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Lambda Andromedae

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Lambda Andromedae
Location of λ Andromedae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 23h 37m 33.84278s[1]
Declination +46° 27′ 29.3447″[1]
Apparent magnitude (V) 3.65 - 4.05[2]
Characteristics
Evolutionary stage subgiant[3]
Spectral type G8 III-IV[4] or G8 IV[3]
U−B color index +0.688[5]
B−V color index +0.996[5]
Variable type RS CVn[2]
Astrometry
Radial velocity (Rv)+6.8[6] km/s
Proper motion (μ) RA: 159.606(101)[1] mas/yr
Dec.: −421.822(97)[1] mas/yr
Parallax (π)38.5736 ± 0.1179 mas[1]
Distance84.6 ± 0.3 ly
(25.92 ± 0.08 pc)
Absolute magnitude (MV)1.91[7]
Details
Mass1.24±0.72[8] M☉
Radius7.787±0.053[8] R☉
Luminosity28.8[8] L☉
Surface gravity (log g)2.75±0.25[4] cgs
Temperature4,800±100[4] K
Metallicity [Fe/H]−0.56[9] dex
Rotation54 d[4]
Rotational velocity (v sin i)7.3[10] km/s
Other designations
λ And, 16 Andromedae, BD+45°4283, FK5 890, GJ 9832, HD 222107, HIP 116584, HR 8961, SAO 53204, PPM 64456, LTT 16964, NLTT 57442[11]
Database references
SIMBADdata

Lambda Andromedae, Latinized from λ Andromedae, is the Bayer designation for a binary star system in the northern constellation of Andromeda. At an estimated distance of approximately 84.6 light-years (25.9 parsecs) from Earth,[1] it has an apparent visual magnitude of +3.8.[5] This is bright enough to be seen with the naked eye. The system is drifting further away from the Sun with a radial velocity of +6.8 km/s.[6]

Properties

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A light curve for Lambda Andromedae, plotted from Hipparcos data[12]

Lambda Andromedae is a single-lined spectroscopic binary with an orbital period of 20.5212 days.[13] The spectrum of the primary matches a stellar classification of G8 III-IV, suggesting that it is an evolved star that lies part way between the subgiant and giant stages. The mass of this star is similar to the Sun, but it has expanded to around seven times the Sun's radius. It is radiating over 28[8] times the luminosity of the Sun from its outer envelope at an effective temperature of 4,800 K,[4] giving it the characteristic yellow hue of a G-type star.

This is an RS Canum Venaticorum variable and its brightness varies by 0.225 magnitudes, reaching a maximum of 3.70, with a period of 53.952 days.[13] The companion is a low-mass star with a mass of 0.15 M☉.[8] Such variability is theorized to occur because of tidal friction, which results in chromospheric activity. However, the orbit of this system is nearly circular, so the cause of this system's variability remains uncertain.[13] The X-ray luminosity of this star, as measured by the ROSAT satellite, is 2.95 × 1030 erg s−1.[4] A magnetic field with an average strength of 21 G has been detected on this star, which is stronger than the field on the Sun.[3]

Naming

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λ Andromedae in optical light

In Chinese, 螣蛇 (Téng Shé), meaning Flying Serpent, refers to an asterism consisting of λ 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, κ Andromedae, ι Andromedae, and ψ Andromedae. Consequently, the Chinese name for λ Andromedae itself is 螣蛇十九 (Téng Shé shíjiǔ, English: the Nineteenth Star of Flying Serpent).[14]

Evolution

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Many different spectral classes have been published for λ Andromedae, ranging from G6 to K1. Most sources give a luminosity class of III (giant) or IV (subgiant).[15] Analysis of the physical properties of the star, including its temperature, luminosity, magnetic field, and stellar wind, show that it has recently experienced the first dredge-up and has begun to ascend the red giant branch although it still has a hot corona and is classified as a subgiant by some definitions.[4][3]

References

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  1. ^ a b c d e f 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 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ^ a b c d Ó Fionnagáin, D.; Vidotto, A. A.; Petit, P.; Neiner, C.; Manchester IV, W.; Folsom, C. P.; Hallinan, G. (January 2021), "λ And: a post-main-sequence wind from a solar-mass star", Monthly Notices of the Royal Astronomical Society, 500 (3): 3438–3453, arXiv:2011.02406, Bibcode:2021MNRAS.500.3438O, doi:10.1093/mnras/staa3468.
  4. ^ a b c d e f g Drake, Jeremy J.; et al. (November 2011), "Close to the dredge: precise X-Ray C and N abundances in λ Andromeda and its precocious red giant branch mixing problem", The Astronomical Journal, 142 (5): 144, arXiv:1109.3663, Bibcode:2011AJ....142..144D, doi:10.1088/0004-6256/142/5/144, S2CID 118271341.
  5. ^ a b c Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants.", Monthly Notices of the Royal Astronomical Society, 172 (3): 667–679, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667.
  6. ^ a b 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.
  7. ^ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999), "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity", Astronomy and Astrophysics, 343: 222–228, Bibcode:1999A&A...343..222E.
  8. ^ a b c d e Martinez, Arturo O.; Baron, Fabien R.; Monnier, John D.; Roettenbacher, Rachael M.; Parks, J. Robert (2021). "Dynamical Surface Imaging of λ Andromedae". The Astrophysical Journal. 916 (1): 60. arXiv:2107.06366. Bibcode:2021ApJ...916...60M. doi:10.3847/1538-4357/ac06a5. S2CID 235829649.
  9. ^ Mallik, Sushma V. (December 1999), "Lithium abundance and mass", Astronomy and Astrophysics, 352: 495–507, Bibcode:1999A&A...352..495M.
  10. ^ Massarotti, Alessandro; et al. (January 2008), "Rotational and radial velocities for a sample of 761 HIPPARCOS giants and the role of binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
  11. ^ "lam And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-06-21.{{cite web}}: CS1 maint: postscript (link)
  12. ^ "/ftp/cats/more/HIP/cdroms/cats". Centre de Données astronomiques de Strasbourg. Strasbourg astronomical Data Center. Retrieved 15 October 2022.
  13. ^ a b c Frasca, A.; et al. (February 2008), "Spots, plages, and flares on λ Andromedae and II Pegasi", Astronomy and Astrophysics, 479 (2): 557–565, arXiv:0711.3322, Bibcode:2008A&A...479..557F, doi:10.1051/0004-6361:20077915, S2CID 8049649.
  14. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 7 日 Archived 2011-05-21 at the Wayback Machine
  15. ^ Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009–2016)". VizieR On-line Data Catalog. Bibcode:2014yCat....1.2023S.
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