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Pi Andromedae

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Binary star system in the constellation Andromeda
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Pi Andromedae
Location of π Andromedae (circled)
Observation data
Epoch J2000Equinox ICRS
Constellation Andromeda
Right ascension 00h 36m 52.85132s[1]
Declination +33°43′09.6363′′[1]
Apparentmagnitude(V) 4.36[2] (4.9/5.3)[3]
Characteristics
Spectraltype B5V[4] (B5 V + B5 V[3] )
U−B color index −0.55[2]
B−V color index −0.16[2]
Astrometry
Radial velocity (Rv)+8.7[5] km/s
Proper motion (μ) RA:14.669(118) mas/yr [1]
Dec.:−3.385(93) mas/yr [1]
Parallax (π)5.6563±0.1474mas [1]
Distance 580 ± 20ly
(177 ± 5pc)
Orbit [6]
Period (P)143.53±0.06d
Semi-major axis (a)6.69±0.05mas
Eccentricity (e)0.542±0.006
Inclination (i)103.0±0.2°
Longitude of the node (Ω)94.7±0.2°
Periastron epoch (T)7717.7±0.4
Argument of periastron (ω)
(secondary)		170.7±0.7°
Semi-amplitude (K1)
(primary)		47.50±0.53km/s
Semi-amplitude (K2)
(secondary)		117.4±2.8km/s
Details[7]
A
Mass 5.8[6] M☉
Radius 4.7R☉
Luminosity 1,000L☉
Surface gravity (logg)4.10[4] cgs
Temperature 15,000K
Metallicity [Fe/H]–0.20[4] dex
Rotational velocity (vsini)25[8] km/s
Age 80Myr
B
Mass 4.8[6] M☉
Radius 4.7R☉
Luminosity1,000L☉
Temperature 15,000K
Other designations
PiAnd, πAndromedae, πAnd, 29 Andromedae, BD+32°101, FK5 18, HD 3369, HIP 2912, HR 154, SAO 54033, PPM 65480, ADS 513
Database references
SIMBAD data

Pi Andromedae is a binary star [3] system in the northern constellation of Andromeda. Its Bayer designation is latinized from π Andromedae, and abbreviated Pi And or π And, respectively. With an apparent visual magnitude of 4.4,[2] it is visible to the naked eye. Based on parallax measurements, it is located at a distance of approximately 580 light-years (180 parsecs ) from Earth.[1]

π Andromedae in optical light

The pair is classified as a blue-white B-type main sequence dwarf, with an apparent magnitude of +4.34. It is a spectroscopic binary with an orbital period of 143.5 days and an eccentricity of 0.54.[6]

The spectroscopic binary forms a triple system with BD+32 102, a magnitude 8.6 star located 35.9 arcseconds away.[3] At 55 arcseconds separation is an 11th magnitude companion that is just located on the same line of sight, but at a very different distance from us.

Naming

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In Chinese, 奎宿 (Kuí Sù), meaning Legs (asterism), refers to an asterism consisting of π Andromedae, η Andromedae, 65 Piscium, ζ Andromedae, ε Andromedae, δ Andromedae, ν Andromedae, μ Andromedae, β Andromedae, σ Piscium, τ Piscium, 91 Piscium, υ Piscium, φ Piscium, χ Piscium and ψ1 Piscium. Consequently, the Chinese name for π Andromedae itself is 奎宿六 (Kuí Sù liù, English: the Sixth Star of Legs.)[9]

References

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  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 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. 1 2 3 4 Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x . S2CID 14878976.
  4. 1 2 3 Cenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters", Monthly Notices of the Royal Astronomical Society , 374 (2): 664–690, arXiv:astro-ph/0611618 , Bibcode:2007MNRAS.374..664C, doi:10.1111/j.1365-2966.2006.11196.x , S2CID 119428437.
  5. ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  6. 1 2 3 4 Hummel, C. A.; et al. (July 1995). "Orbits of Small Angular Scale Binaries Resolved with the Mark III Interferometer". Astronomical Journal. 110: 376. Bibcode:1995AJ....110..376H. doi:10.1086/117528.
  7. ↑ "Pi And". stars.astro.illinois.edu. Retrieved 2025年02月06日.
  8. ↑ Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590 .
  9. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 19 日 Archived 2016年03月03日 at the Wayback Machine
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