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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 mas[1]
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, GCRV 65757[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. S2CID 119257644.
  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. S2CID 119234492.
  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. S2CID 119476992.
  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 (3): 1159–1163. arXiv:astro-ph/0510561. Bibcode:2006A&A...447.1159E. doi:10.1051/0004-6361:20053720. S2CID 18200070. Retrieved December 12, 2007.


На других языках

[de] HD 142022

HD 142022 A ist ein 112 Lichtjahre von der Erde entfernter später Hauptreihenstern mit einer Rektaszension von 16h 10m 15s und einer Deklination von −84° 13' 53". Er besitzt eine scheinbare Helligkeit von 7,7 mag. Im Jahre 2005 entdeckte Anne Eggenberger einen extrasolaren Planeten, der diesen Stern umkreist. Dieser trägt den Namen HD 142022 Ab. Weiterhin befindet sich in diesem System auch ein zweiter Stern mit dem Namen HD 142022 B, der HD 142022 A umkreist. Dies macht dieses System zu einem Doppelstern.
- [en] HD 142022

[ru] HD 142022

HD 142022 — двойная звезда, расположенная в созвездии Октант на расстоянии 117 световых лет от Земли. Первая звезда (HD 142022 A) имеет спектральный тип G9V и видимую звёздную величину в 7.69. Её масса на 1 % меньше, чем у Солнца, а радиус равен только 70,5 %.


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