V575 Persei is a blue main sequence dwarf star that can be located in the constellation of Perseus. The description is based on the spectral class. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it.
HIP15770 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD20809.
V575 Persei has alternative name(s) :- , V575 Per.
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+48 899.
More details on star alternative names can be found at Star Names .
The location of the star in the night sky 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 V575 Persei, the location is 03h 23m 13.18 and +49° 12` 48.0 .
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 -25.84 ± 0.22 miliarcseconds/year towards the north and 21.40 ± 0.33 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 -0.50000 km/s with an error of about 0.80 km/s .
Luminosity is the amount of energy that a star pumps out and its relative to the amount that our star, the Sun gives out. The figure of 329.08 that I have given is based on the value in the Simbad Hipparcos Extended Catalogue at the University of Strasbourg from 2012.
V575 Persei has a spectral type of B5V. This means the star is a blue main sequence dwarf star. The star is 7,552.00 Parsecs from the Galactic Centre or terms of Light Years is 24,631.86 s. The star has a B-V Colour Index of -0.07 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 10,845 Kelvin.
V575 Persei Radius has been calculated as being 4.37 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 3,040,460.87.km. If you need the diameter of the star, you just need to multiple the radius by 2. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 3.79. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.
V575 Persei has an apparent magnitude of 5.32 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 -1.09 If you used the 2007 Parallax value, you would get an absolute magnitude of -0.78. 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 5.22 which gave the calculated distance to V575 Persei as 624.83 light years away from Earth or 191.57 parsecs. It would take a spaceship travelling at the speed of light, 624.83 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 6.02 which put V575 Persei at a distance of 541.80 light years or 166.11 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 7,552.00 Parsecs or 24,631.86 Light Years. The Galacto-Centric Distance is the distance from the star to the Centre of the Galaxy which is Sagittarius A*. V575 Persei brightness ranges from a magnitude of 5.316 to a magnitude of 5.267 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.1 days (variability).
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.
|Primary / Proper / Traditional Name||V575 Persei|
|Alternative Names||HD 20809, HIP 15770, BD+48 899, V575 Per|
|Multiple Star System||No / Unknown|
|Star Type||main sequence Dwarf Star|
|Absolute Magnitude||-1.09 / -0.78|
|Visual / Apparent Magnitude||5.32|
|Naked Eye Visible||Yes - Magnitudes|
|Right Ascension (R.A.)||03h 23m 13.18|
|Declination (Dec.)||+49° 12` 48.0|
|Galactic Latitude||-6.50 degrees|
|Galactic Longitude||146.78 degrees|
|1997 Distance from Earth||5.22 Parallax (milliarcseconds)|
|624.83 Light Years|
|2007 Distance from Earth||6.02 Parallax (milliarcseconds)|
|541.80 Light Years|
|Galacto-Centric Distance||24,631.86 Light Years / 7,552.00 Parsecs|
|Proper Motion Dec.||-25.84 ± 0.22 milliarcseconds/year|
|Proper Motion RA.||21.40 ± 0.33 milliarcseconds/year|
|Radial Velocity||-0.50 ± 0.80 km/s|
|Stellar Luminosity (Lsun)||329.08|
|Mean Variability Period in Days||0.051|
|Variable Magnitude Range (Brighter - Dimmer)||5.267 - 5.316|
|Calculated Effective Temperature||10,845 Kelvin|