WR 22 is a eclipsing binary system Wolf-Rayet star that can be located in the constellation of Carina. The description is based on the spectral class. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it.
HIP52308 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD92740.
WR 22 has alternative name(s) :- , V429 Car.
More details on star alternative names can be found at Star Names .
The location of the star in the night sky is determined by the Right Ascension (R.A.) and Declination (Dec.), these are equivalent to the Longitude and Latitude on the Earth. The Right Ascension is how far expressed in time (hh:mm:ss) the star is along the celestial equator. If the R.A. is positive then its eastwards. The Declination is how far north or south the star is compared to the celestial equator and is expressed in degrees. For WR 22, the location is 10h 41m 17.52 and -59° 40` 36.9 .
The star is a Wolf-Rayet, a rare type of star of which not many are known. These stars are extremely luminous and large compared to our Sun. They live fast and die hard in a matter of millions not billions of years like our Sun. They exhaust their hydrogen supplies, turning to other gasses and expand outwards with massive solar winds, moving a step closer in the stellar evolution towards their death in a super or hypernova explosion.
All stars like planets orbit round a central spot, in the case of planets, its the central star such as the Sun. In the case of a star, its the galactic centre. The constellations that we see today will be different than they were 50,000 years ago or 50,000 years from now. Proper Motion details the movements of these stars and are measured in milliarcseconds. The star is moving 2.86 ± 0.28 miliarcseconds/year towards the north and -7.71 ± 0.34 miliarcseconds/year east if we saw them in the horizon. The Radial Velocity, that is the speed at which the star is moving away/towards us is -28.00000 km/s with an error of about 7.40 km/s .
WR 22 has a spectral type of WN7 + A(SB1). The star has a B-V Colour Index of 0.08 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 8,721 Kelvin.
WR 22 Radius has been calculated as being 35.96 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 25,020,823.31.km. If you need the diameter of the star, you just need to multiple the radius by 2. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 274.07. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
WR 22 has an apparent magnitude of 6.35 which is how bright we see the star from Earth. Apparent Magnitude is also known as Visual Magnitude. If you used the 1997 Parallax value, you would get an absolute magnitude of -4.72 If you used the 2007 Parallax value, you would get an absolute magnitude of -9.13. Magnitude, whether it be apparent/visual or absolute magnitude is measured by a number, the smaller the number, the brighter the Star is. Our own Sun is the brightest star and therefore has the lowest of all magnitudes, -26.74. A faint star will have a high number.
Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 0.61 which gave the calculated distance to WR 22 as 5346.94 light years away from Earth or 1639.34 parsecs. It would take a spaceship travelling at the speed of light, 5346.94 years to get there. We don't have the technology or spaceship that can carry people over that distance yet.
In 2007, Hipparcos data was revised with a new parallax of 0.08 which put WR 22 at a distance of 40770.42 light years or 12500 parsecs. It should not be taken as though the star is moving closer or further away from us. It is purely that the distance was recalculated.
The star is a eclipsing binary system Beta Persei (Algol) variable type which means that its size changes over time. The Variable Type is usually named after the first star of that type to be spotted. WR 22 brightness ranges from a magnitude of 6.407 to a magnitude of 6.364 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.0 days (variability).
The source of the information if it has a Hip I.D. is from Simbad, the Hipparcos data library based at the University at Strasbourg, France. Hipparcos was a E.S.A. satellite operation launched in 1989 for four years. The items in red are values that I've calculated so they could well be wrong. Information regarding Metallicity and/or Mass is from the E.U. Exoplanets. The information was obtained as of 12th Feb 2017.
|Alternative Names||HD 92740, HIP 52308, V429 Car, WR 22|
|Spectral Type||WN7 + A(SB1)|
|Multiple Star System||No / Unknown|
|Star Type||Wolf-Rayet star|
|Absolute Magnitude||-4.72 / -9.13|
|Visual / Apparent Magnitude||6.35|
|Naked Eye Visible||Yes - Magnitudes|
|Right Ascension (R.A.)||10h 41m 17.52|
|Declination (Dec.)||-59° 40` 36.9|
|Galactic Latitude||-0.85 degrees|
|Galactic Longitude||287.17 degrees|
|1997 Distance from Earth||0.61 Parallax (milliarcseconds)|
|5346.94 Light Years|
|2007 Distance from Earth||0.08 Parallax (milliarcseconds)|
|40770.42 Light Years|
|Proper Motion Dec.||2.86 ± 0.28 milliarcseconds/year|
|Proper Motion RA.||-7.71 ± 0.34 milliarcseconds/year|
|Radial Velocity||-28.00 ± 7.40 km/s|
|Variable Star Class||Eclipsing binary system|
|Variable Star Type||Beta Persei (Algol)|
|Mean Variability Period in Days||0.031|
|Variable Magnitude Range (Brighter - Dimmer)||6.364 - 6.407|
|Calculated Effective Temperature||8,721 Kelvin|