Why will the Sun leave the main sequence?
When the stars go out Eventually, a main sequence star burns through the hydrogen in its core, reaching the end of its life cycle. At this point, it leaves the main sequence. Stars smaller than a quarter the mass of the sun collapse directly into white dwarfs.
Why does the Sun’s radius change after it leaves the main sequence?
At some point during the collapse, the pressure and temperature will increase at the core, to the point that the helium now begins to fuse. When it does, the energy produced will cause the sun to expand, and to a much greater size than what it is currently.
Will our Sun evolve off the main sequence?
One-Solar Post-Main Sequence Evolution. Stars such as our Sun move off the main sequence and up the red giant branch (RGB), fusing hydrogen into helium in hydrogen shell burning. Once shell temperature is sufficient, helium shell burning starts and the star moves up into the asymptotic giant branch (AGB).
How the Sun will end?
In about 5 billion years, the Sun is due to turn into a red giant. The core of the star will shrink, but its outer layers will expand out to the orbit of Mars, engulfing our planet in the process.
What will be the end stage of the Sun?
The end stage of the sun will be white dwarf.
When the Sun leaves the main sequence and becomes a red giant?
And roughly 1.2 billion years after it leaves the main sequence, at the height of its glory as a red giant, the center of the helium core of the Sun will become sufficiently massive, dense, and hot that something amazing will happen: within a matter of minutes, it will ignite and burn.
What three stages will our Sun undergo after the main sequence phase?
The Sun is currently a main sequence star and will remain so for another 4-5 billion years. It will then expand and cool to become a red giant, after which it will shrink and heat up again to become a white dwarf. The white dwarf star will run out of nuclear fuel and slowly cool down over many billions of years.
How will the sun end?
After fusing helium in its core to carbon, the Sun will begin to collapse again, evolving into a compact white dwarf star after ejecting its outer atmosphere as a planetary nebula. The predicted final mass is 54.1\% of the present value, most likely consisting primarily of carbon and oxygen.