How Long Will a B0 Star Last on the Main Sequence?

In summary, the question asks if we can estimate the main sequence lifetime of a B0 star based on its luminosity and mass. The equation L~M^3 is relevant for main sequence stars. To solve this, we need to calculate the fraction of fuel the star needs to burn each year to maintain its luminosity and use the equation E=m*c^2 and the luminosity of the sun.
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Homework Statement



A B0 star has a luminosity of ~ 16000 L(solar) and a mass of ~ 16 M(solar). Can you estimate the time on the main sequence for this star simply from considering the rest mass energy of the core of the star (~10% of the total, and fusion burns with an efficiency of about 0.7%) and its luminosity?

Homework Equations



I know that for main sequence stars, L is proportional to M^3

The Attempt at a Solution



I have no idea where to go with this question, I've trawled through so many webpages and textbooks without success. Any ideas?
 
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  • #2
You will need to figure out what fraction of the available fuel the star would need to burn every year to maintain its luminosity. This will let you project when it will run out. You shouldn't need to know much more than E=m*c^2 and the luminosity of the sun.
 

What is "Star time on main sequence"?

Star time on main sequence refers to the amount of time a star spends on the main sequence, which is the longest stage in its life cycle. This is when a star fuses hydrogen into helium in its core, providing the energy that allows it to shine.

How long does a star stay on the main sequence?

The length of time a star stays on the main sequence varies depending on its mass. Smaller, cooler stars can remain on the main sequence for trillions of years, while larger, hotter stars may only stay on the main sequence for a few million years.

What happens to a star after it leaves the main sequence?

After a star exhausts its supply of hydrogen fuel on the main sequence, it will begin to expand and cool, becoming a red giant. Eventually, it will shed its outer layers and form a planetary nebula, leaving behind a small, dense remnant known as a white dwarf.

Can stars return to the main sequence?

No, once a star leaves the main sequence, it cannot return to it. The fusion of hydrogen into helium in the core of a star is what defines the main sequence stage, and once this process stops, the star will continue to evolve and eventually die.

How do scientists measure the age of a star on the main sequence?

Scientists can estimate the age of a star on the main sequence by measuring its mass, luminosity, and temperature. By comparing these measurements to theoretical models of stellar evolution, scientists can determine how long a star has been on the main sequence and how much longer it is expected to stay there.

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