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V Cancri - HD70276 - HIP40977

V Cancri is a pulsating star that can be located in the constellation of Cancer. 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.

Location of V Cancri

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 +17d17`07.0 .

Physical Properties (Temperature, Radius) of V Cancri

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 has been calculated as 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.

V Cancri Apparent and Absolute Magnitudes

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. If you used the 1997 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.

Distance to V Cancri

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.

Variable Type of V Cancri

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 12.000 to a magnitude of 7.000 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 278.0 days (variability).

Source of Information

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.

V Cancri Facts

Alternative Names

Traditional NameV Cancri
Short NameV Cnc
Hipparcos Library I.D.40977
Bonner DurchmusterungBD+17 1825
Henry Draper Designation70276

Visual Facts

Star Type star
Apparent Magnitude9.25
Right Ascension (R.A.)08h 21m 42.91
Declination (Dec.)+17d17`07.0
1997 Distance from Earth26.58 Parallax (milliarcseconds)
 122.71 Light Years
 37.62 Parsecs
B-V Index2.08
Spectral TypeSevar

Variable Star Details

Variable Star ClassPulsating
Variable Star TypeOmicron Ceti
Mean Variability Period in Days278.000
Variable Magnitude Range (Brighter - Dimmer)7.000 - 12.000

Estimated Facts

Radius (x the Sun)9.70
Calculated Effective Temperature1,306 Kelvin

Sources and Links

SIMBAD SourceLink

Related Stars

Multi-Star System

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. IdB.D. IdStar CodeMagnitudeR.A.Dec.SpectrumColourYear
70276+17 1825.0A3.0000010.00000M4Red
B1917

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