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14 Lacertae - HD216200 - HIP112778

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

HIP112778 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD216200.

14 Lacertae has alternative name(s), 14 Lacertae , V360_Lac, 14 Lac. 14 Lacertae is a multiple star system with 2 stars orbiting in its solar system.

Location of 14 Lacertae

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 14 Lacertae, the location is 22h 50m 21.77 and +41d57`12.3 .

Proper Motion of 14 Lacertae

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 -3.73 ± 0.30 miliarcseconds/year towards the north and 7.96 ± 0.46 miliarcseconds/year east if we saw them in the horizon.

Physical Properties (Colour, Temperature, Radius) of 14 Lacertae

14 Lacertae has a spectral type of B3IV:var. This means the star is a blue subgiant star. The star is 7464.00000000 Parsecs from the Galactic Centre or terms of Light Years is 24344.8319961600000000s. The star has a B-V Colour Index of 0.06 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 8,815 Kelvin.

14 Lacertae Radius has been calculated as being 8.76 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 6,094,806.00.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 9.17. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

14 Lacertae Apparent and Absolute Magnitudes

14 Lacertae has an apparent magnitude of 5.91 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 -1.70 If you used the 2007 Parallax value, you would get an absolute magnitude of -1.80. 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 14 Lacertae

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 3.00 which gave the calculated distance to 14 Lacertae as 1087.21 light years away from Earth or 333.33 parsecs. It would take a spaceship travelling at the speed of light, 1087.21 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 2.87 which put 14 Lacertae at a distance of 1136.46 light years or 348.43 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 7,464.00 Parsecs or 24,344.83 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 14 Lacertae

The star is a eclipsing binary system Beta Lyrae (Sheliak) 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. 14 Lacertae brightness ranges from a magnitude of 6.000 to a magnitude of 6.000 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 10.0 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.

14 Lacertae Facts

Alternative Names

Traditional/Proper Name14 Lacertae
Short NameV360 Lac, 14 Lac
Alternative Name(s)14 Lacertae
Hipparcos Library I.D.112778
Bonner DurchmusterungBDD+41 4623
Henry Draper Designation216200

Visual Facts

Star Typesubgiant star
Absolute Magnitude-1.70 / -1.80
Visual / Apparent Magnitude5.91
Naked Eye VisibleYes - Ref: Wiki
Right Ascension (R.A.)22h 50m 21.77
Declination (Dec.)+41d57`12.3
Galactic Latitude-15.47 degrees
Galactic Longitude100.04 degrees
1997 Distance from Earth3.00 Parallax (milliarcseconds)
 1087.21 Light Years
 333.33 Parsecs
2007 Revised Distance from Earth2.87 Parallax (milliarcseconds)
 1136.46 Light Years
 348.43 Parsecs
Galacto-Centric Distance24,344.83 Light Years / 7,464.00 Parsecs
Proper Motion Dec.-3.73 ± 0.30 milliarcseconds/year
Proper Motion RA.7.96 ± 0.46 milliarcseconds/year
B-V Index0.06
Radial Velocity-15.80 ± 3.10 km/s
Spectral TypeB3IV:var
Colour(B) blue
Stars in Solar System2

Variable Star Details

Variable Star ClassEclipsing binary system
Variable Star TypeBeta Lyrae (Sheliak)
Mean Variability Period in Days10.000

Estimated Facts

Calculated Effective Temperature8,815 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
216200+41 4623.0A6.000008.00000-4.00000B3Blue/White
B9.400008.00000-4.000001991

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