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GW Orionis, HD244138, HIP25689

GW Orionis is a white to yellow eruptive main sequence dwarf star that can be located in the constellation of Orion. The description is based on the spectral class. The star can not be seen by the naked eye, you need a telescope to see it.

GW Orionis's Alternative Names

HIP25689 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD244138.

GW Orionis has alternative name(s) :- , GW Ori.

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+11 819.

More details on star alternative names can be found at Star Names .

Location of GW Orionis

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 GW Orionis, the location is 05h 29m 08.39 and +11° 52` 12.7 .

Proper Motion of GW Orionis

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 2.78 ± 0.77 miliarcseconds/year towards the north and 0.26 ± 1.39 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 28.06000 km/s with an error of about 0.20 km/s .

Physical Properties (Colour, Temperature) of GW Orionis

GW Orionis has a spectral type of G5.8Ve.... This means the star is a white to yellow main sequence dwarf star. The star has a B-V Colour Index of 0.97 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 4,907 Kelvin.

GW Orionis Radius has been calculated as being 4.26 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 2,963,002.75.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 3.80. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

GW Orionis Apparent and Absolute Magnitudes

GW Orionis has an apparent magnitude of 9.85 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 2.41 If you used the 2007 Parallax value, you would get an absolute magnitude of 2.66. 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 GW Orionis

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 3.25 which gave the calculated distance to GW Orionis as 1003.58 light years away from Earth or 307.69 parsecs. It would take a spaceship travelling at the speed of light, 1003.58 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 3.64 which put GW Orionis at a distance of 896.05 light years or 274.73 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.

Variable Type of GW Orionis

The star is a eruptive Irregular 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. GW Orionis brightness ranges from a magnitude of 10.058 to a magnitude of 9.904 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.1 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.

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GW Orionis Facts

Visual Facts


 GW Orionis
Alternative NamesHD 244138, HIP 25689, BD+11 819, GW Ori
Spectral TypeG5.8Ve...
Multiple Star SystemNo / Unknown
Star Type main sequence Dwarf Star
Colour white to yellow
GalaxyMilky Way
ConstellationOrion
Absolute Magnitude2.41 / 2.66
Visual / Apparent Magnitude9.85
Naked Eye VisibleRequires a 7x50 Binoculars - Magnitudes
Right Ascension (R.A.)05h 29m 08.39
Declination (Dec.)+11° 52` 12.7
Galactic Latitude-12.26 degrees
Galactic Longitude192.58 degrees
1997 Distance from Earth3.25 Parallax (milliarcseconds)
 1003.58 Light Years
 307.69 Parsecs
2007 Distance from Earth3.64 Parallax (milliarcseconds)
 896.05 Light Years
 274.73 Parsecs
Proper Motion Dec.2.78 ± 0.77 milliarcseconds/year
Proper Motion RA.0.26 ± 1.39 milliarcseconds/year
B-V Index0.97
Radial Velocity28.06 ± 0.20 km/s

Companions (Multi-Star and Exoplanets) Facts


Exoplanet CountNone/Unaware

Variable Star Details


Variable Star ClassEruptive
Variable Star TypeIrregular
Mean Variability Period in Days0.125
Variable Magnitude Range (Brighter - Dimmer)9.904 - 10.058

Estimated Facts


Calculated Effective Temperature4,907 Kelvin

Sources and Links


SIMBAD SourceLink

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