WW Aurigae

WW Aurigae

A light curve for WW Aurigae, plotted from Hiparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 06h 32m 27.18477s[2]
Declination +32° 27′ 17.6324″[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: −26.3507[2] mas/yr
Dec.: −17.343[2] mas/yr
Parallax (π)11.1431 ± 0.0691 mas[2]
Distance293 ± 2 ly
(89.7 ± 0.6 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
Mass1.964±0.007 M☉
Radius1.980±0.009 R☉
Luminosity13.5[8] L☉
Surface gravity (log g)4.160±0.007 cgs
Temperature8,350±200 K
Rotational velocity (v sin i)35±10 km/s
Age565±15 Myr
WW Aur B
Mass1.814±0.007 M☉
Radius1.807±0.009 R☉
Luminosity10.5[8] L☉
Surface gravity (log g)4.165±0.007 cgs
Temperature8,170±300 K
Rotational velocity (v sin i)55±10[7] km/s
Other designations
WW Aur, BD+32°1324, FK5 2500, HD 46052, HIP 31173, HR 2372, SAO 59194[9]
Database references
SIMBADdata

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 11.1 mas,[2] it is located 293 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]

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]

  1. ^ Cite error: The named reference HipDataAccess was invoked but never defined (see the help page).
  2. ^ a b c d e f Cite error: The named reference dr3 was invoked but never defined (see the help page).
  3. ^ a b c d e Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference SreedharRao1991 was invoked but never defined (see the help page).
  5. ^ a b c Cite error: The named reference gcvs was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference Kitamura1976 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Southworth2004 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference Southworth2015 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Dugan1930 was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference Pavlovski2008 was invoked but never defined (see the help page).