Nuclear Fusion in a Giant Star involves Helium being fused into a hydrogen shell that surrounds the core, and Nuclear Fusion in a Main-Sequence star involves Hydrogen being fused into Helium to produce Energy inside of the core.
It is a fact that while a star plots on the main sequence line of the Hertzsprung-Russelldiagram, it is fusing the element HYDROGEN into the element helium to produce its energy output. The actual size of the star does not matter, the bigger stars just produce more energy than the smaller ones but they all sit on the main sequence line (just at opposite ends of it).
Once the star runs out of hydrogen in its core, the core shrinks further under gravity and gets hotter and denser and it reaches a point that causes the helium that it made earlier to fuse into heavier elements. This HELIUM fusion produces even more energy and the plot of the energy output profile is now no longer on the main sequence line. The extra energy makes the outer layers of the star inflate and the star enters it "giant" phase.
The larger the star, the less time it spends on the main sequence line because the larger it is the faster it fuses its hydrogen.
Fusion is much faster in giant stars causing them to burn out faster.
(study island answer= all of these statements are true) Stars with masses less than 1.6 × 1029 kg become brown dwarfs because they are unable to reach high enough temperatures for hydrogen fusion to take place. Extremely massive stars are able to produce supernovas, or stellar explosions, when they cease to undergo nuclear fusion or when they undergo a sudden gravitational collapse. Low-mass stars develop more slowly than more massive stars; their lifetimes can last trillions of years as opposed to only a few million years.
High-mass stars
Higher mass stars "burn" faster due to the increased pressure in the core.
High-mass stars might become black holes, if the remaining matter (after the supernova explosion) is sufficiently large.
The defining characteristic of a star is that it is large enough, hot enough, and has enough pressure, to sustain nuclear fusion. In general, stars are typically larger, more massive, hotter, and have greater pressure in their cores, than planets. As a result of their nuclear fusion, their surface temperature is typically at least a few thousand kelvin, and they are quite bright.
Nuclear Fusion
Initially it is hydrogen. When that is spent, stars move to fusion of helium. There are also other fusion processes which take place: which process depends on the stars' mass.
Initially it is hydrogen. When that is spent, stars move to fusion of helium. There are also other fusion processes which take place: which process depends on the stars' mass.
(study island answer= all of these statements are true) Stars with masses less than 1.6 × 1029 kg become brown dwarfs because they are unable to reach high enough temperatures for hydrogen fusion to take place. Extremely massive stars are able to produce supernovas, or stellar explosions, when they cease to undergo nuclear fusion or when they undergo a sudden gravitational collapse. Low-mass stars develop more slowly than more massive stars; their lifetimes can last trillions of years as opposed to only a few million years.
They produce light.
The fusion of atoms powers the sun and other stars
This is fusion not fission. In stars like our sun, hydrogen is turned into helium
High-mass stars
Fusion in stars are usually the result of gravity.Once a mass of hydrogen accumulates enough mass, the gravity of all that mass compresses the core of the star to the point that the hydrogen atoms there begin fusing into helium. The process then cascades outward, and the end result is a star.
There are three types of stellar remnants. Low to medium mass stars will become white dwarfs. High mass stars will become neutron stars. Very high mass stars will become black holes.
Main Sequence Stars
In a newly formed star cluster stars with low masses must greaty out number stars with high masses. High mass stars are rare and low mass stars are extremely common.