Epoch 2000 Equinox 2000
|Right ascension||00h 43m 28.39827s|
|Declination||+64° 45′ 35.4011″|
|Apparent magnitude (V)||10.69|
|U−B color index||−0.86|
|B−V color index||+0.02|
|Radial velocity (Rv)||100.00 km/s|
|Proper motion (μ)|| RA: −4.061±0.063 mas/yr |
Dec.: −1.422±0.072 mas/yr
|Parallax (π)||0.3131 ± 0.0412 mas|
|Distance||approx. 10,000 ly |
(approx. 3,200 pc)
|Absolute magnitude (MV)||−3.13|
WR 3 is a member of the nitrogen sequence of WR stars and has a spectrum with strong HeII and NV lines, but weak NIV. HeI lines are very weak or missing, but there are lines of OVI. Unusually, there are lines of hydrogen and absorption components in many lines creating P Cygni profiles. Overall, the emission is weaker than stars of similar spectral type, and it has often been suggested that WR 3 has a type O binary companion. However, there are no other signs of a companion and it is thought to be a single star with a spectral type of WN3-hw. The "h" and "w" indicate that hydrogen is present and the emission is weaker for the class.
WR 3 is a massive and luminous star. The presence of hydrogen in its spectrum suggests that it is younger than hydrogen-free WR stars and may still be fusing hydrogen in its core. The emission lines of heavy elements in its spectrum are produced by strong convection and powerful stellar winds rather than complete loss of the outer layers of the star. The wind has been measured at 2,700 km/s leading to mass being lost at four millionths M☉ per year.
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