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Star in the constellation Andromeda From Wikipedia, the free encyclopedia
KZ Andromedae (often abbreviated to KZ And) is a double lined spectroscopic binary in the constellation Andromeda. Its apparent visual magnitude varies between 7.91 and 8.03 during a cycle slightly longer than 3 days.
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Andromeda |
Right ascension | 23h 09m 57.3642s[2] |
Declination | +35° 32′ 55.65804″[2] |
Apparent magnitude (V) | 7.91 – 8.03 variable[3] |
Characteristics | |
Spectral type | K2Ve+K2Ve[3] |
Apparent magnitude (B) | 8.81[4] |
Apparent magnitude (V) | 7.93[4] |
Apparent magnitude (G) | 7.6580[2] |
Apparent magnitude (J) | 6.225[5] |
Apparent magnitude (H) | 5.778[5] |
Apparent magnitude (K) | 5.659[5] |
Variable type | BY Dra[3] |
Astrometry | |
Radial velocity (Rv) | −5.818±0.026[6] km/s |
Proper motion (μ) | RA: 150.123±0.063 [2] mas/yr Dec.: 1.226±0.059[2] mas/yr |
Parallax (π) | 32.8449 ± 0.0369 mas[2] |
Distance | 99.3 ± 0.1 ly (30.45 ± 0.03 pc) |
Orbit[6] | |
Period (P) | 3.03291126±0.00000046 days |
Eccentricity (e) | 0.01174±0.00056 |
Periastron epoch (T) | HJD 2455133.480±0.020 |
Argument of periastron (ω) (secondary) | 7.11±2.35° |
Semi-amplitude (K1) (primary) | 69.362±0.046 km/s |
Semi-amplitude (K2) (secondary) | 71.300±0.054 km/s |
Details[6] | |
Primary | |
Radius | 0.77±0.07 R☉ |
Luminosity | 0.34±0.06 L☉ |
Rotational velocity (v sin i) | 12.5 km/s |
Secondary | |
Radius | 0.66±0.06 R☉ |
Luminosity | 0.25±0.04 L☉ |
Rotational velocity (v sin i) | 12.2 km/s |
Other designations | |
Database references | |
SIMBAD | data |
Both stars in the KZ Andromedae system are main sequence stars of spectral type K2Ve, meaning that the spectrum shows strong emission lines.[3] This is caused by their active chromospheres that cause large spots on the surface.[6]
KZ Andromedae is listed in the Washington Double Star Catalog as the secondary component in a visual binary system, with the primary being HD 218739. In 50 years of observations, there is little evidence of relative motion between the two stars; however, they have a common proper motion and a similar radial velocity.[6]
The rotational velocity of both stars is consistent with a synchronous rotation of the pair, and the rotational period is itself comparable to the brightness variation period. KX Andromedae is thus classified as a BY Draconis variable, and the variability is caused by the large spots on the surface.[6]
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