HD 134060

From Wikipedia
https://en.wikipedia.org/wiki/HD_134060
HD 134060
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 [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
Rotational velocity (v sin i)3.21 [5] km/s
Age1.75 [5]  Gyr
Other designations
38 G. Circini, CD−60° 5490, HD 134060, HIP 74273, SAO 253043, LTT 6035 [6]
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. [7]

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. [8]

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. [9]

The HD 134060 planetary system [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 [5] 3.269555+0.000092
−0.000080
[5]
0.480±0.034 [5]
c 0.1507±0.071  MJ 2.2263±0.0507 1,160.9±27.046 0.75±0.19

References

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ 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.
  6. ^ "HD 134060". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-12.
  7. ^ 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. Retrieved 19 June 2020.
  8. ^ 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]
  9. ^ 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.
  10. ^ "Archived copy". Archived from the original on 2014-02-02. Retrieved 2013-01-31.CS1 maint: archived copy as title ( link)

External links