Psi Andromedae
Diagram showing star positions and boundaries of the Andromeda constellation and its surroundings
Location of ψ Andromedae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 23h 46m 02.04703s[1]
Declination +46° 25′ 12.9865″[1]
Apparent magnitude (V) 4.95[2]
Characteristics
Spectral type G5 Ib[3] + B9[4]
U−B color index +0.83[2]
B−V color index +1.085[3]
Astrometry
Radial velocity (Rv)-23.62[3] km/s
Proper motion (μ) RA: 8.446(132)[1] mas/yr
Dec.: −7.143(109)[1] mas/yr
Parallax (π)1.6352 ± 0.1627 mas[1]
Distance2,000 ± 200 ly
(610 ± 60 pc)
Absolute magnitude (MV)–3.039[3]
Details
ψ And A
Mass5.4[4] M☉
Radius686[5] R☉
Surface gravity (log g)1.50[3] cgs
Temperature4,990[3] K
Metallicity [Fe/H]+0.10[3] dex
Age79[4] Myr
Other designations
20 And, BD+45° 4321, FK5 1622, HD 223047, HIP 117221, HR 9003, SAO 53355, PPM 64635[6]
Database references
SIMBADdata

Psi Andromedae (ψ And, ψ Andromedae) is the Bayer designation for a triple star[4] system in the northern constellation of Andromeda. The combined apparent visual magnitude of this system is 4.95.[2] Based upon parallax measurements, is roughly 2,000 light-years (610 parsecs) from Earth, with a large margin of error.[1]

The primary component has a stellar classification of G5 Ib,[3] which matches the spectrum of an evolved supergiant star. It forms a pair with a star of type B9 with an unknown luminosity class separated by 0.28 arcseconds. A third component has a separation of 0.14 arcseconds. Details of the orbital arrangement remain uncertain.[4]

Naming

In Chinese, 螣蛇 (Téng Shé), meaning Flying Serpent, refers to an asterism consisting of ψ Andromedae, α Lacertae, 4 Lacertae, π2 Cygni, π1 Cygni, HD 206267, ε Cephei, β Lacertae, σ Cassiopeiae, ρ Cassiopeiae, τ Cassiopeiae, AR Cassiopeiae, 9 Lacertae, 3 Andromedae, 7 Andromedae, 8 Andromedae, λ Andromedae, κ Andromedae and ι Andromedae,. Consequently, the Chinese name for ψ Andromedae itself is 螣蛇二十 (Téng Shé èrshí, English: the Twentieth of Flying Serpent).[7]

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 Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133 (4): 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475.
  3. 1 2 3 4 5 6 7 8 Soubiran, C.; et al. (March 2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID 16602121.
  4. 1 2 3 4 5 Parsons, Sidney B. (May 2004), "New and Confirmed Triple Systems with Luminous Cool Primaries and Hot Companions", The Astronomical Journal, 127 (5): 2915–2930, Bibcode:2004AJ....127.2915P, doi:10.1086/383546.
  5. ↑ Stassun K.G.; et al. (October 2019). "The revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. S2CID 166227927.
  6. ↑ "* psi And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 January 2018.
  7. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 7 日
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