HD 10800

Last updated
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]
Distance 88.1 ± 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
Mass 1.09 [7]   M☉
Radius 1.1 [8]   R☉
Luminosity 1.82±0.04 [9]   L☉
Surface gravity (log g)5 [10]   cgs
Temperature 5,802 [11]   K
Metallicity [Fe/H]−0.09±0.11 [12]   dex
Rotational velocity (v sin i)7 [7]  km/s
Age 5.01±4.51 [9]   Gyr
Ab
Mass 0.64 [13]   M☉
B
Mass 1±0.1 [9]   M☉
Luminosity 0.98+0.25
−0.20 [9]   L☉
Temperature 5,741 [7]   K
Age 4.79+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
SIMBAD data

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]

Contents

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

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

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]

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<span class="mw-page-title-main">HD 27245</span> Star in the constellation Camelopardalis

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HD 27274, also known as Gliese 167, is a solitary, orange hued star located in the southern constellation Dorado. It has an apparent magnitude of 7.63, making it readily visible in binoculars, but not to the naked eye. Based on parallax measurements from the Gaia spacecraft, the star is known to be located 42.5 light-years away from the Solar System However, it is drifting closer with a heliocentric radial velocity of −23 km/s. At its current distance, HD 27274 is dimmed down by 0.05 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 24479</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">2 Piscis Austrini</span> Star in the constellation Microscopium

2 Piscis Austrini, also known as HD 200763 or simply 2 PsA, is a solitary orange hued star located in the southern constellation Microscopium. It was once part of Piscis Austrinus, the southern fish. The object has an apparent magnitude of 5.2, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, it is estimated to be 354 light years away from the Solar System. However, it is receding with a poorly constrained heliocentric radial velocity of 3.1 km/s. At its current distance, 2 PsA's brightness is diminished by 0.11 magnitudes due to interstellar dust. It has an absolute magnitude of 0.19.

<span class="mw-page-title-main">S Apodis</span> Variable star in the constellation Apus

S Apodis, also known as HD 133444 is a variable star located in the southern circumpolar constellation Apus. It has an apparent magnitude ranging from 9.6 to 17, which is below the limit for naked eye visibility. The object is located relatively far at a distance of approximately 15,000 light years based on Gaia DR3 parallax measurements, but it is drifting closer with a heliocentric radial velocity of −75 km/s.

<span class="mw-page-title-main">HD 61005</span> Star in the constellation Puppis

HD 61005, also known as HIP 36948 and The Moth, is a young star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 8.22, making it readily visible in binoculars, but not to the naked eye. The object is located relatively close at a distance of 119 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 22.6 km/s.

<span class="mw-page-title-main">HD 90132</span> Solitary White-hued star and high proper motion star

HD 90132 is a solitary white hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.33, making it one of the brighter members of this generally faint constellation. The star is relatively close at a distance of 135 light years but is receding with a heliocentric radial velocity of 17 km/s.

<span class="mw-page-title-main">14 Trianguli</span> Star in the constellation Triangulum

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HD 89571 is a binary star located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye with a combined apparent magnitude of 5.51 and is estimated to be 142 light years away from the Solar System. However, it is receding with a heliocentric radial velocity of 3.5 km/s.

HD 208741, also known as HR 8380, is a yellowish-white hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.91, making it faintly visible to the naked eye. Parallax measurements place it at a distance of 211 light years, and it is currently receding with a heliocentric radial velocity of 8 km/s.

HD 34255, also known HR 1720, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.60, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of about 1.65 kly but is approaching the Solar System with a heliocentric radial velocity of −7.7 km/s.

HD 50885, also known as HR 2581, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.69, making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from Gaia DR3, the object is estimated to be 513 light years distant. It appears to be approaching the Solar System with a heliocentric radial velocity of −17.8 km/s.

HR 8526, also known as HD 212168, is the primary of a triple star located in the southern circumpolar constellation Octans. The star and its companion have apparent magnitudes of 6.12 and 9.36 respectively. The system is located relatively close at a distance of 76 light years based on Gaia DR3 parallax measurements, but is receding with a heliocentric radial velocity of 15 km/s.

<span class="mw-page-title-main">HD 201772</span> Star in the constellation Microscopium

HD 201772, also known as HR 8104, is a yellowish-white hued star located in the southern constellation Microscopium. It has an apparent magnitude of 5.26, making it one of the brighter members of this generally faint constellation. The object is located relatively close at a distance of 111 light-years based on Gaia DR3 parallax measurements but is approaching closer with a heliocentric radial velocity of −41 km/s. At its current distance, HD 201772's brightness is diminished by 0.11 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 117566</span> High proper motion star; Camelopardalis

HD 117566, also known as HR 5091, is a solitary yellow-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.74, making it faintly visible to the naked eye. This object is relatively close at a distance of 291 light years based on Gaia DR3 parallax measurements but is receding with a heliocentric radial velocity of 14 km/s. At its current distance, HD 117566's brightness is diminished by 0.12 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 197630</span> Star in the constellation of Microscopium

HD 197630, also known as HR 7933 or rarely 23 G. Microscopii, is a probable astrometric binary located in the southern constellation Microscopium. The visible component is a bluish-white hued star that is faintly visible to the naked eye with an apparent magnitude of 5.47. Based on parallax measurements from the Gaia satellite, the system is estimated to be 328 light years away. However, it is drifting closer with a heliocentric radial velocity of −30 km/s. At its current distance, HD 197630's brightness is diminished by 0.11 magnitudes due to interstellar dust. A 2012 multiplicity survey failed to confirm the velocity variations.

<span class="mw-page-title-main">HD 190422</span> F-type main-sequence star; Telescopium

HD 190422, also known as HR 7674 or rarely 77 G. Telescopii, is a solitary star located in the southern constellation Telescopium. It has an apparent magnitude of +6.25, placing it near the limit for naked eye, even under ideal conditions. At its current distance, HD 190422's brightness is diminished by 0.11 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of +4.41.

<span class="mw-page-title-main">HD 24141</span> Am star?; Camelopardalis

HD 24141, also known as HR 1192, is a star located in the northern constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.79. The object is located relatively close at a distance of 176 light-years based on Gaia DR3 parallax measurements and it is slowly drifting closer with a heliocentric radial velocity of −0.2 km/s. At its current distance, HD 24141's brightness is diminished by 0.17 magnitudes due to interstellar extinction and it has an absolute magnitude of +2.28.

<span class="mw-page-title-main">HD 84607</span> F-type subgiant; Sextans

HD 84607 is a solitary star located in the equatorial constellation Sextans. It is faintly visible to the naked eye as a yellowish-white hued point of light with an apparent magnitude of 5.64. The object is located relatively close at a distance of 250 light-years based on Gaia DR3 parallax measurements, but it is receding with a heliocentric radial velocity of 7.8 km/s. At its current distance, HD 84607's brightness is diminished by an interstellar extinction of 0.18 magnitudes and it has an absolute magnitude +1.12.

References

  1. 1 2 3 4 5 6 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. 1 2 3 4 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. 1 2 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. 1 2 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.
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  7. 1 2 3 4 5 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. 1 2 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. 1 2 3 4 5 6 7 8 9 10 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.
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  12. 1 2 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. 1 2 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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