QS Aquilae
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File:QSAqlLightCurve.png A visual band light curve for QS Aquilae. Adapted from Zasche et al. (2017)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[2] |
| Apparent magnitude (V) | 5.988 |
| Characteristics | |
| Spectral type | B5V |
| U−B Template:Engvar | −0.52 |
| B−V Template:Engvar | −0.08 |
| Variable type | Eclipsing binary[3] |
| Astrometry | |
| Radial velocity (Rv) | −14.2 ± 2 km/s |
| Proper motion (μ) | RA: −0.04 ± 0.60[2] mas/yr Dec.: −11.47 ± 0.43[2] mas/yr |
| Parallax (π) | 0.49±0.62 mas[2] |
| Orbit[3] | |
| Primary | QS Aquilae AB (eclipsing pair) |
| Companion | QS Aquilae C |
| Period (P) | Script error: No such module "val". yr |
| Semi-major axis (a) | Script error: No such module "val".″ |
| Eccentricity (e) | Script error: No such module "val". |
| Inclination (i) | Script error: No such module "val".° |
| Longitude of the node (Ω) | Script error: No such module "val".° |
| Periastron epoch (T) | Script error: No such module "val". |
| Argument of periastron (ω) (secondary) | Script error: No such module "val".° |
| Orbit[3] | |
| Primary | QS Aquilae A |
| Companion | QS Aquilae B |
| Period (P) | Script error: No such module "val". |
| Semi-major axis (a) | Script error: No such module "val". |
| Inclination (i) | Script error: No such module "val".° |
| Semi-amplitude (K1) (primary) | Script error: No such module "val". km/s |
| Semi-amplitude (K2) (secondary) | Script error: No such module "val". km/s |
| Other designations | |
| Template:Odlist[4] | |
| Database references | |
| SIMBAD | data |
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QS Aquilae is a triple or quadruple star system consisting of an eclipsing binary in a 2.5 day orbit around which a third star orbits in 77 years.[3] There is some indication that there is a fourth component with a period of roughly 18 years.[5] Located in the constellation Aquila, its visual magnitude varies from 5.93 to 6.06, making it barely visible to the naked eye.[6]
The star's variability was discovered photometrically by Paul Guthnick and Richard Prager in 1930. It was given its variable star designation in 1934.[7]
References
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