According to Charles's Law, there is a direct relationship between the volume and absolute temperature of an ideal gas, assuming pressure remains constant. This law states that as temperature increases, the volume of the gas also increases proportionally, and vice versa.
A Hertzsprung-Russell diagram is a scatter graph that can be used to plot the relationship between the absolute magnitude (i.e. luminosity) of a star versus it's spectral type / classification and effective temperature. Since a black hole does not have an absolute magnitude, spectral type, or an effective temperature, it cannot be located on an H-R diagram.
The relationship between LM (limiting magnitude), TM (telescopic magnitude), and SEM (standard error of measurement) is that LM represents the faintest magnitude observable with the naked eye, TM is the maximum magnitude a telescope can observe, and SEM is a statistical measure of the precision of a measurement. There is no direct mathematical relationship between these terms as they represent different concepts in astronomy and measurement.
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.
Ejnar Hertzsprung and Henry Norris Russell,working independently, realized the relationship between a star's temperature and its brightness.Together, in 1910, they formed what is now known as the Hertzsprung--Russell diagram or HR Diagram.It's a scatter graph showing the relationship between a star's absolute magnitudes, their spectral types and temperatures.
The answer to this question is Hertzsprung-Russell diagram
You need to do this. It is homework and we don't have the graph . You teacher is looking for your critical thinking skills and not ours.
That is called the Hertzsprung-Russell or HR diagram and each star occupies a point. The horizontal axis is temperature and the vertical axis is the absolute magnitude.
The HR diagram, also known as the Hertzsprung-Russell diagram, depicts the relationship between the luminosity and temperature of stars. It shows how stars are distributed in terms of their brightness and temperature, allowing astronomers to classify stars based on these characteristics.
The Hertzsprung-Russell (HR) diagram is a graph that shows the relationship between a star's magnitude (luminosity) and temperature. It plots stars based on their color (temperature) and brightness (magnitude), allowing astronomers to classify stars and understand their evolutionary stage.
The relationship between absolute temperature and volume of an ideal gas at constant pressure.
As temperature increases the absolute brightness increases
The Hertzsprung-Russell diagram predicts the relationship between a star's luminosity (brightness) and temperature, allowing astronomers to classify stars based on their properties. It shows the correlation between a star's temperature and its absolute magnitude, helping to understand their evolutionary stage and lifecycle.
between the yellow stage color on the digram
According to Charles's Law, there is a direct relationship between the volume and absolute temperature of an ideal gas, assuming pressure remains constant. This law states that as temperature increases, the volume of the gas also increases proportionally, and vice versa.
The brightness of a star depends on its temperature, size and distance from the earth. The measure of a star's brightness is called its magnitude. Bright stars are first magnitude stars. Second magnitude stars are dimmer. The larger the magnitude number, the dimmer is the star.The magnitude of stars may be apparent or absolute.
The Hertzsprung-Russell diagram (H-R diagram) shows the relationship between absolute magnitude, luminosity, classification, and effective temperature of stars. The diagram as originally conceived displayed the spectral type (effectively the surface temperature) of stars on the horizontal axis and the absolute magnitude (their intrinsic brightness) on the vertical axis.