Pi-3 Ursae Minoris is a blue to white star that can be located in the constellation of UrsaMinor. The star can not be seen by the naked eye, you need a telescope to see it. The star has an estimated age of 1.10 Billion of Years but could be as young as 1.00 to 1.20 according to Hipparcos.
Pi-3 Ursae Minoris is the Bayer Classification for the star. HIP76695 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD141652.
Pi-3 Ursae Minoris has alternative name(s), 18 Ursae Minoris , 18 UMi. Pi-3 Ursae Minoris is a multiple star system with 2 stars orbiting in its solar system.
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 Pi-3 Ursae Minoris, the location is 15h 39m 38.72 and +79d58`59.2 .
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 40.28 ± 0.72 miliarcseconds/year towards the north and -32.92 ± 0.61 miliarcseconds/year east if we saw them in the horizon.
Pi-3 Ursae Minoris has a spectral type of F2. This means the star is a blue to white star. The star is 7442.00000000 Parsecs from the Galactic Centre or terms of Light Years is 24273.0760604800000000s. The star has a B-V Colour Index of 0.39 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 6,431 Kelvin.
Pi-3 Ursae Minoris Radius has been calculated as being 3.70 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 2,575,228.04.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 3.79. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures. The star's solar mass is 2.00 times that of the Sun's. The Sun's Mass is 1,989,100,000,000,000,000,000 billion kg. which to calculate using this website is too large. To give idea of size, the Sun is 99.86% the mass of the solar system.
The star's metallicity is -0.030000, this value is the fractional amount of the star that is not Hydrogen (X) or Helium (Y). An older star would have a high metallicity whereas a new star would have a lower one.
The stars age according to Hipparcos data files put the star at an age of about 1.10 Billion years old but could be between 1.00 and 1.20 Billion years old. In comparison, the Sun's age is about 4.6 Billion Years Old.
Pi-3 Ursae Minoris has an apparent magnitude of 6.89 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 1.54 If you used the 2007 Parallax value, you would get an absolute magnitude of 1.49. 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 8.50 which gave the calculated distance to Pi-3 Ursae Minoris as 383.72 light years away from Earth or 117.65 parsecs. It would take a spaceship travelling at the speed of light, 383.72 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 8.33 which put Pi-3 Ursae Minoris at a distance of 391.55 light years or 120.05 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 7,442.00 Parsecs or 24,273.08 Light Years. The Galacto-Centric Distance is the distance from the star to the Centre of the Galaxy which is Sagittarius A*.
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.
|Short Name||18 UMi|
|Bayer Designation||Pi-3 Ursae Minoris|
|Alternative Name(s)||18 Ursae Minoris|
|Hipparcos Library I.D.||76695|
|Bonner Durchmusterung||BDD+80 487|
|Henry Draper Designation||141652|
|Age||1.10 Billion Years Old|
|Age Range||1.00 - 1.20 Billion Years Old|
|Absolute Magnitude||1.54 / 1.49|
|Visual / Apparent Magnitude||6.89|
|Naked Eye Visible||Requires a 7x50 Binoculars - Ref: Wiki|
|Right Ascension (R.A.)||15h 39m 38.72|
|Galactic Latitude||34.33 degrees|
|Galactic Longitude||114.82 degrees|
|1997 Distance from Earth||8.50 Parallax (milliarcseconds)|
|383.72 Light Years|
|2007 Revised Distance from Earth||8.33 Parallax (milliarcseconds)|
|391.55 Light Years|
|Galacto-Centric Distance||24,273.08 Light Years / 7,442.00 Parsecs|
|Proper Motion Dec.||40.28 ± 0.72 milliarcseconds/year|
|Proper Motion RA.||-32.92 ± 0.61 milliarcseconds/year|
|Radial Velocity||-32.10 ± 1.80 km/s|
|Iron Abundance||0.16 ± 0.15 Fe/H|
|Colour||(F) blue to white|
|Stars in Solar System||2|
|Calculated Effective Temperature||6,431 Kelvin|
|Mass Compared to the Sun||2.00|
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|