V368 Cephei is a white to yellow eclipsing binary system main sequence dwarf star that can be located in the constellation of Cepheus. The star can not be seen by the naked eye, you need a telescope to see it.
HIP115147 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD220140.
V368 Cephei has alternative name(s), V368 Cep.
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 V368 Cephei, the location is 23h 19m 26.02 and +79d00`12.0 .
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 71.59 ± 0.38 miliarcseconds/year towards the north and 201.56 ± 0.47 miliarcseconds/year east if we saw them in the horizon.
V368 Cephei has a spectral type of G9V. This means the star is a white to yellow main sequence dwarf star. The star is 7409.00000000 Parsecs from the Galactic Centre or terms of Light Years is 24165.4421569600000000s. The star has a B-V Colour Index of 0.89 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 5,074 Kelvin.
V368 Cephei Radius has been calculated as being 0.74 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 518,355.26.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 0.72. 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 -0.19 with an error value of 9.99 Fe/H with the Sun has a value of 1 to put it into context.
V368 Cephei has an apparent magnitude of 7.53 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 6.05 If you used the 2007 Parallax value, you would get an absolute magnitude of 6.11. 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 50.65 which gave the calculated distance to V368 Cephei as 64.40 light years away from Earth or 19.74 parsecs. It would take a spaceship travelling at the speed of light, 64.40 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 52.07 which put V368 Cephei at a distance of 62.64 light years or 19.20 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's Galacto-Centric Distance is 7,409.00 Parsecs or 24,165.44 Light Years. The Galacto-Centric Distance is the distance from the star to the Centre of the Galaxy which is Sagittarius A*.
The star is a eclipsing binary system RS Canum Venaticorum 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. V368 Cephei brightness ranges from a magnitude of 7.703 to a magnitude of 7.630 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.1 days (variability).
|Traditional/Proper Name||V368 Cephei|
|Short Name||V368 Cep|
|Hipparcos Library I.D.||115147|
|Bonner Durchmusterung||BD+78 826|
|Henry Draper Designation||220140|
|Star Type||main sequence dwarf star|
|Absolute Magnitude||6.05 / 6.11|
|Visual / Apparent Magnitude||7.53|
|Naked Eye Visible||Requires a 7x50 Binoculars - Magnitudes|
|Right Ascension (R.A.)||23h 19m 26.02|
|Galactic Latitude||16.94 degrees|
|Galactic Longitude||118.46 degrees|
|1997 Distance from Earth||50.65 Parallax (milliarcseconds)|
|64.40 Light Years|
|2007 Revised Distance from Earth||52.07 Parallax (milliarcseconds)|
|62.64 Light Years|
|Galacto-Centric Distance||24,165.44 Light Years / 7,409.00 Parsecs|
|Proper Motion Dec.||71.59 ± 0.38 milliarcseconds/year|
|Proper Motion RA.||201.56 ± 0.47 milliarcseconds/year|
|Radial Velocity||-16.80 ± 2.00 km/s|
|Iron Abundance||-0.19 ± 9.99 Fe/H|
|Colour||(G) White to Yellow|
|Variable Star Class||Eclipsing binary system|
|Variable Star Type||RS Canum Venaticorum|
|Mean Variability Period in Days||0.054|
|Variable Magnitude Range (Brighter - Dimmer)||7.630 - 7.703|
|Calculated Effective Temperature||5,074 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|