V472 Persei is a blue pulsating supergiant star that can be located in the constellation of Perseus. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it.
HIP9990 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD12953.
V472 Persei has alternative name(s) :- , V472 Per.
BD number is the number that the star was filed under in the Durchmusterung or Bonner Durchmusterung, a star catalogue that was put together by the Bonn Observatory between 1859 to 1903. The star's BD Number is BD+57 494.
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 V472 Persei, the location is 02h 08m 40.58 and +58° 25` 25.0 .
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 -1.65 ± 0.25 miliarcseconds/year towards the north and -1.37 ± 0.39 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 -35.50000 km/s with an error of about 1.00 km/s .
V472 Persei has a spectral type of A1Ia. This means the star is a blue supergiant star. The star has a B-V Colour Index of 0.59 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 5,898 Kelvin.
V472 Persei Radius has been calculated as being 36.94 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 25,704,462.79.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 68.79. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures. The star's Iron Abundance is 0.37 with an error value of 9.99 Fe/H with the Sun has a value of 1 to put it into context.
V472 Persei has an apparent magnitude of 5.66 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 -3.08 If you used the 2007 Parallax value, you would get an absolute magnitude of -4.43. 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 1.79 which gave the calculated distance to V472 Persei as 1822.14 light years away from Earth or 558.66 parsecs. It would take a spaceship travelling at the speed of light, 1822.14 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 0.96 which put V472 Persei at a distance of 3397.53 light years or 1041.67 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 pulsating Alpha Cygnus 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. V472 Persei brightness ranges from a magnitude of 5.831 to a magnitude of 5.793 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 6.4 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 12953, HIP 9990, BD+57 494, V472 Per|
|Star Type||very luminous Supergiant Star|
|Absolute Magnitude||-3.08 / -4.43|
|Visual / Apparent Magnitude||5.66|
|Naked Eye Visible||Yes - Magnitudes|
|Right Ascension (R.A.)||02h 08m 40.58|
|Declination (Dec.)||+58° 25` 25.0|
|Galactic Latitude||-2.94 degrees|
|Galactic Longitude||132.92 degrees|
|1997 Distance from Earth||1.79 Parallax (milliarcseconds)|
|1822.14 Light Years|
|2007 Revised Distance from Earth||0.96 Parallax (milliarcseconds)|
|3397.53 Light Years|
|Proper Motion Dec.||-1.65 ± 0.25 milliarcseconds/year|
|Proper Motion RA.||-1.37 ± 0.39 milliarcseconds/year|
|Radial Velocity||-35.50 ± 1.00 km/s|
|Iron Abundance||0.37 ± 9.99 Fe/H|
|Variable Star Class||Pulsating|
|Variable Star Type||Alpha Cygnus|
|Mean Variability Period in Days||6.361|
|Variable Magnitude Range (Brighter - Dimmer)||5.793 - 5.831|
|Calculated Effective Temperature||5,898 Kelvin|