The stars formed
The stars start out as microscopic particles in massive clouds of dust and gas, and these nebulae stay stable and frigid for aeons away from the active stars. Then a distant element, such as a comet or a wave, passes through these nebulae, and the resulting force flows around Nebula.
The force that results from it moves throughout the nebula, stimulating the particles within it to collide and form clumps, causing each mass to gain more mass, leading to an increase in the force of attraction.
Which attracts more particles from the surrounding cloud, and as this mass expands, its centre increases as well, becoming larger and hotter, and over a million years, the mass becomes a small dense protostar, which attracts more gas and grows to become hotter.
When the protostar's core heats up enough, the thermal pressure builds up enough to slow the collapse of the components towards the centre, and the contractions become considerably slower, as the protostar's continual contraction converts gravitational potential energy to thermal energy, leading it to generate light at a pace of roughly 1000 suns.
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| The stars formed |
Keeping the angular momentum in the beginning leads the sluggish clouds to rotate much faster, resulting in a large momentum towards the centre in order to oppose the collapse of more elements towards the centre due to gravity along the midline of the initial rapidly rotating star.
The components at the poles, on the other hand, will not be influenced by the same force of resistance, so only a planetary disc will form around the parent star's centre.
The constituent elements
Because stars are made up of 99 percent gas and 1 percent dust, the Milky Way's gas is 70 percent hydrogen. Helium makes up 28% of the atmosphere. There are 2% of elements that are heavier than helium.
The death of the stars
The major fuel source of the stars, hydrogen, runs out after millions to billions of years, depending on their initial mass, and once the hydrogen supply in the centre is depleted, the nuclear processes that occur there stop, and in the absence of the external pressure generated by these events to resist the force of gravity, the stars collapse.
The star's outer layers are pushed out, and the star expands to a larger size than it has ever been before, transforming it into a red giant. What occurs next in the star's life is determined by its initial mass.
The steps following the red giant phase range greatly depending on whether the star is massive, with a mass of 5 or more times that of the sun, or low or medium mass, with a mass of 0.4 to 3.4 times that of the sun.