Universe Guide

HomeFactsConstellationsUrsa Major

84 Ursae Majoris - HD120198 - HIP67231

84 Ursae Majoris is a blue rotating star that can be located in the constellation of UrsaMajor. It is calculated at being 5.000 Billion Years old. This information comes from ExoPlanet. HIP67231 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD120198. 84 Ursae Majoris has alternative name(s), 84 Ursae Majoris , CR_UMa, 84 UMa.

Location of 84 Ursae Majoris

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 84 Ursae Majoris, the location is 13h 46m 35.68 and +54d25`57.7 .

Proper Motion of 84 Ursae Majoris

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 -005.09 ± 000.20 towards the north and -018.69 ± 000.23 east if we saw them in the horizon.

Physical Properties (Colour, Temperature, Age, Mass, Radius) of 84 Ursae Majoris

84 Ursae Majoris has a spectral type of B9p EuCr. This means the star is a blue star. The star has a B-V Colour Index of -0.03 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 11,122 Kelvin.

84 Ursae Majoris has been calculated as 1.59 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 1,104,109.71.km. The star's solar mass is 1.00 times that of the Sun's. The Sun's Mass is 1,989,100,000,000,000,000,000 billion kg. which to calculate using this website is too large. To give idea of size, the Sun is 99.86% the mass of the solar system.

The star's metallicity is -0.250000, this value is the fractional amount of the star that is not Hydrogen (X) or Helium (Y). An older star would have a high metallicity whereas a new star would have a lower one.

The star is believed to be about 5.00 Billion years old. To put in context, the Sun is believed to be about five billion years old and the Universe is about 13.8 billion years old.

84 Ursae Majoris Apparent and Absolute Magnitudes

84 Ursae Majoris has an apparent magnitude of 5.68 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 1.00 If you used the 2007 Parallax value, you would get an absolute magnitude of 0.93. 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 84 Ursae Majoris

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 11.58 which gave the calculated distance to 84 Ursae Majoris as 281.66 light years away from Earth or 86.36 parsecs. It would take a spaceship travelling at the speed of light, 281.66 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 11.23 which put 84 Ursae Majoris at a distance of 290.44 light years or 89.05 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 84 Ursae Majoris

The star is a rotating Alpha2 Canum Venaticorum 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. 84 Ursae Majoris 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 1.0 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 Stellar Age, Metallicity or Mass is from the E.U. Exoplanets. The information was obtained as of 12th Feb 2017.

84 Ursae Majoris Facts

Alternative Names

Traditional Name84 Ursae Majoris
Short NameCR UMa, 84 UMa
Alternative Name(s)84 Ursae Majoris
Hipparcos Library I.D.67231
Bonner DurchmusterungBD+55 1634
Henry Draper Designation120198

Visual Facts

Star Type star
Age5.000 Billions of Years
Absolute Magnitude1.00 / 0.93
Apparent Magnitude5.68
Right Ascension (R.A.)13h 46m 35.68
Declination (Dec.)+54d25`57.7
1997 Distance from Earth11.58 Parallax (milliarcseconds)
 281.66 Light Years
 86.36 Parsecs
2007 Revised Distance from Earth11.23 Parallax (milliarcseconds)
 290.44 Light Years
 89.05 Parsecs
Proper Motion Dec.-5.09 ± 0.20 milliarcseconds/year
Proper Motion RA.-18.69 ± 0.23 milliarcseconds/year
B-V Index-0.03
Spectral TypeB9p EuCr
Colour(B) blue

Variable Star Details

Variable Star ClassRotating
Variable Star TypeAlpha2 Canum Venaticorum
Mean Variability Period in Days1.000

Estimated Facts

Radius (x the Sun)1.59
Calculated Effective Temperature11,122 Kelvin
Mass Compared to the Sun1.00

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
120198+55 1634.0A5.50000-25.000001.00000A0White

Add a Comment

Email: (Optional)