For most of a star's life, the main fuel is protium (hydrogen-1), which is fused into helium-4.
The main sequence of stars is called the "main sequence" itself. It is a continuous and distinctive band on the Hertzsprung-Russell diagram where stars spend most of their lifetime, fusing hydrogen into helium in their cores. Main sequence stars vary in size, temperature, and luminosity, ranging from hot, massive O-type stars to cooler, smaller M-type stars. This stage represents a significant phase in stellar evolution before stars evolve into red giants or other end states.
Spectral class O5 stars remain on the main sequence for around 3-4 million years before they evolve off the main sequence stage. These stars have extremely high luminosities and temperatures, leading to a short main sequence lifetime compared to lower mass stars.
White dwarf stars are much smaller and denser than main sequence stars, as they are the remnants of stars that have exhausted their nuclear fuel. They have no nuclear fusion reactions occurring in their cores and are supported by electron degeneracy pressure. White dwarfs are typically much cooler than main sequence stars, emitting most of their energy in the form of visible light rather than as high-energy radiation.
It depends on the mass of the star. The lower the mass, the longer it will stay on the main sequence. A red dwarf may stay on the main sequence for trillions of years, while a blue star only lasts a few million years.
Stars are formed when elevation gass escapes the sun. They will then catch heat from planets, the planets orbit will then place the stars in a special order. Then the star will glow for 10,000 years then will die.
A star's lifetime depends on its mass. More massive stars have shorter lifetimes, burning through their fuel faster, while less massive stars have longer lifetimes. Additionally, the composition of a star determines how it burns its fuel and influences its lifetime.
The primary fuel for all stars is hydrogen
The main fuel for nuclear reactions in stars is hydrogen. Through a process called nuclear fusion, hydrogen atoms combine to form helium, releasing energy in the form of light and heat. This process powers the stars and allows them to shine brightly.
No, red giants are generally older than main sequence stars, as red giants have no hydrogen left for fuel, and burn helium instead. where as Main Sequence stars burn hydrogen for fuel.
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.
The mass of the star. The bigger it is, the faster it will burn through its fuel supply.
gas, and other vibrate radiations.
an o-type blue star has a less length life than a g-type sun like star, this is because a the larger, hotter star, (the o-type blue star) uses its fuel (converting hydrogen into oxygen) quicker, so the correct answer to your question is the o-type blue star.
A star that uses hydrogen as fuel is a main sequencestar.
main sequence stars all are burning though fuel at asteadyrate in there cores. with the proton+proton chain our sun is a main sequence star
main sequence stars of which colr use up their fuel supply in the shortest period of time? and why.
Hydrogen is being "burned" into helium.