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Main sequence stars of low mass spend a lot more time on the main sequence than do more massive stars. Less massive stars are also much less luminous than high mass stars.
Using the empirical mass-luminosity relation we can show this to be true.
L/Lsun~M/Msun3.5
Where L is luminosity and M is the mass of the star.
Consider a very low mass of M=0.1
Using this relation we get L =0.000316, a tiny fraction of the sun's luminosity!
Then we take a more massive star, say M=10
We get L = 3162 times more luminous than the sun!
The amount of material available (mass) and the rate of energy release (luminosity) can also be used to determine how long a star will remain stable on the main sequence with the equation:
MS Lifetime = M/Msun / L/Lsun x 1010 Years
We'll use the same two examples from above, M=0.1 and M=10
Low Mass Star = 0.1 / .000316 x 1010 years = 3.16x1012 years
High Mass Star = 10 / 3162 x 1010 years = 31.6 x 106 years
As we can plainly see, a high mass star shines much brighter than a low mass star, and stays on the main sequence a much shorter time. This implies that the higher the mass of the star, the faster it goes through its fuel. There are many factors contributing to this, including gravitational collapse and heating, increased surface area for energy output (since high mass stars are bigger than low mass stars), and fusion of materials in the core. Please note that internal fusion IS NOT responsible for luminosity--it IS responsible, however, for how long a star can remain on the main sequence.
A star has a much higher internal temperature than the temperature of its outer shell. Generally, the core of a star can be in the millions of degrees Kelvin, where the Effective Temperature (Teff) at the surface of the star is generally in the thousands to tens of thousands of degrees K.
For the sake of the question you asked, I'm going to assume you were referring to Teff, since it is related directly to the 'color' of the star.
As a generalization, we can think of stars as perfect radiators, or blackbodies. Practically this means that the hotter a star is, the more blue it appears, and the cooler a star is, the redder it appears. As you may have already guessed, the more massive stars are generally 'blue,' and the lower mass stars are generally 'red,' with yellow and white stars in between.
From Wikipedia:
Stellar
ClassRadiusMassLuminosityTemperatureExamples[24]R/R☉M/M☉L/L☉KO51840500,00038,000Zeta PuppisB07.41820,00030,000Phi1 OrionisB53.86.580016,400Pi Andromedae AA02.53.28010,800Alpha Coronae Borealis AA51.72.1208,620Beta PictorisF01.41.767,240Gamma VirginisF51.21.292.56,540Eta ArietisG01.051.101.266,000Beta Comae BerenicesG21.001.001.005,920Sun[note 2]G50.930.930.795,610Alpha MensaeK00.850.780.405,15070 Ophiuchi AK50.740.690.164,64061 Cygni A[25]M00.630.470.0633,920Gliese 185[26]M50.320.210.00793,120EZ Aquarii AM80.130.100.0008-Van Biesbroeck's star[27]
The Stellar Classes on this chart indicate several things about the star, including its brightness, color, and spectrum. O type stars are the biggest and hottest, and the most Blue. B are usually considered blue-white, A considered white, F called yellow-white, G are yellow (our sun is a G2 star), K are orange, and M are red.
What else can I help you with?
How do the stars luminosity compare with their radius?
A star's luminosity is related to its radius and temperature through the Stefan-Boltzmann law, which states that luminosity (L) is proportional to the square of the radius (R) multiplied by the fourth power of its surface temperature (T): (L \propto R^2 T^4). This means that for two stars of the same temperature, a larger radius results in significantly greater luminosity. Conversely, for stars of similar size, a higher temperature will lead to increased luminosity. Thus, both radius and temperature are crucial in determining a star's luminosity.
How do stars luminosity compare with their radius?
A star's luminosity is directly related to its radius and temperature, as described by the Stefan-Boltzmann law. Specifically, luminosity increases with the fourth power of the star's temperature and the square of its radius. Therefore, larger stars with higher temperatures emit significantly more light than smaller, cooler stars. This relationship helps astronomers classify stars and understand their life cycles.
What does the hr diagram compare?
The HR diagram compares the luminosity (brightness) of stars against their surface temperature or spectral type. This plot helps astronomers classify stars based on their intrinsic characteristics and evolutionary stages.
How is Jupiter temperature compare to earth temperature?
jupiter's temperature is way colder than earth.
How does the temperature of earth crust compare to the temperature of the earth interior?
it depends on the deepth
What does the Hertzsprung-Russell compare?
They compare surface temperature (horizontal axis) and luminosity (vertical axis).
How does the temperature and luminosity of the sun compare to that of the other stars on the main sequence?
The Sun, classified as a G-type main-sequence star (G dwarf), has a surface temperature of about 5,500 degrees Celsius and a luminosity of 1 solar unit. Compared to other main-sequence stars, the Sun is relatively average; hotter stars, like O and B types, exhibit much higher temperatures and luminosities, while cooler stars, such as K and M types, have lower temperatures and luminosities. Overall, the main sequence shows a correlation where higher temperatures correspond to greater luminosity, with the Sun positioned in the middle of this range.
How do the stars luminosity compare with their radius?
A star's luminosity is related to its radius and temperature through the Stefan-Boltzmann law, which states that luminosity (L) is proportional to the square of the radius (R) multiplied by the fourth power of its surface temperature (T): (L \propto R^2 T^4). This means that for two stars of the same temperature, a larger radius results in significantly greater luminosity. Conversely, for stars of similar size, a higher temperature will lead to increased luminosity. Thus, both radius and temperature are crucial in determining a star's luminosity.
What does an H-R diagram compare?
An H-R diagram compares the luminosity (brightness) of stars with their surface temperature. It helps classify stars based on their temperature and luminosity, allowing astronomers to study their characteristics and evolution.
How do you determine a stars luminosity?
To determine a star's luminosity, one can measure its apparent brightness as seen from Earth and correct for distance. Using this information along with the star's surface temperature, one can apply the Stefan-Boltzmann law to calculate the star's luminosity. This process allows astronomers to compare the intrinsic brightness of stars regardless of their distance from Earth.
How do stars luminosity compare with their radius?
A star's luminosity is directly related to its radius and temperature, as described by the Stefan-Boltzmann law. Specifically, luminosity increases with the fourth power of the star's temperature and the square of its radius. Therefore, larger stars with higher temperatures emit significantly more light than smaller, cooler stars. This relationship helps astronomers classify stars and understand their life cycles.
How does an H R diagram compare stars?
An H-R (Hertzsprung-Russell) diagram compares stars based on their luminosity (brightness) and temperature (color). The horizontal axis typically represents temperature, decreasing from left to right, while the vertical axis represents luminosity, increasing from bottom to top. This diagram reveals patterns in stellar evolution, categorizing stars into groups such as main sequence, giants, and white dwarfs, and helps astronomers understand the relationships between a star's mass, age, and evolutionary stage.
Does smaller mass stars have a greater luminosity than larger mass stars?
This is not necessarily true. most of the time stars with a larger diameter have more mass but some stars with a smaller diameter are more dense and have a greater mass. Find a main sequence star chart and you can compare the data.
What if the star has a bigger surface area but a smaller temperature how would that affect the luminosity?
As temperature decreases, luminosity will also decrease As radius increases (and with it surface area, but radius is a much easier to work with if you're trying to compare stars so we usually say radius) luminosity will also increase. If both are happening at the same time, it is possible that the luminosity of the star will remain more or less constant. Often one change will dominate the other, such as when a star goes through the red giant phase when the increase in radius has a far greater effect than the drop in temperature, and the star becomes more luminous.
What is luminosity related to?
Luminosity is related to the total amount of energy emitted by a star, galaxy, or other astronomical object per unit time, typically measured in watts. It is an intrinsic property that reflects the object's brightness and is influenced by factors such as temperature, size, and composition. In astrophysics, luminosity is crucial for understanding the life cycle of stars and their distance from Earth. It is often compared to the Sun's luminosity, allowing astronomers to categorize and compare different celestial bodies.
How does the main-sequence lifetime of a star compare to its entire fusion lifetime?
The main-sequence lifetime is a phase in a star's life when it fuses hydrogen into helium in its core. This phase typically lasts about 90% of a star's total fusion lifetime. After the main sequence, a star may continue to fuse other elements, depending on its mass, which will determine the total duration of its fusion lifetime.
What does the hr diagram compare?
The HR diagram compares the luminosity (brightness) of stars against their surface temperature or spectral type. This plot helps astronomers classify stars based on their intrinsic characteristics and evolutionary stages.
