HD 142022

HD 142022 is a binary star[7] system located in the southernmost constellation of Octans. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.70.[2] The distance to this system is 112 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −9.6 km/s.[2]

HD 142022
Observation data
Epoch J2000      Equinox J2000
Constellation Octans
Right ascension  16h 10m 15.02686s[1]
Declination −84° 13′ 53.8137″[1]
Apparent magnitude (V) 7.70[2] + 11.19[3]
Characteristics
Spectral type G9IV-V[4] + M1V[3]
B−V color index 0.79±0.01[2]
Astrometry
Radial velocity (Rv)−9.6±0.4[2] km/s
Proper motion (μ) RA: −337.055±0.041[1] mas/yr
Dec.: −31.202±0.050[1] mas/yr
Parallax (π)29.1424 ± 0.0266[1] mas
Distance111.9 ± 0.1 ly
(34.31 ± 0.03 pc)
Absolute magnitude (MV)5.02[2]
Details[5][3]
A
Mass0.972+0.036
−0.029 M☉
Radius1.028+0.011
−0.012 R☉
Luminosity0.886±0.001[1] L☉
Surface gravity (log g)4.386±0.251 cgs
Temperature5,516±31 K
Metallicity [Fe/H]0.24±0.073 dex
Rotational velocity (v sin i)2.048±0.214 km/s
Age7.667+1.704
−1.764 Gyr
B
Mass0.60±0.07 M☉
Radius0.56±0.05 R☉
Luminosity0.063±0.014 L☉
Temperature3,892±95 K
Other designations
CPD−83° 202, GC 21507, GJ 9536, HD 142022, HIP 79242, SAO 258738, LTT 6382[6]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

The primary, designated component A, is an old,[7] Population I G-type star with a stellar classification of G9IV-V,[4] showing a spectrum with mixed traits of a main sequence and a subgiant star. It is an estimated 7.6 billion years old and is spinning with a projected rotational velocity of 2 km/s. The star has similar mass and dimensions as the Sun, but has a 55% higher metallicity.[5] It is radiating 89%[1] of the luminosity of the Sun from its photosphere at an effective temperature of 5516 K.[5]

The magnitude 11.19[3] companion has the designation LTT 6384 and appears gravitationally bound to the primary. The pair have an angular separation of 22 arcseconds, which corresponds to a projected separation of ~820 AU. The estimated semimajor axis of their orbit is 1,033 AU.[7] The secondary is a red dwarf star with a stellar classification of M1V.[3]

The primary star has a single known planetary companion, discovered in 2005.[7]

The HD 142022 planetary system[7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >4.47 MJ 2.93 1,928±46 0.53±0.20 — —

See also

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. 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.
  3. Gaidos, E.; et al. (September 2014). "Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life". Monthly Notices of the Royal Astronomical Society. 443 (3): 2561–2578. arXiv:1406.7353. Bibcode:2014MNRAS.443.2561G. doi:10.1093/mnras/stu1313.
  4. Gray, R. O.; et al. (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.
  5. Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. A76.
  6. "HD 142022". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-25.
  7. Eggenberger; et al. (2006). "The CORALIE survey for southern extrasolar planets XIV. HD 142022 b: a long-period planetary companion in a wide binary". Astronomy and Astrophysics. 447: 1159–1163. arXiv:astro-ph/0510561. Bibcode:2006A&A...447.1159E. doi:10.1051/0004-6361:20053720. Retrieved December 12, 2007.

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