astro.wikisort.org - StarCN 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]
Star in the constellation Andromeda
CN Andromedae
 The visual band light curve of CN Andromedae, adapted from a plot presented by Varol Keskin [1] |
Observation data Epoch J2000 Equinox J2000 |
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 |
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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 mas[2] |
Distance | 657 ± 6 ly (201 ± 2 pc) |
|
Orbit[6] |
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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 |
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Primary |
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Mass | 1.433±0.030[7] M☉ |
Radius | 1.48±0.03[7] R☉ |
Luminosity | 3.40[7] L☉ |
Surface gravity (log g) | 4.24[6] cgs |
Temperature | 6,450[7] K |
Secondary |
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Mass | 0.552±0.020[7] M☉ |
Radius | 0.95[7] R☉ |
Luminosity | 0.40[7] L☉ |
Surface gravity (log g) | 4.22[6] cgs |
Temperature | 4,726[7] K |
Other designations |
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2MASS J00203054+4013337, BD+39 59, TYC 2787-1815-1 |
Database references |
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SIMBAD | data |
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 obit 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
- 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. Retrieved 7 October 2021.
- 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. Gaia DR2 record for this source at VizieR.
- 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.
- Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
- Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (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.
- 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. Bibcode:2001AJ....122.3436V. doi:10.1086/324110.
- 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. arXiv:1011.5682. Bibcode:2010AcA....60..305S.
- 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.
Constellation of Andromeda |
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На других языках
- [en] CN Andromedae
[ru] CN Андромеды
CN Андромеды (лат. CN Andromedae) — двойная затменная переменная звезда типа Беты Лиры в созвездии Андромеды на расстоянии приблизительно 655 световых лет (около 201 парсека) от Солнца. Видимая звёздная величина звезды — от +10,21m до +9,62m[6]. Орбитальный период — около 0,4628 суток (11,107 часов). Возраст звезды определён как около 2,96 млрд лет[7].
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