V766 Centauri is a white to yellow eruptive supergiant star that can be located in the constellation of Centaurus. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it.
In the Hipparcos catalogue of 1997, the star is recorded as A7p in the data download file whereas everywhere else says it is G8. The source of information about stars on this site is the Hipparcos data file and the Hipparcos Double Star file. The latter file has the matching Spectral Type. It is also said that this star is the largest yellow supergiant so far discovered.
The star is a double star where the second star is smaller and feeds into the larger. To get an idea of what I mean, watch the Nemesis Maturity video to explain it better. It is better known by its HR id rather than by its V, Hip or HD Id.
The Id of the star in the Yale Bright Star Catalogue is HR5171. HIP67261 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD119796.
V766 Centauri has alternative name(s) :- HR 5171 , V766 Cen.
The Gould star designation is one that was designed by American astronomer, Benjamin Apthorp Gould. Gould stars are predominantly in the Southern and Equatorial constellations but do appear in northern constellations such as Bootes and Orion. The star has the designation 264 G. Centauri. There are no stars with a Gould designation in Ursa Major for example.
More details on star alternative names can be found at Star Names.
The location of the star in the galaxy 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 V766 Centauri, the location is 13h 47m 10.87 and -62° 35` 22.9 .
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 -2.54 ± 0.92 miliarcseconds/year towards the north and -2.94 ± 1.59 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 -38.20000 km/s with an error of about 0.60 km/s .
V766 Centauri has a spectral type of G8Ia++B0Ibp. This means the star is a white to yellow supergiant star. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
V766 Centauri has an apparent magnitude of 6.40 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 -6.36 If you used the 2007 Parallax value, you would get an absolute magnitude of -2.95. 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 0.28 which gave the calculated distance to V766 Centauri as 11648.69 light years away from Earth or 3571.43 parsecs. It would take a spaceship travelling at the speed of light, 11648.69 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 1.35 which put V766 Centauri at a distance of 2416.02 light years or 740.74 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 eruptive S Doradus. S Doradus is a star in the Large Magellanic Cloud, not the Milky Way 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. V766 Centauri brightness ranges from a magnitude of 6.810 to a magnitude of 6.550 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.3 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||HR 5171, HD 119796, HIP 67261, HR 5171, 264 G. Centauri, V766 Cen|
|Star Type||very luminous Supergiant Star|
|Absolute Magnitude||-6.36 / -2.95|
|Visual / Apparent Magnitude||6.40|
|Naked Eye Visible||Yes - Magnitudes|
|Right Ascension (R.A.)||13h 47m 10.87|
|Declination (Dec.)||-62° 35` 22.9|
|Galactic Latitude||-0.41 degrees|
|Galactic Longitude||309.30 degrees|
|1997 Distance from Earth||0.28 Parallax (milliarcseconds)|
|11648.69 Light Years|
|2007 Revised Distance from Earth||1.35 Parallax (milliarcseconds)|
|2416.02 Light Years|
|Proper Motion Dec.||-2.54 ± 0.92 milliarcseconds/year|
|Proper Motion RA.||-2.94 ± 1.59 milliarcseconds/year|
|Radial Velocity||-38.20 ± 0.60 km/s|
|Colour||(G) White to Yellow|
|Variable Star Class||Eruptive|
|Variable Star Type||S Doradus. S Doradus is a star in the Large Magellanic Cloud, not the Milky Way|
|Mean Variability Period in Days||0.265|
|Variable Magnitude Range (Brighter - Dimmer)||6.550 - 6.810|
The star has been identified as being a multi-star system, one in which there is at least one star in close orbit to another star or two or more stars orbiting a central point. The stars may be of equal mass, unequal mass where one star is stronger than the other or be in groups orbiting a central point which doesn't necessarily have to be a star. More information can be found on my dedicated multiple star systems page. The source of the info is Simbad. The file is dated 2000 so any differences between this and any other source will be down to the actual source from where the information came from.
|Proper Motion mas/yr|
|H.D. Id||B.D. Id||Star Code||Magnitude||R.A.||Dec.||Spectrum||Colour||Year|