V Pavonis is a carbon red pulsating luminous giant star that can be located in the constellation of Pavo. The star can not be seen by the naked eye, you need a telescope to see it.
HIP86728 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD160435.
V Pavonis has alternative name(s) :- , V Pav.
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 V Pavonis, the location is 17h 43m 18.94 and -57° 43` 26.2 .
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 -5.96 ± 0.35 miliarcseconds/year towards the north and -3.43 ± 0.53 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 15.60000 km/s with an error of about 2.40 km/s .
V Pavonis has a spectral type of C5II. This means the star is a carbon red luminous giant star. The star is 7092.00000000 Parsecs from the Galactic Centre or terms of Light Years is 23131.5043564800000000s. The star has a B-V Colour Index of 2.45 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 41 Kelvin.
V Pavonis Radius has been calculated as being 237,323.64 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 165,129,786,065.32.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 291974.83. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
V Pavonis has an apparent magnitude of 6.85 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 -0.54 If you used the 2007 Parallax value, you would get an absolute magnitude of -0.99. 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 3.32 which gave the calculated distance to V Pavonis as 982.42 light years away from Earth or 301.20 parsecs. It would take a spaceship travelling at the speed of light, 982.42 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 2.70 which put V Pavonis at a distance of 1208.01 light years or 370.37 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's Galacto-Centric Distance is 7,092.00 Parsecs or 23,131.50 Light Years. The Galacto-Centric Distance is the distance from the star to the Centre of the Galaxy which is Sagittarius A*.
The star is a pulsating Semiregular late- (M, C, S or Me, Ce, Se) giants with poorly defined periodicity 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. V Pavonis brightness ranges from a magnitude of 6.872 to a magnitude of 6.468 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.4 days (variability).
|Alternative Names||HD 160435, HIP 86728, V Pav|
|Multiple Star system||Yes|
|Star Type||Luminous Giant Star|
|Absolute Magnitude||-0.54 / -0.99|
|Visual / Apparent Magnitude||6.85|
|Naked Eye Visible||Requires a 7x50 Binoculars - Magnitudes|
|Right Ascension (R.A.)||17h 43m 18.94|
|Declination (Dec.)||-57° 43` 26.2|
|Galactic Latitude||-14.26 degrees|
|Galactic Longitude||334.72 degrees|
|1997 Distance from Earth||3.32 Parallax (milliarcseconds)|
|982.42 Light Years|
|2007 Distance from Earth||2.70 Parallax (milliarcseconds)|
|1208.01 Light Years|
|Galacto-Centric Distance||23,131.50 Light Years / 7,092.00 Parsecs|
|Proper Motion Dec.||-5.96 ± 0.35 milliarcseconds/year|
|Proper Motion RA.||-3.43 ± 0.53 milliarcseconds/year|
|Radial Velocity||15.60 ± 2.40 km/s|
|Variable Star Class||Pulsating|
|Variable Star Type||Semiregular late- (M, C, S or Me, Ce, Se) giants with poorly defined periodicity|
|Mean Variability Period in Days||0.413|
|Variable Magnitude Range (Brighter - Dimmer)||6.468 - 6.872|
|Calculated Effective Temperature||41 Kelvin|
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|