Astronomy:CN Andromedae

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Short description: Star in the constellation Andromeda
CN Andromedae
CNAndLightCurve.png
The visual band light curve of CN Andromedae, adapted from a plot presented by Varol Keskin[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  00h 20m 30.54209s[2]
Declination +40° 13′ 33.80342″[2]
Apparent magnitude (V) 9.62 – 10.21 variable [3]
Characteristics
Spectral type F5V[3]
Apparent magnitude (B) 10.24[4]
Apparent magnitude (V) 9.706[4]
Apparent magnitude (G) 9.6637[2]
Apparent magnitude (J) 8.670[5]
Apparent magnitude (H) 8.452[5]
Apparent magnitude (K) 8.427[5]
B−V color index 0.49725[4]
Variable type EB[3]
Astrometry
Radial velocity (Rv)−24.2±1.0[6] km/s
Proper motion (μ) RA: −8.549±0.054 [2] mas/yr
Dec.: −35.291±0.024[2] mas/yr
Parallax (π)4.9670 ± 0.0425[2] mas
Distance657 ± 6 ly
(201 ± 2 pc)
Orbit[6]
Period (P)0.4627952±0.000035 days
Semi-major axis (a)3.066±0.035
Inclination (i)68.51±0.17°
Periastron epoch (T)HJD 2445231.51710±0.00059
Details
Primary
Mass1.433±0.030[7] M☉
Radius1.48±0.03[7] R☉
Luminosity3.40[7] L☉
Surface gravity (log g)4.24[6] cgs
Temperature6,450[7] K
Secondary
Mass0.552±0.020[7] M☉
Radius0.95[7] R☉
Luminosity0.40[7] L☉
Surface gravity (log g)4.22[6] cgs
Temperature4,726[7] K
Other designations
2MASS J00203054+4013337, BD+39 59, TYC 2787-1815-1
Database references
SIMBADdata

CN Andromedae (CN And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.62 and drops down to a minimum of 10.2 during the main eclipse. It is classified as a Beta Lyrae variable with a period roughly of 0.4628 days.[3]

System

The two stars in this system orbit very close to each other; their spectrum cannot be separated and as a whole they have a spectrum of an F5V star. They are in marginal contact,[7] and there is a mass flow from the primary star to the secondary at a rate of 1.4 × 10−7 M☉ yr−1.[6] The binary orbit is slowly decaying at rate 1.5*10−7 days/year. The third suspected component of the system is the red dwarf star with mass about 0.11 M☉, at 38±4 years orbit around binary. [8]

Variability

The light curve of CN Andromedae shows a primary eclipse, with its brightness dropping down to 10.21 magnitude, and a secondary one down to a magnitude of 9.9.[3] This phenomenon repeats with a cycle of approximately 11.1 hours, with period decreasing in time due to the mass transfer from one star to the other.[6]

References

  1. ↑ Keskin, Varol (March 1989). "Light Changes of the Close Binary System CN Andromedae". Astrophysics and Space Science 153 (2): 191–199. doi:10.1007/BF00636655. Bibcode: 1989Ap&SS.153..191K. http://articles.adsabs.harvard.edu/pdf/1989Ap%26SS.153..191K. Retrieved 7 October 2021. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 3.4 CN And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2018-10-17.
  4. ↑ 4.0 4.1 4.2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics 355: L27–L30, Bibcode: 2000A&A...355L..27H. 
  5. ↑ 5.0 5.1 5.2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Van Hamme, W.; Samec, R. G.; Gothard, N. W.; Wilson, R. E.; Faulkner, D. R.; Branly, R. M. (2001). "CN Andromedae: A Broken-Contact Binary?". The Astronomical Journal 122 (6): 3436–3446. doi:10.1086/324110. Bibcode: 2001AJ....122.3436V. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 7.8 Siwak, M.; Zola, S.; Koziel-Wierzbowska, D. (2010). "A Study of Contact Binaries with Large Temperature Differences between Components". Acta Astronomica 60 (4): 305–336. Bibcode: 2010AcA....60..305S. 
  8. ↑ Yildirim, Muhammed (2019). "CN Andromedae: a shallow contact binary with a possible tertiary component". Research in Astronomy and Astrophysics 19 (1): 10-1 - 10-10. doi:10.1088/1674-4527/19/1/10. 



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