WW Aurigae is an eclipsing binary star system in the northern constellation of Auriga. It has a combined maximum apparent visual magnitude of 5.86,[5] which is bright enough to be dimly visible to the naked eye. Based upon an annual parallax shift of 11.0 mas,[2] it is located 297 light years from the Earth. The system is moving further away with a heliocentric radial velocity of −9 km/s, having come to within 212.5 ly some 3.12 million years ago.[3]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 06h 32m 27.18445s[2] |
Declination | +32° 27′ 17.6330″[2] |
Apparent magnitude (V) | 5.82[3] |
Characteristics | |
Spectral type | A4m + A5m[4] |
B−V color index | 0.188±0.007[3] |
Variable type | EA[5] |
Astrometry | |
Radial velocity (Rv) | −8.7±0.9[3] km/s |
Proper motion (μ) | RA: −26.347[2] mas/yr Dec.: −17.343[2] mas/yr |
Parallax (π) | 10.9979 ± 0.0829 mas[2] |
Distance | 297 ± 2 ly (90.9 ± 0.7 pc) |
Absolute magnitude (MV) | 1.29[3] |
Orbit[6] | |
Period (P) | 2.525 d |
Eccentricity (e) | 0.00 |
Periastron epoch (T) | 2,432,945.539±1.0 JD |
Argument of periastron (ω) (secondary) | 0.00° |
Semi-amplitude (K1) (primary) | 115.6 km/s |
Semi-amplitude (K2) (secondary) | 127.7 km/s |
Details[7] | |
WW Aur A | |
Mass | 1.964±0.007 M☉ |
Radius | 1.980±0.009 R☉ |
Luminosity | 13.5[8] L☉ |
Surface gravity (log g) | 4.160±0.007 cgs |
Temperature | 8,350±200 K |
Rotational velocity (v sin i) | 35±10 km/s |
Age | 565±15 Myr |
WW Aur b | |
Mass | 1.814±0.007 M☉ |
Radius | 1.807±0.009 R☉ |
Luminosity | 10.5[8] L☉ |
Surface gravity (log g) | 4.165±0.007 cgs |
Temperature | 8,170±300 K |
Rotational velocity (v sin i) | 55±10[7] km/s |
Other designations | |
Database references | |
SIMBAD | data |
This is a double-lined[4] spectroscopic binary system, having a circular orbit with a period of 2.5 days.[6] It was discovered to be variable independently by Friedrich Schwab and Heinrich Van Solowiew in 1913.[10] Both components are metallic-lined, or Am stars, with a spectrum showing a deficiency of calcium and scandium, and an overabundance of heavier elements.[11] Together they form an EA, or Algol-type, eclipsing binary with the primary occultation reducing the net magnitude to a minimum of 6.54 and the secondary eclipse lowering it to 6.43, over a cycle time of 2.52501936 days.[5]
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