HIP47279 is the reference name for the star in the Hipparcos Star Catalogue.
VV Ursae Majoris has alternative name(s) :- VV UMa, VV UMa.
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 1395.
More details on objects' alternative names can be found at Star Names .
The location of the main sequence 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 VV Ursae Majoris, the location is 09h 38m 06.74 and +56° 01` 07.2 .
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 1.94 ± 0.91 miliarcseconds/year towards the north and -18.38 ± 1.67 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 the Sun is -13.00 km/s with an error of about 7.40 km/s . When the value is negative then the star and the Sun are getting closer to one another, likewise, a positive number means that two stars are moving away. Its nothing to fear as the stars are so far apart, they won't collide in our life-time, if ever.
VV Ursae Majoris has a spectral type of A2V. This means the star is a blue main sequence star. The star has a B-V Colour Index of 0.14 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 8,153 Kelvin.
VV Ursae Majoris Radius has been calculated as being 107.23 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 74,613,893.82.km. If you need the diameter of the star, you just need to multiple the radius by 2. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 1.68. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
VV Ursae Majoris has an apparent magnitude of 10.19 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 -6.80 If you used the 2007 Parallax value, you would get an absolute magnitude of 2.23. 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 0.04 which gave the calculated distance to VV Ursae Majoris as 81540.84 light years away from Earth or 25000 parsecs. It would take a spaceship travelling at the speed of light, 81540.84 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 2.56 which put VV Ursae Majoris at a distance of 1274.08 light years or 390.62 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.
Using the 2007 distance, the star is roughly 80,570,597.19 Astronomical Units from the Earth/Sun give or take a few. An Astronomical Unit is the distance between Earth and the Sun. The number of A.U. is the number of times that the star is from the Earth compared to the Sun.
The star is a eclipsing Beta Persei (Algol)/ 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. VV Ursae Majoris brightness ranges from a magnitude of 10.975 to a magnitude of 10.195 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.7 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||VV Ursae Majoris|
|Alternative Names||VV UMa, HIP 47279, BD+56 1395, VV UMa|
|Constellation's Main Star||No|
|Multiple Star System||No / Unknown|
|Star Type||main sequence Dwarf Star|
|Absolute Magnitude||-6.80 / 2.23|
|Visual / Apparent Magnitude||10.19|
|Naked Eye Visible||Requires a 4.5 - 6 Inch Telescope - Magnitudes|
|Right Ascension (R.A.)||09h 38m 06.74|
|Declination (Dec.)||+56° 01` 07.2|
|Galactic Latitude||45.14 degrees|
|Galactic Longitude||159.22 degrees|
|1997 Distance from Earth||0.04 Parallax (milliarcseconds)|
|81540.84 Light Years|
|2007 Distance from Earth||2.56 Parallax (milliarcseconds)|
|1274.08 Light Years|
|80,570,597.19 Astronomical Units|
|Proper Motion Dec.||1.94 ± 0.91 milliarcseconds/year|
|Proper Motion RA.||-18.38 ± 1.67 milliarcseconds/year|
|Radial Velocity||-13.00 ± 7.40 km/s|
|Variable Star Class||Eclipsing|
|Variable Star Type||Beta Persei (Algol)/|
|Mean Variability Period in Days||0.687|
|Variable Magnitude Range (Brighter - Dimmer)||10.195 - 10.975|
|Radius (x the Sun)||1.68|
|Effective Temperature||8,153 Kelvin|
There's no register feature and no need to give an email address if you don't need to. All messages will be reviewed before being displayed. Comments may be merged or altered slightly such as if an email address is given in the main body of the comment.