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V378 Puppis, HD60855, HIP36981

V378 Puppis is a blue eclipsing main sequence dwarf star that can be located in the constellation of Puppis. 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.

V378 Puppis's Alternative Names

HIP36981 is the reference name for the star in the Hipparcos Star Catalogue. The Id of the star in the Henry Draper catalogue is HD60855.

V378 Puppis has alternative name(s) :- , V378 Pup.

The Gould star designation is one that was designed by American astronomer, Benjamin Apthorp Gould. Gould stars are predominantly in the Southern and Equatorial constellations but do appear in northern constellations such as Bootes and Orion. The star has the designation 122 G. Puppis. There are no stars with a Gould designation in Ursa Major for example.

BD number is the number that the star was filed under in the Durchmusterung or Bonner Durchmusterung, a star catalogue that was put together by the Bonn Observatory between 1859 to 1903. The star's BD Number is BD-14 1999.

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

Location of V378 Puppis

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 V378 Puppis, the location is 07h 36m 03.90 and -14° 29` 34.0 .

Proper Motion of V378 Puppis

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 0.38 ± 0.22 miliarcseconds/year towards the north and -6.70 ± 0.38 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 22.10000 km/s with an error of about 1.90 km/s .

V378 Puppis 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 1,101.59 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 V378 Puppis

V378 Puppis has a spectral type of B2/3V(n). This means the star is a blue main sequence dwarf star. The star is 7,657.00 Parsecs from the Galactic Centre or terms of Light Years is 24,974.33 s. 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 10,611 Kelvin.

V378 Puppis Radius has been calculated as being 10.36 times bigger than the Sun.The Sun's radius is 695,800km, therefore the star's radius is an estimated 7,209,470.64.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 7.93. The figure is derived at by using the formula from SDSS and has been known to produce widely incorrect figures.

V378 Puppis Apparent and Absolute Magnitudes

V378 Puppis has an apparent magnitude of 5.66 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 -2.87 If you used the 2007 Parallax value, you would get an absolute magnitude of -2.29. 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 V378 Puppis

Using the original Hipparcos data that was released in 1997, the parallax to the star was given as 1.97 which gave the calculated distance to V378 Puppis as 1655.65 light years away from Earth or 507.61 parsecs. It would take a spaceship travelling at the speed of light, 1655.65 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 2.57 which put V378 Puppis at a distance of 1269.12 light years or 389.11 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 7,657.00 Parsecs or 24,974.33 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 V378 Puppis

The star is a eclipsing 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. This is a some uncertainty as to the type but the type mentioned is the current variable star classification for this star. V378 Puppis brightness ranges from a magnitude of 5.682 to a magnitude of 5.597 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 0.1 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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V378 Puppis Facts

Visual Facts


Primary / Proper / Traditional NameV378 Puppis
Alternative NamesHD 60855, HIP 36981, 122 G. Puppis, BD-14 1999, V378 Pup
Spectral TypeB2/3V(n)
Multiple Star SystemYes
Star Type main sequence Dwarf Star
Colour blue
GalaxyMilky Way
ConstellationPuppis
Absolute Magnitude-2.87 / -2.29
Visual / Apparent Magnitude5.66
Naked Eye VisibleYes - Magnitudes
Right Ascension (R.A.)07h 36m 03.90
Declination (Dec.)-14° 29` 34.0
Galactic Latitude3.02 degrees
Galactic Longitude230.91 degrees
1997 Distance from Earth1.97 Parallax (milliarcseconds)
 1655.65 Light Years
 507.61 Parsecs
2007 Distance from Earth2.57 Parallax (milliarcseconds)
 1269.12 Light Years
 389.11 Parsecs
Galacto-Centric Distance24,974.33 Light Years / 7,657.00 Parsecs
Proper Motion Dec.0.38 ± 0.22 milliarcseconds/year
Proper Motion RA.-6.70 ± 0.38 milliarcseconds/year
B-V Index-0.06
Radial Velocity22.10 ± 1.90 km/s
Eccentricity0.05
Semi-Major Axis8074.00
Stellar Luminosity (Lsun)1,101.59

Companions (Multi-Star and Exoplanets) Facts


Exoplanet CountNone/Unaware

Variable Star Details


Variable Star ClassEclipsing
Variable Star TypeBeta Lyrae (Sheliak) probably
Mean Variability Period in Days0.087
Variable Magnitude Range (Brighter - Dimmer)5.597 - 5.682

Estimated Facts


Calculated Effective Temperature10,611 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
60855-14 1999.0A5.60000-6.00000-5.00000B5Blue/White
B12.200001928
-14 2000.0C9.500001830
D9.500001985
E9.500001985
F11.000001985

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