Universe Guide


V572 Persei, HD20096, HIP15193

V572 Persei is a blue eclipsing binary system star that can be located in the constellation of Perseus. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it.

HIP15193 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD20096.

V572 Persei has alternative name(s), V572 Per.

Location of V572 Persei

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 V572 Persei, the location is 03h 15m 48.65 and +50d57`21.5 .

Proper Motion of V572 Persei

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 -34.55 ± 0.58 miliarcseconds/year towards the north and 29.90 ± 0.77 miliarcseconds/year east if we saw them in the horizon.

Physical Properties (Colour, Temperature, Radius) of V572 Persei

V572 Persei has a spectral type of A0. This means the star is a blue star. The star is 7509.00000000 Parsecs from the Galactic Centre or terms of Light Years is 24491.6055009600000000s. The star has a B-V Colour Index of 0.1 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 8,434 Kelvin.

V572 Persei Radius has been calculated as being 2.82 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 1,964,768.15.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 3.01. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

V572 Persei Apparent and Absolute Magnitudes

V572 Persei has an apparent magnitude of 6.46 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 0.95 If you used the 2007 Parallax value, you would get an absolute magnitude of 0.81. 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 V572 Persei

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 7.90 which gave the calculated distance to V572 Persei as 412.86 light years away from Earth or 126.58 parsecs. It would take a spaceship travelling at the speed of light, 412.86 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 7.41 which put V572 Persei at a distance of 440.17 light years or 134.95 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 7,509.00 Parsecs or 24,491.61 Light Years. The Galacto-Centric Distance is the distance from the star to the Centre of the Galaxy which is Sagittarius A*.

Variable Type of V572 Persei

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. V572 Persei brightness ranges from a magnitude of 6.790 to a magnitude of 6.504 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 1.2 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 Metallicity and/or Mass is from the E.U. Exoplanets. The information was obtained as of 12th Feb 2017.

V572 Persei Facts

Alternative Names

Traditional/Proper NameV572 Persei
Short NameV572 Per
Hipparcos Library I.D.15193
Bonner DurchmusterungBD+50 725
Henry Draper Designation20096

Visual Facts

Star Type star
Absolute Magnitude0.95 / 0.81
Visual / Apparent Magnitude6.46
Naked Eye VisibleYes - Magnitudes
Right Ascension (R.A.)03h 15m 48.65
Declination (Dec.)+50d57`21.5
Galactic Latitude-5.67 degrees
Galactic Longitude144.83 degrees
1997 Distance from Earth7.90 Parallax (milliarcseconds)
 412.86 Light Years
 126.58 Parsecs
2007 Revised Distance from Earth7.41 Parallax (milliarcseconds)
 440.17 Light Years
 134.95 Parsecs
Galacto-Centric Distance24,491.61 Light Years / 7,509.00 Parsecs
Proper Motion Dec.-34.55 ± 0.58 milliarcseconds/year
Proper Motion RA.29.90 ± 0.77 milliarcseconds/year
B-V Index0.10
Spectral TypeA0
Colour(A) blue

Variable Star Details

Variable Star ClassEclipsing binary system
Variable Star TypeBeta Persei (Algol)
Mean Variability Period in Days1.213
Variable Magnitude Range (Brighter - Dimmer)6.504 - 6.790

Estimated Facts

Calculated Effective Temperature8,434 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
20096+50 725.0A6.8000025.00000-36.00000A0White

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