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W Coronae Australis, HD164889, HIP88584

W Coronae Australis is a pulsating variable star that can be located in the constellation of Corona Australis. The description is based on the spectral class. W Coronae Australis is not part of the constellation but is within the borders of the constellation.

The star can not be seen by the naked eye, you need a telescope to see it.

W Coronae Australis's Alternative Names

HIP88584 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD164889.

W Coronae Australis has alternative name(s) :- , W CrA.

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

Location of W Coronae Australis

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 W Coronae Australis, the location is 18h 05m 12.24 and -39° 20` 32.3 .

Radial Velocity and Proper Motion of W Coronae Australis

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 -24.43 ± 1.04 miliarcseconds/year towards the north and 5.30 ± 1.69 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 the Sun is -99.90 km/s with an error of about 3.10 km/s . When the value is negative then the star and the Sun are getting closer to one another, likewise, a positive number means that two stars are moving away. Its nothing to fear as the stars are so far apart, they won't collide in our life-time, if ever.

Physical Properties of W Coronae Australis

W Coronae Australis has a spectral type of R5.

W Coronae Australis Apparent and Absolute Magnitudes

W Coronae Australis has an apparent magnitude of 9.82 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 0.69 If you used the 2007 Parallax value, you would get an absolute magnitude of -1.12. 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 W Coronae Australis

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 1.49 which gave the calculated distance to W Coronae Australis as 2189.02 light years away from Earth or 671.14 parsecs. It would take a spaceship travelling at the speed of light, 2189.02 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 0.65 which put W Coronae Australis at a distance of 5017.90 light years or 1538.46 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.

Using the 2007 distance, the star is roughly 317,327,942.65 Astronomical Units from the Earth/Sun give or take a few. An Astronomical Unit is the distance between Earth and the Sun. The number of A.U. is the number of times that the star is from the Earth compared to the Sun.

Variable Type of W Coronae Australis

The star is a pulsating Semiregular late- (M 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. W Coronae Australis brightness ranges from a magnitude of 10.180 to a magnitude of 9.910 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.3 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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W Coronae Australis Facts

Visual Facts

Primary / Proper / Traditional NameW Coronae Australis
Alternative NamesHD 164889, HIP 88584, W CrA
Spectral TypeR5
Constellation's Main StarNo
Multiple Star SystemYes
Star TypeVariable Star
GalaxyMilky Way
ConstellationCorona Australis
Absolute Magnitude 0.69 / -1.12
Visual / Apparent Magnitude9.82
Naked Eye VisibleRequires a 7x50 Binoculars - Magnitudes
Right Ascension (R.A.)18h 05m 12.24
Declination (Dec.)-39° 20` 32.3
Galactic Latitude-8.69 degrees
Galactic Longitude352.97 degrees
1997 Distance from Earth1.49 Parallax (milliarcseconds)
 2189.02 Light Years
 671.14 Parsecs
2007 Distance from Earth0.65 Parallax (milliarcseconds)
 5017.90 Light Years
 1538.46 Parsecs
 317,327,942.65 Astronomical Units
Proper Motion Dec.-24.43 ± 1.04 milliarcseconds/year
Proper Motion RA.5.30 ± 1.69 milliarcseconds/year
B-V Index-99.00
Radial Velocity-99.90 ± 3.10 km/s

Companions (Multi-Star and Exoplanets) Facts

Exoplanet CountNone/Unaware

Variable Star Details

Variable Star ClassPulsating
Variable Star TypeSemiregular late- (M
Mean Variability Period in Days0.323
Variable Magnitude Range (Brighter - Dimmer)9.910 - 10.180

Sources and Links

SIMBAD SourceLink

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

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