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HD 10800

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HD 10800
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Octans
Right ascension 01h 37m 55.5567s[1]
Declination −82° 58′ 29.9867″[1]
Apparent magnitude (V) 5.87[2]
Characteristics
Spectral type G1 V[3]
U−B color index +0.10[2]
B−V color index +0.61[2]
Astrometry
Radial velocity (Rv)−1.1±0.4[4] km/s
Proper motion (μ) RA: +122.526 mas/yr[1]
Dec.: +120.827 mas/yr[1]
Parallax (π)37.0128 ± 0.229 mas[1]
Distance88.1 ± 0.5 ly
(27.0 ± 0.2 pc)
Absolute magnitude (MV)+3.69[5]
Orbit[6]
PrimaryAa
CompanionAb
Period (P)19.371 d
Eccentricity (e)0.103±0.001
Periastron epoch (T)2,456,938.6±0.02 JD
Argument of periastron (ω)
(primary)		243±0.4°
Semi-amplitude (K1)
(primary)		36.45±0.04 km/s
Semi-amplitude (K2)
(secondary)		43.32±0.05 km/s
Orbit[6]
PrimaryA
CompanionB
Period (P)1.7486±0.0005 yr
Semi-major axis (a)7.823±0.047 mas
Eccentricity (e)0.191±0.002
Inclination (i)47.6±0.5°
Periastron epoch (T)2,456,903.42±0.94 JD
Argument of periastron (ω)
(primary)		151.2±0.3°
Semi-amplitude (K1)
(primary)		9.1±0.03 km/s
Semi-amplitude (K2)
(secondary)		17.9±0.05 km/s
Details
Aa
Mass1.09[7] M☉
Radius1.1[8] R☉
Luminosity1.82±0.04[9] L☉
Surface gravity (log g)5[10] cgs
Temperature5,802[11] K
Metallicity [Fe/H]−0.09±0.11[12] dex
Rotational velocity (v sin i)7[7] km/s
Age5.01±4.51[9] Gyr
Ab
Mass0.64[13] M☉
B
Mass1±0.1[9] M☉
Luminosity0.98+0.25
−0.20[9] L☉
Temperature5,741[7] K
Age4.79+1.24
−0.98[9] Gyr
Other designations
3 G. Octantis[14], CPD−83°27, GC 2063, GJ 67.1, HD 10800, HIP 7601, HR 512, SAO 258271, WDS J01379-8259AB[15]
Database references
SIMBADdata

HD 10800, also known as HR 512 or Gliese 67.1, is a triple star located in the southern circumpolar constellation Octans. It has a combined apparent magnitude of 5.87,[2] allowing it to be faintly seen with the naked eye. The system is relatively close at a distance of 88.1 light years[1] but is drifting closer with a heliocentric radial velocity −1.1 km/s.[4]

The system has a blended spectral classification of G1 V,[3] indicating an ordinary G-type main-sequence star. The primary is a spectroscopic binary consisting of a G-type and K-type star circling around each other in 19 days.[6] HD 10800B has a class of G2 V,[9] the same spectral class as our own Sun. The AB pair take 1.7 years to orbit each other.[6]

HD 10800A

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The primary (Aa) has 109% the mass of the Sun[7] and a radius 1.1 times that of the Sun.[8] It radiates at 1.82 times the luminosity of the Sun[9] from its photosphere at an effective temperature of 5,802 K,[11] giving a yellow hue. HD 10800A has a metallicity 81% that of the Sun, making it slightly metal deficient.[12] At an age of 5 billion years,[9] it spins with a projected rotational velocity of 7 km/s.[7] The close companion (Ab) has a mass 69% that of the Sun.[13]

HD 10800B

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HD 10800B, the slightly distant companion, has the same mass of the Sun but is slightly cooler (37 K difference) and dimmer, with a luminosity 98% that of the Sun.[9] The object is only marginally older than the Sun at an age of 4.8 billion years.[9]

References

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  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ^ a b c d Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ^ a b Torres, C. A. O.; Quast, G. R.; da Silva, L.; de la Reza, R.; Melo, C. H. F.; Sterzik, M. (12 September 2006). "Search for associations containing young stars (SACY)". Astronomy & Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. eISSN 1432-0746. ISSN 0004-6361.
  4. ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN 1562-6873. ISSN 1063-7737. S2CID 119231169.
  5. ^ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  6. ^ a b c d Tokovinin, Andrei (20 June 2016). "Orbits of Four Young Triple-lined Multiple Systems". The Astronomical Journal. 152 (1): 11. arXiv:1604.06395. Bibcode:2016AJ....152...11T. doi:10.3847/0004-6256/152/1/11. eISSN 1538-3881.
  7. ^ a b c d e Nordström, B.; Mayor, M.; Andersen, J.; Holmberg, J.; Pont, F.; Jørgensen, B. R.; Olsen, E. H.; Udry, S.; Mowlavi, N. (May 2004). "The Geneva-Copenhagen survey of the Solar neighbourhood: Ages, metallicities, and kinematic properties of ~14 000 F and G dwarfs". Astronomy & Astrophysics. 418 (3): 989–1019. arXiv:astro-ph/0405198. Bibcode:2004A&A...418..989N. doi:10.1051/0004-6361:20035959. ISSN 0004-6361.
  8. ^ a b Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition -Comments and statistics". Astronomy and Astrophysics. 367 (2): 521–524. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451.
  9. ^ a b c d e f g h i j Piccotti, Luca; Docobo, José Ángel; Carini, Roberta; Tamazian, Vakhtang S; Brocato, Enzo; Andrade, Manuel; Campo, Pedro P (3 January 2020). "A study of the physical properties of SB2s with both the visual and spectroscopic orbits". Monthly Notices of the Royal Astronomical Society. 492 (2): 2709–2721. Bibcode:2020MNRAS.492.2709P. doi:10.1093/mnras/stz3616. eISSN 1365-2966. ISSN 0035-8711.
  10. ^ Piters, A. J.M.; van Paradijs, J.; Schmitt, J. H.M.M. (February 1998). "X-ray/optical observations of stars with shallow convection zones (A8 - G2 V)". Astronomy and Astrophysics Supplement Series. 128 (1): 29–33. Bibcode:1998A&AS..128...29P. doi:10.1051/aas:1998126. eISSN 1286-4846. ISSN 0365-0138.
  11. ^ a b Rocha-Pinto, H. J.; Maciel, W. J. (1 August 1998). "Metallicity effects on the chromospheric activity-age relation for late-type dwarfs". Monthly Notices of the Royal Astronomical Society. 298 (2): 332–346. arXiv:astro-ph/9803219. Bibcode:1998MNRAS.298..332R. doi:10.1046/j.1365-8711.1998.01597.x. eISSN 1365-2966. ISSN 0035-8711.
  12. ^ a b Netopil, Martin (4 May 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society. 469 (3): 3042–3055. arXiv:1705.00883. Bibcode:2017MNRAS.469.3042N. doi:10.1093/mnras/stx1077. eISSN 1365-2966. ISSN 0035-8711.
  13. ^ a b Tokovinin, Andrei (14 March 2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 87. arXiv:1401.6827. Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87. eISSN 1538-3881. ISSN 0004-6256.
  14. ^ Gould, B. A. "Uranometria Argentina". Reprinted and updated by Pilcher, F. Archived from the original on 2012-02-27. Retrieved 2012-01-06.
  15. ^ "HR 512". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved July 28, 2022.
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