V Cancri is a pulsating star that can be located in the constellation of Cancer. The star can not be seen by the naked eye, you need a telescope to see it.
HIP40977 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD70276.
V Cancri has alternative name(s), V Cnc.
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 Cancri, the location is 08h 21m 42.91 and +17d 17` 07.0 .
V Cancri has a spectral type of Sevar. This means the star is a star. The star has a B-V Colour Index of 2.08 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 1,306 Kelvin.
V Cancri Radius has been calculated as being 9.70 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 6,752,101.13.km. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
V Cancri has an apparent magnitude of 9.25 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 6.37 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 26.58 which gave the calculated distance to V Cancri as 122.71 light years away from Earth or 37.62 parsecs. It would take a spaceship travelling at the speed of light, 122.71 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 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 Cancri brightness ranges from a magnitude of 11.823 to a magnitude of 7.340 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 277.8 days (variability).
|Traditional/Proper Name||V Cancri|
|Short Name||V Cnc|
|Hipparcos Library I.D.||40977|
|Bonner Durchmusterung||BD+17 1825|
|Henry Draper Designation||70276|
|Visual / Apparent Magnitude||9.25|
|Naked Eye Visible||Requires a 7x50 Binoculars - Magnitudes|
|Right Ascension (R.A.)||08h 21m 42.91|
|Declination (Dec.)||+17d 17` 07.0|
|Galactic Latitude||27.49 degrees|
|Galactic Longitude||206.63 degrees|
|Distance from Earth||26.58 Parallax (milliarcseconds)|
|122.71 Light Years|
|Radial Velocity||-4.60 ± 0.80 km/s|
|Variable Star Class||Pulsating|
|Variable Star Type||Omicron Ceti|
|Mean Variability Period in Days||277.800|
|Variable Magnitude Range (Brighter - Dimmer)||7.340 - 11.823|
|Calculated Effective Temperature||1,306 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|