HIP31905 is the reference name for the star in the Hipparcos Star Catalogue.
BE Monocerotis has alternative name(s) :- BE Mon, BE Mon.
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+07 1394.
More details on objects' alternative names can be found at Star Names .
The location of the variable 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 object is compared to the celestial equator and is expressed in degrees. For BE Monocerotis, the location is 06h 40m 05.58 and +07° 36` 21.0 .
BE Monocerotis has a spectral type of F6.7. This means the star is a yellow to white variable star. The star has a B-V Colour Index of 1.14 which means the star's temperature is about 4,683 Kelvin. The temperature was calculated using information from Morgans @ Uni.edu at being .
BE Monocerotis has an apparent magnitude of 10.50 which is how bright we see the star from Earth. Apparent Magnitude is also known as Visual Magnitude. Using the supplied Parallax value, you would get an absolute magnitude of 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.
Using the original Hipparcos data that was released in 1997, the parallax to the star was given as -0.28 which gave the calculated distance to BE Monocerotis as -11648.69 light years away from Earth or -3571.43 parsecs. If you want that in miles, it is -7,811,805,220,066.
The star is a pulsating Delta Cepheid 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. BE Monocerotis brightness ranges from a magnitude of 10.993 to a magnitude of 10.395 over its variable period. The smaller the magnitude, the brighter the star. Its variable/pulsating period lasts for 2.7 days (variability).
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.
|Primary / Proper / Traditional Name||BE Monocerotis|
|Alternative Names||BE Mon, HIP 31905, BD+07 1394, BE Mon|
|Constellation's Main Star||No|
|Multiple Star System||No / Unknown|
|Star Type||Variable Star|
|Colour||Yellow - White|
|Visual / Apparent Magnitude||10.50|
|Naked Eye Visible||Requires a 4.5 - 6 Inch Telescope - Magnitudes|
|Right Ascension (R.A.)||06h 40m 05.58|
|Declination (Dec.)||+07° 36` 21.0|
|Galactic Latitude||0.96 degrees|
|Galactic Longitude||204.87 degrees|
|Distance from Earth||-0.28 Parallax (milliarcseconds)|
|-11648.69 Light Years|
|-736,655,183.89 Astronomical Units|
|Radial Velocity||45.30 ± 0.60 km/s|
|Variable Star Class||Pulsating|
|Variable Star Type||Delta Cepheid|
|Mean Variability Period in Days||2.706|
|Variable Magnitude Range (Brighter - Dimmer)||10.395 - 10.993|
|Effective Temperature||4,683 Kelvin|
There's no register feature and no need to give an email address if you don't need to. All messages will be reviewed before being displayed. Comments may be merged or altered slightly such as if an email address is given in the main body of the comment.
You can decline to give a name which if that is the case, the comment will be attributed to a random star. A name is preferred even if its a random made up one by yourself.