HIP10805 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD14134.
V520 Persei has alternative name(s) :- , V520 Per.
Flamsteed designations are named after the creator, Sir John Flamsteed. Sir John numbered the stars in the constellation with a number and the latin name, this star's Flamsteed designation is 61 Persei with it shortened to 61 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+56 522.
More details on objects' alternative names can be found at Star Names .
The location of the supergiant 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 object is compared to the celestial equator and is expressed in degrees. For V520 Persei, the location is 02h 19m 04.45 and +57° 08` 07.8 .
V520 Persei has a spectral type of B3Ia. This means the star is a blue supergiant star. The star has a B-V Colour Index of 0.46 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 6,220 Kelvin.
V520 Persei has an apparent magnitude of 6.57 which is how bright we see the star from Earth. Apparent Magnitude is also known as Visual Magnitude. Using the supplied Parallax value, you would get an absolute magnitude of 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 -0.93 which gave the calculated distance to V520 Persei as -3507.13 light years away from Earth or -1075.27 parsecs. It would take a spaceship travelling at the speed of light, -3507.13 years to get there. We don't have the technology or spaceship that can carry people over that distance yet.
The star is a pulsating Slow Irregular 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. V520 Persei brightness ranges from a magnitude of 6.755 to a magnitude of 6.655 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.1 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.
|Primary / Proper / Traditional Name||V520 Persei|
|Alternative Names||HD 14134, HIP 10805, 61 Persei, 61 Per, BD+56 522, V520 Per|
|Constellation's Main Star||No|
|Multiple Star System||Yes|
|Star Type||very luminous Supergiant Star|
|Visual / Apparent Magnitude||6.57|
|Naked Eye Visible||Requires a 7x50 Binoculars - Magnitudes|
|Right Ascension (R.A.)||02h 19m 04.45|
|Declination (Dec.)||+57° 08` 07.8|
|Galactic Latitude||-3.73 degrees|
|Galactic Longitude||134.64 degrees|
|Distance from Earth||-0.93 Parallax (milliarcseconds)|
|-3507.13 Light Years|
|-221,788,812.77 Astronomical Units|
|Radial Velocity||-43.40 ± 1.60 km/s|
|Variable Star Class||Pulsating|
|Variable Star Type||Slow Irregular|
|Mean Variability Period in Days||0.079|
|Variable Magnitude Range (Brighter - Dimmer)||6.655 - 6.755|
|Effective Temperature||6,220 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|
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