V Coronae Borealis is a pulsating star that can be located in the constellation of CoronaBorealis. HIP77501 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD141826. V Coronae Borealis has alternative name(s), V_CrB.
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 Coronae Borealis, the location is 15h 49m 31.31 and +39d34`18.0 .
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 -012.45 ± 000.87 towards the north and 004.60 ± 001.08 east if we saw them in the horizon.
V Coronae Borealis has a spectral type of N2. This means the star is a star. The star has a B-V Colour Index of 4.41 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 0 Kelvin.
V Coronae Borealis has an apparent magnitude of 10.10 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 -1.36 If you used the 2007 Parallax value, you would get an absolute magnitude of -2.06. 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 0.51 which gave the calculated distance to V Coronae Borealis as 6395.36 light years away from Earth or 1960.78 parsecs. It would take a spaceship travelling at the speed of light, 6395.36 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 0.37 which put V Coronae Borealis at a distance of 8815.23 light years or 2702.70 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 Omicron Ceti 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 Coronae Borealis brightness ranges from a magnitude of 10.000 to a magnitude of 8.000 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 358.0 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 Stellar Age, Metallicity or Mass is from the E.U. Exoplanets. The information was obtained as of 12th Feb 2017.
|Traditional Name||V Coronae Borealis|
|Short Name||V CrB|
|Hipparcos Library I.D.||77501|
|Bonner Durchmusterung||BD+40 2929|
|Henry Draper Designation||141826|
|Absolute Magnitude||-1.36 / -2.06|
|Right Ascension (R.A.)||15h 49m 31.31|
|1997 Distance from Earth||0.51 Parallax (milliarcseconds)|
|6395.36 Light Years|
|2007 Revised Distance from Earth||0.37 Parallax (milliarcseconds)|
|8815.23 Light Years|
|Proper Motion Dec.||-12.45 ± 0.87 milliarcseconds/year|
|Proper Motion RA.||4.60 ± 1.08 milliarcseconds/year|
|Variable Star Class||Pulsating|
|Variable Star Type||Omicron Ceti|
|Mean Variability Period in Days||358.000|
|Variable Magnitude Range (Brighter - Dimmer)||8.000 - 10.000|