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HD 106906 is a binary star[6] system in the southern constellation of Crux. It is too faint to be visible to the naked eye, having a combined apparent visual magnitude of 7.80.[2] The distance to this system is approximately 337 light years based on parallax, and it is receding from the Sun with a radial velocity of +10 km/s.[2] It is a member of the Lower Centaurus–Crux group of the Scorpius–Centaurus OB association of co-moving stars.[4]

HD 106906

Star map shows star position on the northern edge of the constellation Crux
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Crux
Right ascension 12h 17m 53.191430s[1]
Declination −55° 58′ 31.8904″[1]
Apparent magnitude (V) 7.80[2]
Characteristics
Spectral type F5 V[3]
B−V color index 0.458±0.003[2]
Astrometry
Radial velocity (Rv)+10.2±1.7[2] km/s
Proper motion (μ) RA: −39.014[1] mas/yr
Dec.: −12.872[1] mas/yr
Parallax (π)9.6774 ± 0.0429 mas[1]
Distance337 ± 1 ly
(103.3 ± 0.5 pc)
Absolute magnitude (MV)2.99[2]
Details
Radius2.03+0.11
−0.10[1] R☉
Luminosity6.56±0.04[1] L☉
Temperature6,484+157
−168[1] K
Metallicity [Fe/H]−0.04±0.08[2] dex
Age13±2[4] Myr
Other designations
CD−55°4537, HD 106906, HIP 59960, SAO 239819, 2MASS J12175319-5558319[5]
Database references
SIMBADdata

This is a double-lined spectroscopic binary system consisting of two F-type main-sequence stars with similar masses and a matching stellar classification of F5 V.[6] Their orbital period is less than 100 days.[4]


Planetary system


A distant circumbinary planet—HD 106906 b—is orbiting the pair at a projected separation of 732±30 AU with a period of at least 3,000 years. An infrared excess around the binary is coming from a circumstellar debris disk that is being viewed edge-on. This has a pronounced asymmetrical shape, extending 120 AU on the east side and out to 550 AU to the west.[4] Planetary orbit is inclined to the debris disk by 39+20
−15 degrees, and planet itself is visible nearly pole-on, having a large axial tilt.[7]

The HD 106906 planetary system[8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
debris disk 65–550 AU 84.65±0.35° —
b 11±2 MJ ~2600 >3000 — 64° —

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. Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  4. Rodet, L.; et al. (June 2017), "Origin of the wide-orbit circumbinary giant planet HD 106906. A dynamical scenario and its impact on the disk", Astronomy & Astrophysics, 602: 15, arXiv:1703.01857, Bibcode:2017A&A...602A..12R, doi:10.1051/0004-6361/201630269, S2CID 119424481, A12.
  5. "HD 106906". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-01-30.
  6. Lagrange, A. -M.; et al. (February 2016), "A narrow, edge-on disk resolved around HD 106906 with SPHERE", Astronomy & Astrophysics, 586: 6, arXiv:1510.02511, Bibcode:2016A&A...586L...8L, doi:10.1051/0004-6361/201527264, S2CID 4812512, L8.
  7. Obliquity Constraints on the Planetary-mass Companion HD 106906 b, 2021, arXiv:2108.13437, doi:10.3847/1538-3881/ac1bb1
  8. Kalas, Paul G.; et al. (2015), "Direct Imaging of an Asymmetric Debris Disk in the Hd 106906 Planetary System", The Astrophysical Journal, 814 (1): 32, arXiv:1510.02747, Bibcode:2015ApJ...814...32K, doi:10.1088/0004-637X/814/1/32, S2CID 59575201

На других языках

[de] HD 106906

HD 106906 (HIP 59960) ist ein 300 Lichtjahre von der Erde entfernter und nur etwa 13 Millionen Jahre alter Doppelstern.[5] Das binäre System besteht aus zwei Sternen des Spektraltyps F5V, die die Hauptreihe noch nicht erreicht haben. Die kombinierte Magnitude liegt bei 7,80.[6] Die beiden Sterne haben eine vergleichbare Masse, zusammen etwa die 1,5-fache Sonnenmasse. Ihre Umlaufszeit beträgt weniger als 100 Tage.[7] Der Doppelstern gehört zur Lower-Centaurus-Crux (LCC)-Gruppe, einem Teil der Scorpius-Centaurus-Assoziation[7] und wurde ab dem Jahr 2005 am Magellan-Teleskop am Las-Campanas-Observatorium in Chile beobachtet, nachdem in frühen Beobachtungen des Spitzer-Weltraumteleskops ein Infrarotexzess gefunden wurde.
- [en] HD 106906

[ru] HD 106906

HD 106906 — двойная звёздная[6] система в созвездии Южного Креста. Находится на расстоянии около 337 световых лет от Солнца


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