V755 Cassiopeiae is a blue eclipsing binary system supergiant star that can be located in the constellation of Cassiopeia. The star can not be seen by the naked eye, you need a telescope to see it.
HIP3367 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD3940.
V755 Cassiopeiae has alternative name(s) :- , V755 Cas.
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+63 81.
More details on star alternative names can be found at Star Names.
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 V755 Cassiopeiae, the location is 00h 42m 50.07 and +64° 17` 28.6 .
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 -0.48 ± 0.35 miliarcseconds/year towards the north and -3.59 ± 0.54 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 us is -58.20000 km/s with an error of about 1.90 km/s .
V755 Cassiopeiae has a spectral type of A1Ia. This means the star is a blue supergiant star. The star has a B-V Colour Index of 0.6 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 5,875 Kelvin.
V755 Cassiopeiae Radius has been calculated as being 71.60 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 49,821,439.01.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 36.22. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures. The star's Iron Abundance is -0.39 with an error value of 9.99 Fe/H with the Sun has a value of 1 to put it into context.
V755 Cassiopeiae has an apparent magnitude of 7.28 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 -4.50 If you used the 2007 Parallax value, you would get an absolute magnitude of -3.02. 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 0.44 which gave the calculated distance to V755 Cassiopeiae as 7412.80 light years away from Earth or 2272.73 parsecs. It would take a spaceship travelling at the speed of light, 7412.80 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 0.87 which put V755 Cassiopeiae at a distance of 3749.00 light years or 1149.43 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 eclipsing binary system 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. V755 Cassiopeiae brightness ranges from a magnitude of 7.443 to a magnitude of 7.378 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.0 days (variability).
|Alternative Names||HD 3940, HIP 3367, BD+63 81, V755 Cas|
|Star Type||very luminous Supergiant Star|
|Absolute Magnitude||-4.50 / -3.02|
|Visual / Apparent Magnitude||7.28|
|Naked Eye Visible||Requires a 7x50 Binoculars - Magnitudes|
|Right Ascension (R.A.)||00h 42m 50.07|
|Declination (Dec.)||+64° 17` 28.6|
|Galactic Latitude||1.44 degrees|
|Galactic Longitude||122.00 degrees|
|1997 Distance from Earth||0.44 Parallax (milliarcseconds)|
|7412.80 Light Years|
|2007 Revised Distance from Earth||0.87 Parallax (milliarcseconds)|
|3749.00 Light Years|
|Proper Motion Dec.||-0.48 ± 0.35 milliarcseconds/year|
|Proper Motion RA.||-3.59 ± 0.54 milliarcseconds/year|
|Radial Velocity||-58.20 ± 1.90 km/s|
|Iron Abundance||-0.39 ± 9.99 Fe/H|
|Variable Star Class||Eclipsing binary system|
|Variable Star Type||Beta Persei (Algol)|
|Mean Variability Period in Days||0.042|
|Variable Magnitude Range (Brighter - Dimmer)||7.378 - 7.443|
|Calculated Effective Temperature||5,875 Kelvin|