Universe Guide


X Trianguli, HD12211, HIP9383

X Trianguli is a blue eclipsing main sequence dwarf star that can be located in the constellation of Triangulum. The star can not be seen by the naked eye, you need a telescope to see it.

HIP9383 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD12211.

X Trianguli has alternative name(s), X Tri.

Location of X Trianguli

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 X Trianguli, the location is 02h 00m 33.72 and +27d53`19.3 .

Proper Motion of X Trianguli

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 -15.41 ± 1.32 miliarcseconds/year towards the north and 29.35 ± 1.97 miliarcseconds/year east if we saw them in the horizon.

X Trianguli 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 9.0000000 that I have given is based on the Spectral Types page that I have found on the Internet. You might find a different figure, one that may have been calculated rather than generalised that I have done. The figure is always the amount times the luminosity of the Sun. It is an imprecise figure because of a number of factors including but not limited to whether the star is a variable star and distance.

Physical Properties (Colour, Temperature, Radius) of X Trianguli

X Trianguli has a spectral type of A7V. This means the star is a blue main sequence dwarf star. The star has a B-V Colour Index of 0.34 which means the star's temperature has been calculated using information from Morgans @ Uni.edu at being 7,016 Kelvin.

X Trianguli Radius has been calculated as being 1.77 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 1,233,620.49.km. However with the 2007 release of updated Hipparcos files, the radius is now calculated at being round 1.50. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

X Trianguli Apparent and Absolute Magnitudes

X Trianguli has an apparent magnitude of 8.86 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 2.76 If you used the 2007 Parallax value, you would get an absolute magnitude of 3.12. 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 X Trianguli

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 6.03 which gave the calculated distance to X Trianguli as 540.90 light years away from Earth or 165.84 parsecs. It would take a spaceship travelling at the speed of light, 540.90 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 7.12 which put X Trianguli at a distance of 458.09 light years or 140.45 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 X Trianguli

The star is a eclipsing Beta Persei (Algol)/Semi-Detached System (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. X Trianguli brightness ranges from a magnitude of 11.150 to a magnitude of 8.850 over its variable period. The smaller the magnitude, the brighter the star.

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.

X Trianguli Facts

Alternative Names

Traditional/Proper NameX Trianguli
Short NameX Tri
Hipparcos Library I.D.9383
Bonner DurchmusterungBD+27 318
Henry Draper Designation12211

Visual Facts

Star Typemain sequence dwarf star
Absolute Magnitude2.76 / 3.12
Visual / Apparent Magnitude8.86
Naked Eye VisibleRequires a 7x50 Binoculars - Magnitudes
Right Ascension (R.A.)02h 00m 33.72
Declination (Dec.)+27d53`19.3
Galactic Latitude-32.54 degrees
Galactic Longitude141.08 degrees
1997 Distance from Earth6.03 Parallax (milliarcseconds)
 540.90 Light Years
 165.84 Parsecs
2007 Revised Distance from Earth7.12 Parallax (milliarcseconds)
 458.09 Light Years
 140.45 Parsecs
Proper Motion Dec.-15.41 ± 1.32 milliarcseconds/year
Proper Motion RA.29.35 ± 1.97 milliarcseconds/year
B-V Index0.34
Radial Velocity-5.00 ± 4.60 km/s
Spectral TypeA7V
Colour(A) blue

Variable Star Details

Variable Star ClassEclipsing
Variable Star TypeBeta Persei (Algol)/Semi-Detached System (subtype)
Variable Magnitude Range (Brighter - Dimmer)8.850 - 11.150

Estimated Facts

Luminosity (x the Sun)9.0000000
Calculated Effective Temperature7,016 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
12211+27 318.0A8.8000037.00000-3.00000A2White

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