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V Pavonis, HD160435, HIP86728

V Pavonis is a pulsating luminous giant star that can be located in the constellation of Pavo. V Pavonis is the brightest star in Pavo based on the Hipparcos 2007 apparent magnitude. 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.

Location of V Pavonis

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 -57d 43` 26.2 .

Proper Motion of V Pavonis

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.

Physical Properties (Temperature, Radius) of V Pavonis

V Pavonis has a spectral type of C5II. This means the star is a 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 Apparent and Absolute Magnitudes

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.

Distance to V Pavonis

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*.

Variable Type of V Pavonis

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).

Source of Information

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.

V Pavonis Facts

Alternative Names

Traditional/Proper NameV Pavonis
Short NameV Pav
Hipparcos Library I.D.86728
Henry Draper Designation160435

Visual Facts

Star Typeluminous giant star
Absolute Magnitude-0.54 / -0.99
Visual / Apparent Magnitude6.85
Naked Eye VisibleRequires a 7x50 Binoculars - Magnitudes
Right Ascension (R.A.)17h 43m 18.94
Declination (Dec.)-57d 43` 26.2
Galactic Latitude-14.26 degrees
Galactic Longitude334.72 degrees
1997 Distance from Earth3.32 Parallax (milliarcseconds)
 982.42 Light Years
 301.20 Parsecs
2007 Revised Distance from Earth2.70 Parallax (milliarcseconds)
 1208.01 Light Years
 370.37 Parsecs
Galacto-Centric Distance23,131.50 Light Years / 7,092.00 Parsecs
Proper Motion Dec.-5.96 ± 0.35 milliarcseconds/year
Proper Motion RA.-3.43 ± 0.53 milliarcseconds/year
B-V Index2.45
Radial Velocity15.60 ± 2.40 km/s
Spectral TypeC5II

Variable Star Details

Variable Star ClassPulsating
Variable Star TypeSemiregular late- (M, C, S or Me, Ce, Se) giants with poorly defined periodicity
Mean Variability Period in Days0.413
Variable Magnitude Range (Brighter - Dimmer)6.468 - 6.872

Estimated Facts

Calculated Effective Temperature41 Kelvin

Sources and Links

SIMBAD SourceLink

Related Stars

Multi-Star System

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. IdB.D. IdStar CodeMagnitudeR.A.Dec.SpectrumColourYear
160435-57 8687.4A-2.00000-49.00000NB

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