preallax
The apparent magnitude is what we see, and this can be measured directly. The absolute magnitude must be calculated, mainly on the basis of (1) the apparent magnitude, and (2) the star's distance. So, to calculate the absolute magnitude, you must first know the star's distance.
0 Kelvin (-273.15 C) is the temperature when all atomic motion stops. that is why it is called Absolute Zero.
Stars are measured in brilliance called magnitude. The faintest stars visible to the naked eye are mag.6. Brighter ones are mag. 1 or 2, the even brighter stars have negative magnitude. So its like a number line in math: Brighter Fainter -6_-5_-4_-3_-2_-1__0__1_2_3_4_5_6
They are measured on the Richter Scale, if you are talking about the magnitude
This is known as magnitude. It is measured on the moment magnitude scale.
Typically, negative numbers could be "measured" by the difference between the number and another number. The magnitude of a negative number is the distance from zero. Essentially, remove the minus sign, and you have the magnitude (also called absolute value) of the number.
Absolute temperature is measured from 0 in Kelvin units.
Absolute temperature IS MEASURED IN KELVIN.
-273 C
It is actually absolute magnitude, opposed to apparent magnitude which is how much light stars appear to give off.
I assume you mean the absolute magnitude (brightness) of stars. The problem with this is that it can't be directly measured. What astronomers can measure is the apparent magnitude. To make conclusions about the absolute magnitude, they would also have to know the distance to the star, as well as data about extinction, i.e., how much dust and gas there is between us and the start which may make the light look fainter. Note that the absolute magnitude is very important to characterize a star - but it may be difficult to calculate it with much precision.
Absolute zero is defined as 0 Kelvin and is equivalent to −273.15 °C
The apparent magnitude is what we see, and this can be measured directly. The absolute magnitude must be calculated, mainly on the basis of (1) the apparent magnitude, and (2) the star's distance. So, to calculate the absolute magnitude, you must first know the star's distance.
Information on millions of stars shows that there is a relationship between temperature and brightness. Surface temperature is measured in degrees C and brightness is measured in absolute magnitude (the star's brightness at a standard distance). If all the stars are plotted on a graph of temperature against absolute magnitude, called a Hertzsprung-Russell diagram, very many of them lie close to a straight line that is called the Main Sequence. There are some stars that do not lie on the Main Sequence, notably the red giants that are very bright despite having a relatively low temperature. The Sun is right in the middle of the Main Sequence showing it is an average star in the middle of its life and very stable.
Brightness of stars (apparent and absolute magnitude) is measured by convention, taking an another star as a standard.
Distances of stars and objects in space can be measured by light years. Edit: This is a big question. The problem of measuring distance in astronomy has gradually been improved over many years. If you just mean stars within our Galaxy, the nearest ones can be measured using "parallax". The stars called "Cepheid variables" are very useful for bigger distances. The periods over which their brightness varies is linked to their "absolute magnitude" ( how luminous they really are). So their "apparent magnitude" (how bright they seem) gives a good guide to their distance. Spectroscopy is very useful too, because it gives us a good idea of how bright a star really is. Again the distance can be estimated by comparing the absolute and apparent magnitudes.
Information on millions of stars shows that there is a relationship between temperature and brightness. Surface temperature is measured in degrees C and brightness is measured in absolute magnitude (the star's brightness at a standard distance). If all the stars are plotted on a graph of temperature against absolute magnitude, called a Hertzsprung-Russell diagram, very many of them lie close to a straight line that is called the Main Sequence. There are some stars that do not lie on the Main Sequence, notably the red giants that are very bright despite having a relatively low temperature. The Sun is right in the middle of the Main Sequence showing it is an average star in the middle of its life and very stable.