13 Andromedae

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13 Andromedae
Andromeda constellation map.svg
Red circle.svg
Location of 13 Andromedae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 23h 27m 07.40s [1]
Declination +42° 54′ 43.2″ [1]
Apparent magnitude  (V)5.75 [2]
Characteristics
Spectral type B9 III or B9 Mn [3]
B−V color index −0.007±0.004 [2]
Variable type α2 CVn [4]
Astrometry
Radial velocity (Rv)−8.1±1.6 [5] km/s
Proper motion (μ)RA: 87.05 [1] mas/yr
Dec.: 16.54 [1] mas/yr
Parallax (π)10.87±0.30  mas [1]
Distance 300 ± 8  ly
(92 ± 3  pc)
Absolute magnitude  (MV)0.98 [6]
Details
Luminosity 42.89 [2]   L☉
Rotational velocity (v sin i)75 [7]  km/s
Age 345 [6]   Myr
Other designations
13 And, V388 Andromedae, BD+42°4672, HD 220885, HIP 115755, HR 8913, SAO 53039, PPM 64250 [8]
Database references
SIMBAD data
The visual band light curve of 13 Andromedae, adapted from Adelman (2005) 13AndLightCurve.png
The visual band light curve of 13 Andromedae, adapted from Adelman (2005)

13 Andromedae, abbreviated 13 And, is a single, [10] blue-white hued variable star [4] in the northern constellation of Andromeda. 13 Andromedae is the Flamsteed designation, while it bears the variable star designation V388 Andromedae. With a typical apparent visual magnitude of around 5.75, [2] it is dimly visible to the naked eye under good seeing conditions. The distance to this star can be directly estimated from its annual parallax shift of 10.9  mas , [1] yielding a range of 300  light years. At that distance, its brightness is diminished by an extinction of 0.13 magnitude due to interstellar dust. [6] The star is moving closer to the Earth with a heliocentric radial velocity of −8 km/s. [5]

The variability of 13 Andromedae was first detected in Hipparcos satellite data, and it received its variable star designation in 1999. [11] [12]

This is a magnetic chemically peculiar star that has been assigned stellar classifications of B9 III or B9  Mn. [3] It is a variable star of the Alpha2 Canum Venaticorum type, ranging in magnitude from 5.73 down to 5.77 [4] with a period of 1.47946 days. [3] The star has a high rate of spin, showing a projected rotational velocity of 75 km/s. [7] 13 Andromedae is around 345 [6]  million years old and shines with 43 [2] times the Sun's luminosity.

References

  1. 1 2 3 4 5 6 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 .
  2. 1 2 3 4 5 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.
  3. 1 2 3 Adelman, Saul J. (May 2005), "uvby FCAPT Photometry of the Magnetic Chemically Peculiar Stars 36 Aurigae, HR 2722, 13 Andromedae, and HD 220147", The Publications of the Astronomical Society of the Pacific, 117 (831): 476–482, Bibcode:2005PASP..117..476A, doi: 10.1086/429640 .
  4. 1 2 3 Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  5. 1 2 Gontcharov, G. A. (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, S2CID   119231169.
  6. 1 2 3 4 Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv: 1606.09028 , Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035, S2CID   119108982.
  7. 1 2 Abt, Helmut A.; et al. (2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi: 10.1086/340590 .
  8. ↑ "13 And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 19, 2018.
  9. ↑ Adelman, Saul J. (May 2005). "uvby FCAPT Photometry of the Magnetic Chemically Peculiar Stars 36 Aurigae, HR 2722, 13 Andromedae, and HD 220147". Publications of the Astronomical Society of the Pacific. 117 (831): 476–482. Bibcode:2005PASP..117..476A. doi: 10.1086/429640 . S2CID   120788302.
  10. ↑ 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.
  11. ↑ Paunzen, E.; Maitzen, H. M. (November 1998). "New variable chemically peculiar stars identified in the HIPPARCOS archive" (PDF). Astronomy and Astrophysics Supplement. 133: 1–6. Bibcode:1998A&AS..133....1P. doi:10.1051/aas:1998305 . Retrieved 5 November 2024.
  12. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (January 1999). "The 74th Special Name-list of Variable Stars" (PDF). Information Bulletin on Variable Stars. 4659: 1. Bibcode:1999IBVS.4659....1K . Retrieved 5 November 2024.
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