07 M
Radius1.15±0.02 R
Luminosity1.63[4] L
Surface gravity (log g)4.35±0.04 cgs
Temperature5,965±50 K
Metallicity [Fe/H]+0.14±0.01 dex
Rotation21.2±1.1 d[5]
Rotational velocity (v sin i)3.21[6] km/s
Age1.75[6] Gyr
Other designations
38 G. Circini, CD−60° 5490, HD 134060, HIP 74273, SAO 253043, LTT 6035[7]
Database references
SIMBADdata

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]

The HD 134060 planetary system[11]
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. 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, Bibcode2016A&A...595A...2G. 
  2. 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, Bibcode2017A&A...601A.117G. 
  3. 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, Bibcode2006AJ....132..161G. 
  4. 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, Bibcode2012AstL...38..331A. 
  5. 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, Bibcode2015MNRAS.452.2745S 
  6. 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, Bibcode2015A&A...576A..69D. 
  7. "HD 134060". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+134060. 
  8. 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. 
  9. 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]
  10. 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, Bibcode2017A&A...601A..72I. 
  11. "The Extrasolar Planet Encyclopaedia — HD 134060 B". http://voparis-exoplanet-new.obspm.fr/catalog/hd_134060_b/. 

External links