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Wurren, Zeta Phoenicis, HD6882, HIP5348, HR338

Wurren (Zeta Phoenicis) Location in Phoenix

Wurren (Zeta Phoenicis) is a blue eclipsing main sequence dwarf star that can be located in the constellation of Phoenix. 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.

Wurren's Alternative Names

Zeta Phoenicis (Zet Phe) is the Bayer Classification for the star. The Id of the star in the Yale Bright Star Catalogue is HR338. HIP5348 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD6882.

Wurren has alternative name(s) :- , zet Phe.

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

Location of Wurren

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 Wurren, the location is 01h 08m 23.06 and -55° 14` 45.0 .

Proper Motion of Wurren

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 30.64 ± 0.30 miliarcseconds/year towards the north and 20.87 ± 0.39 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 15.30000 km/s with an error of about 2.70 km/s .

Wurren Luminosity

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 381.79 that I have given is based on the value in the Simbad Hipparcos Extended Catalogue at the University of Strasbourg from 2012.

Physical Properties (Colour, Temperature) of Wurren

Wurren has a spectral type of B6V + B0V. This means the star is a blue main sequence dwarf star. The star is 7,380.00 Parsecs from the Galactic Centre or terms of Light Years is 24,070.85 s. 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 11,677 Kelvin.

Wurren Radius has been calculated as being 3.19 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 2,221,940.56.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 3.41. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

Wurren Apparent and Absolute Magnitudes

Wurren has an apparent magnitude of 3.94 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 -0.73 If you used the 2007 Parallax value, you would get an absolute magnitude of -0.87. 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 Wurren

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 11.66 which gave the calculated distance to Wurren as 279.73 light years away from Earth or 85.76 parsecs. It would take a spaceship travelling at the speed of light, 279.73 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 10.92 which put Wurren at a distance of 298.68 light years or 91.58 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 7,380.00 Parsecs or 24,070.85 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 Wurren

The star is a eclipsing Beta Persei (Algol)/Detached Main Sequence (subtype) 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. Wurren brightness ranges from a magnitude of 4.390 to a magnitude of 3.910 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 1.7 days (variability).

Meteor Showers Radiating from near Wurren

The Phoenicids Meteor Shower radiants from a point near this star. The meteor shower runs typically between Nov 29-Dec 9 with a peak date of Dec. 5/6. The speed of a meteor in the shower is 12 Km/s. The amount of meteors predicted to be seen per hour (Zenith Hourly Rate) is 12.

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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Wurren Facts

Visual Facts


Primary / Proper / Traditional NameWurren
Alternative NamesZeta Phoenicis, Zet Phe, HD 6882, HIP 5348, HR 338, zet Phe
Spectral TypeB6V + B0V
Multiple Star SystemYes
Star Type main sequence Dwarf Star
Colour blue
GalaxyMilky Way
ConstellationPhoenix
Absolute Magnitude-0.73 / -0.87
Visual / Apparent Magnitude3.94
Naked Eye VisibleYes - Magnitudes
Right Ascension (R.A.)01h 08m 23.06
Declination (Dec.)-55° 14` 45.0
Galactic Latitude-61.71 degrees
Galactic Longitude297.83 degrees
1997 Distance from Earth11.66 Parallax (milliarcseconds)
 279.73 Light Years
 85.76 Parsecs
2007 Distance from Earth10.92 Parallax (milliarcseconds)
 298.68 Light Years
 91.58 Parsecs
Galacto-Centric Distance24,070.85 Light Years / 7,380.00 Parsecs
Proper Motion Dec.30.64 ± 0.30 milliarcseconds/year
Proper Motion RA.20.87 ± 0.39 milliarcseconds/year
B-V Index-0.10
Radial Velocity15.30 ± 2.70 km/s
Eccentricity0.11
Semi-Major Axis8257.00
Stellar Luminosity (Lsun)381.79

Companions (Multi-Star and Exoplanets) Facts


Exoplanet CountNone/Unaware

Variable Star Details


Variable Star ClassEclipsing
Variable Star TypeBeta Persei (Algol)/Detached Main Sequence (subtype)
Mean Variability Period in Days1.670
Variable Magnitude Range (Brighter - Dimmer)3.910 - 4.390

Estimated Facts


Calculated Effective Temperature11,677 Kelvin

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
6882-55 241.4A4.2000010.0000030.00000B8Blue/White
B7.000001949
C7.000001835

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