Astronomy:V348 Andromedae
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Short description: Variable star system in constellation Andromeda
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 15m 17.84s[1] |
| Declination | +44° 12′ 12.2″[1] |
| Apparent magnitude (V) | 6.77±0.01[2] |
| Characteristics | |
| Evolutionary stage | Main-sequence |
| Spectral type | B9V + B9V + B8V[3] |
| Variable type | Algol[4][5] |
| Astrometry | |
| Radial velocity (Rv) | −11.63±0.52 km/s |
| Proper motion (μ) | RA: 5.461[6] mas/yr Dec.: -3.053[6] mas/yr |
| Parallax (π) | 2.92[3] mas |
| Distance | 1,117 ly (342 pc) |
| Orbit[3] | |
| Primary | A |
| Companion | B |
| Period (P) | 27.703514±0.000325 days |
| Semi-major axis (a) | 68.28±0.87 R☉ |
| Eccentricity (e) | 0.116±0.012 |
| Inclination (i) | 88.26±0.02° |
| Periastron epoch (T) | 2,455,923.129±0.025 HJD |
| Argument of periastron (ω) (secondary) | 95.6±0.2° |
| Semi-amplitude (K1) (primary) | 61.22±0.81 km/s |
| Semi-amplitude (K2) (secondary) | 63.76±0.85 km/s |
| Orbit[3] | |
| Primary | AB |
| Companion | C |
| Period (P) | 86.9±4.3 yr |
| Semi-major axis (a) | 0.118±0.013″ |
| Eccentricity (e) | 0.559±0.015 |
| Inclination (i) | 66.0±3.9° |
| Longitude of the node (Ω) | 61.1±2.4° |
| Periastron epoch (T) | 2,451,501±96 HJD |
| Argument of periastron (ω) (secondary) | 140±10° |
| Details[3] | |
| A | |
| Mass | 2.81±0.04 M☉ |
| Radius | 2.42±0.03 R☉ |
| Temperature | 10,500 K |
| B | |
| Mass | 2.69±0.04 M☉ |
| Radius | 2.34±0.03 R☉ |
| Temperature | 10,412±87 K |
| C | |
| Mass | 3.4 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
V348 Andromedae is a multiple star system located approximately 1,100 light-years from Earth in the constellation of Andromeda. Its combined apparent visual magnitude of around 6.77 makes it visible to the naked eye under good conditions.[2][3]
Characteristics
The primary pair consists of an Algol type[4][5] eclipsing binary system of two B-type main-sequence stars both having a spectral type of B9V both having mass of 2.81 M☉ and 2.69 M☉ and has an orbital period of approximately 27.7 days.[3] This inner pair of binary is accompanied by a tertiary companion of spectral type B8V with a mass of 3.4 M☉ in a wide orbit with an orbital period of about 87 years, making the system a hierarchical triple star system.[3]
References
- ↑ 1.0 1.1 1.2 "V348 Andromedae". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V348+Andromedae.
- ↑ 2.0 2.1 Fabricius, C.; Høg, E.; Makarov, V. V.; Mason, B. D.; Wycoff, G. L.; Urban, S. E. (March 2002). "The Tycho double star catalogue". Astronomy & Astrophysics 384 (1): 180–189. doi:10.1051/0004-6361:20011822. Bibcode: 2002A&A...384..180F.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Zasche, P.; Uhlař, R.; Svoboda, P.; Juryšek, J.; Korčáková, D.; Wolf, M.; Šlechta, M.; Kotková, L. (2019-08-01). "V348 And and V572 Per: Bright Triple Systems with Eccentric Eclipsing Binaries". The Astronomical Journal 158 (2): 95. doi:10.3847/1538-3881/ab2d22. Bibcode: 2019AJ....158...95Z.
- ↑ 4.0 4.1 Zasche, P.; Svoboda, P. (2008). "The Unconfirmed Eclipsing Nature of V348 And and Detection of Variability of HD 1438" (in en). Information Bulletin on Variable Stars 5827: 1. Bibcode: 2008IBVS.5827....1Z.
- ↑ 5.0 5.1 Zasche, P.; Wolf, M.; Hartkopf, W. I.; Svoboda, P.; Uhlař, R.; Liakos, A.; Gazeas, K. (2009-08-01). "A Catalog of Visual Double and Multiple Stars with Eclipsing Components". The Astronomical Journal 138 (2): 664–679. doi:10.1088/0004-6256/138/2/664. Bibcode: 2009AJ....138..664Z.
- ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
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