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36 Andromedae

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36 Andromedae
Location of 36 Andromedae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 00h 54m 58.10609s[1]
Declination +23° 37′ 41.9799″[1]
Apparent magnitude (V) 5.45[2] (6.12 + 6.54)[3]
Characteristics
Spectral type G8 IV + K3 IV[4]
B−V color index 1.012±0.010[5]
Astrometry
Radial velocity (Rv)−0.84±0.12[6] km/s
Proper motion (μ) RA: 135.43±1.00 mas/yr[1]
Dec.: −48.61±0.48 mas/yr[1]
Parallax (π)26.33±0.65 mas[1]
Distance124 ± 3 ly
(38.0 ± 0.9 pc)
Absolute magnitude (MV)2.56[5]
Orbit[7]
Primary36 And A
Companion36 And B
Period (P)169.08±0.37 yr
Semi-major axis (a)0.9847″±0.0017″
(37 AU)[a]
Eccentricity (e)0.3092±0.0014
Inclination (i)44.80±0.18°
Longitude of the node (Ω)173.60±0.32°
Periastron epoch (T)1956.23±0.17
Argument of periastron (ω)
(secondary)		359.0±0.6°
Details
36 And A
Mass1.45[8] M☉
Radius3.71[9] R☉
Luminosity7.75[9] L☉
Temperature5,000[9] K
36 And B
Mass1.34[8] M☉
Other designations
36 And, NSV 343, BD+22°146, HD 5286, HIP 4288, HR 258, SAO 74359, PPM 90284, ADS 755, WDS J00550+2338AB[10]
Database references
SIMBADdata

36 Andromedae is a binary star system in the northern constellation of Andromeda, which is part of a triple star system.[8] The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is faintly visible to the naked eye with an apparent visual magnitude of 5.45.[2] An annual parallax shift of 26.33 mas yields a distance estimate of about 124 light years. The system is moving closer to the Sun with a radial velocity of −0.8 km/s.[6]

Characteristics

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The binary nature of 36 Andromedae was discovered in 1832 by the German-Russian astronomer Wilhelm von Struve.[4] It is a wide binary with an orbital period of 169.1 years and an eccentricity of 0.31. Their semi-major axis is of 37 astronomical units (au), larger than that of Neptune.[7][a] As of 2016, the pair had an angular separation of 0.90 arc seconds along a position angle of 330°.[3]

The primary, component A, is a magnitude 6.12[3] G-type star with a stellar classification of G8 IV,[4] while the secondary, component B, has a magnitude of 6.54[3] and is a K-type star of class K3 IV.[4] Their brightness compared to their temperatures indicate they are evolving subgiant stars. However, at least one of the components is subject to flare activity, which may suggest they are instead pre-main sequence stars.[4]

36 Andromedae makes part of a triple star system. A third star, which shares a common proper motion with the inner pair and hence is believed to form a triple system, is separated by the AB pair by 1,407" (0.39°). At the system's distance, this implies a projected separation of 53,000 astronomical units (0.84 light-years)[b] and an estimated orbital period of seven million years. It is a K-type main-sequence star with 0.68 times the mass of the Sun and an apparent magnitude of 10.92.[8]

Notes

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  1. ^ a b Calculated from angular separation of 0.9847″[7] and distance of 38.0 parsecs.[1]
  2. ^ Calculated from angular separation of 1,407″[8] and distance of 38.0 parsecs.[1]

References

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  1. ^ a b c d e f van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.Vizier catalog entry
  2. ^ a b 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 c d Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
  4. ^ a b c d e Tamazian, V. S.; et al. (November 2000), "Spectral, photometric and speckle observations of visual binary WDS 00550+2338", Astronomy and Astrophysics, 363: 1019−1025, Bibcode:2000A&A...363.1019T.
  5. ^ a b 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.
  6. ^ a b Famaey, B.; et al. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165–186. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  7. ^ a b c Izmailov, Igor; Khovritchev, Maxim (January 2025), "New Orbital Parameters of 850 Wide Visual Binary Stars and Their Statistical Properties", Research in Astronomy and Astrophysics, 25 (1): 015016, Bibcode:2025RAA....25a5016I, doi:10.1088/1674-4527/ad9da3, ISSN 1674-4527 36 Andromedae's database entry at VizieR.
  8. ^ a b c d e Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. 36 Andromedae's database entry at VizieR.
  9. ^ a b c 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.
  10. ^ "36 And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-02.
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