| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Crux |
| Right ascension | 12h 11m 59.16182s[2] |
| Declination | −58° 47′ 00.7374″[2] |
| Apparent magnitude (V) | 8.18(-8.50)-9.01[3] |
| Characteristics | |
| Spectral type | F8/G1Ia/abe[4](B + G1Iab)[5] |
| Variable type | Algol[6] |
| Astrometry | |
| Radial velocity (Rv) | −22.6±2[7] km/s |
| Proper motion (μ) | RA: −6.142[2]mas/yr Dec.: 0.198[2]mas/yr |
| Parallax (π) | 0.5363±0.0421 mas[2] |
| Distance | 6,100 ± 500 ly (1,900 ± 100 pc) |
| Orbit[5] | |
| Period (P) | 198.5 days |
| Semi-major axis (a) | 306 R☉ |
| Inclination (i) | 88.2° |
| Details | |
| Luminosity | 1,928[2] L☉ |
| A | |
| Mass | 8.2[5] M☉ |
| Radius | 71[5] R☉ |
| Temperature | 14,000[8] K |
| B | |
| Mass | 1.6[5] M☉ |
| Radius | 4[5][8] R☉ |
| Temperature | 5,500[8] K |
| Other designations | |
| CD−58 4431,CPD−58 4151,HD 105998,HIP 59483[9] | |
| Database references | |
| SIMBAD | data |
W Crucis is a single-linedeclipsing variable star system in theconstellationCrux. It has a spectral class of F8/G1Ia/abe indicating ayellow supergiant withemission lines in its spectrum.
W Crucis varies in brightness betweenmagnitude 8.18 and 9.01 over a period of 198.5 days. Itslight curve has been observed to be asymmetric with subsequent maxima differing in height, which is described as the so-calledO'Connell effect.[10] A secondary minimum is observed when the brightness drops to magnitude 8.5. The shape and duration of the eclipses show that the two stars aredetached and that there is an accretion disk around the primary, more massive, star.[5]
Spectral lines can only be seen for one of the stars, a yellow supergiant. The other, more massive, star is hidden within an accretion disk of material stripped from the supergiant. The hidden star has properties that suggest it is a mid-Bmain sequence star. The two are separated by 306 R☉, about1.4 AU. The hot main sequence star has a mass of 8.2 M☉, while thesupergiant only has a mass of 1.6 M☉. The supergiant is deformed by the gravity of the more massive primary star, fills itsRoche lobe, and is losing mass.[5]
The disk around the hot star is 124 R☉ wide and 17 R☉ thick, with a temperature at its outer visible edge of3600 K. It is the source of the emission lines seen in the spectrum.[5]
