Summary
BX Andromedae (BX And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 8.87. Within a cycle of approximately 14.6 hours, the brightness drops down to a magnitude of 9.53 during the main eclipse, and to a magnitude of 9.12 during the secondary one. It is classified as a Beta Lyrae variable.[3]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 02h 09m 03.4213s[2] |
| Declination | +40° 47′ 39.167″[2] |
| Apparent magnitude (V) | 8.87 – 9.53 variable [3] |
| Characteristics | |
| Spectral type | F2V[3] |
| Apparent magnitude (B) | 9.37[4] |
| Apparent magnitude (V) | 8.98[4] |
| Apparent magnitude (G) | 8.873359[2] |
| Apparent magnitude (J) | 8.487[5] |
| Apparent magnitude (H) | 8.229[5] |
| Apparent magnitude (K) | 8.134[5] |
| B−V color index | 0.3927[6] |
| Variable type | EB[3] |
| Astrometry | |
| Radial velocity (Rv) | −45.10±2.6[7] km/s |
| Proper motion (μ) | RA: 9.846(23) mas/yr[2] Dec.: −8.425(24) mas/yr[2] |
| Parallax (π) | 5.5643 ± 0.0216 mas[2] |
| Distance | 586 ± 2 ly (179.7 ± 0.7 pc) |
| Orbit[8] | |
| Period (P) | 0.61011240 days |
| Semi-major axis (a) | 4.424 R☉ |
| Inclination (i) | 75.862° |
| Semi-amplitude (K1) (primary) | 106.35±0.61 km/s |
| Semi-amplitude (K2) (secondary) | 233.58±1.77 km/s |
| Details[8] | |
| Primary | |
| Mass | 2.148 M☉ |
| Radius | 2.01 R☉ |
| Luminosity | 7.08 L☉ |
| Temperature | 6,650 K |
| Secondary | |
| Mass | 0.977 M☉ |
| Radius | 1.40 R☉ |
| Luminosity | 0.90 L☉ |
| Temperature | 4,758 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Variability edit
The variability of BX Andromedae was reported first by A. Soloviev, in 1945. He believed it to be an eclipsing binary, but was unable to deduce its period. The star's period was first measured in 1951, by Joseph Ashbrook.[9]
BX Andromedae, like all Beta Lyrae variables, shows a primary and a secondary minimum when, respectively, the most luminous and the less luminous component of the pair is eclipsed by the other. The brightness however changes smoothly, so there is no onset and an end time for the eclipses. This cycle repeats approximately every 14.6 hours.[3]
System edit
The two stars in the system are orbiting so close to each other that they retain an ellipsoidal shape. The spectrum of the two stars has not been separated yet; as a whole, the system has a spectral type F2V.[3] The physical parameters of the stars (like mass, radius, and temperature) can be inferred from the light curve.
BX Andromedae, however, may be a quadruple system. This system shows slight orbital period variations that could be induced by a third faint body in the system with an orbital period of 62 years.[10] There is also a visual companion star TYC 2833-53-1 of 10.85 magnitude only 20 arcseconds away with a common proper motion and a distance (measured with parallax) compatible with the one of BX Andromedae, and has an estimated mass of 1.04 M☉.[11]
References edit
- ^ Samec, R. G.; Fuller, R. E.; Kaitchuck, R. H. (August 1988). "1976 Light Curves of BX Andromedae". Information Bulletin on Variable Stars. 3230: 1. Bibcode:1988IBVS.3230....1S. Retrieved 7 October 2021.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f BX 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.
- ^ a b "BX And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 26, 2018.
- ^ a b c 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.
- ^ 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.
- ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 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.
- ^ a b 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.
- ^ Ashbrook, J. (April 1951). "The eclipsing variable SVS 995 Andromedae". Astronomical Journal. 56: 54–55. Bibcode:1951AJ.....56...54A. doi:10.1086/106509. Retrieved 31 March 2023.
- ^ Pribulla, T.; Rucinski, S. M. (2006). "Contact Binaries with Additional Components. I. The Extant Data". The Astronomical Journal. 131 (6): 2986–3007. arXiv:astro-ph/0601610. Bibcode:2006AJ....131.2986P. doi:10.1086/503871. S2CID 15762240.
- ^ Database entry, Updated Multiple Star Catalog (MSC, 2018), A. Tokovinin CDS ID J/ApJS/235/6 Accessed on line 2018-10-29.