What is absolute size?
Absolute size is an astronomical term that refers to the true level of the brightness of the object in space, not what can be seen as its brightness that can be changed by the distance of the object, gravitational effects and the stellar material that the light must go through to achieve the observer. Despite this clear definition, this term is relative. As an absolute JAB, the size of the building must be further divided by defining the spectrum of measured electromagnetic radiation. If it performs observations based on the overall energy performance of the star object, the term bolometer size, named after Samuel Langley, which invented the bolometer in 1878 to measure electromagnetic radiation. The distance of luminosity must then be determined in the parsecs, which is the actual distance tamin, if it is in the galaxy of the Milky Way. It must also be taken into account by a redshift or the effect of gravity on the light for distant objects, the light moving towards the red end of the spectrum when the object movesBel is from the ground. Finally, with objects above our local galaxy, general calculations of relativity to determine absolute size must be used.
Another process used in determining absolute size is the calculation of the absolute temperature of the object size, and the colors of the light are produced by an object divided into a chemical signature that indicate for photons emitted from different elements. The stars classification system has an absolute size temperature that extends from "O" for the hottest with blue to "M" as the coldest with red. The stars of the class are considered the most precious in space, include only about 0.003% of the tcel, with the stars of the red M-three, which represent the bulk to 76.45% of the total. The hottest burning blue stars of the class o are also the smallest and have the shortest lifetime and eventually humiliate the red giants, with stars one quarter size of the sun degradingo to the white dwarf phase.
The process of determining and classification of objects in space can be traced back to the Greek astronomer of the hipparchus, which invented the first size system in 150 B.C.E. At that time, there were only six classifications for brightness based on what one could see with the naked eye. Today, the absolute size is a much more refined process, and adapting to the original process provides negative values such as our Sun, with -26.74 is its apparent size. Larger negative numbers on the scale indicate bright, nearby objects, while the star Sirius receives -1.4 apparent size as one of the closest stars on Earth, the planet Venus and -4.4 and the ground to -12.6.