Hey! We 've verified this expert answer for you, click below to unlock the details :)
At vero eos et accusamus et iusto odio dignissimos ducimus qui blanditiis praesentium voluptatum deleniti atque corrupti quos dolores et quas molestias excepturi sint occaecati cupiditate non provident, similique sunt in culpa qui officia deserunt mollitia animi, id est laborum et dolorum fuga.
Et harum quidem rerum facilis est et expedita distinctio. Nam libero tempore, cum soluta nobis est eligendi optio cumque nihil impedit quo minus id quod maxime placeat facere possimus, omnis voluptas assumenda est, omnis dolor repellendus.
Itaque earum rerum hic tenetur a sapiente delectus, ut aut reiciendis voluptatibus maiores alias consequatur aut perferendis doloribus asperiores repellat.
I got my questions answered at brainly.com in under 10 minutes. Go to brainly.com now for free help!
Explain the steps of the life cycle of a star. Beginning with a nebula and ending with old age/death of a star, explain each step in a star’s life cycle.
The life cycle of a star can follow a few different paths depending on the mass it starts out with. Really massive stars may live for only a few million years before going supernova, while low mass stars such as the Sun may take billions of years to use up their fuel and then die relatively quietly.
In star life cycles, a high mass star means a star with at least about 8 times the mass of our Sun
All stars are formed when a giant cloud of gas and dust, called a molecular cloud or nebula, begins to collapse under the influence of its own gravity
This may be triggered by a collision with another molecular cloud, the shockwave from a nearby supernova, or even the collision of galaxies
As the cloud contracts, it breaks apart. An individual fragment will condense into a hot, dense sphere known as a protostar
A new star is born when the protostar becomes hot enough to begin fusing hydrogen into helium. Now, the star will enter the main sequence, or adult, phase
If a star is too low in mass to initiate nuclear fusion it will become a brown dwarf
A star will remain in this state for most of its lifetime, fusing hydrogen to make helium and releasing energy in the process
A star may fall on different points on the main sequence depending on its mass. In general, the more massive the star the shorter its lifespan on the main sequence
Red dwarfs are small, dim stars that fuse hydrogen at a slow rate, and may remain on the main sequence for hundreds of billions of years.
Low mass stars such as our Sun will be on the main sequence for several billion years
High mass stars may only stay on the main sequence for a few million years
Eventually a star will run out of its hydrogen fuel, and begin fusing helium and other elements instead. At that point it will leave the main sequence phase
Red dwarf stars will use up all their hydrogen and collapse directly into white dwarfs
Low mass stars like our Sun will expand and become red giants.
This happens when a star runs out of hydrogen at its core. The core will collapse and begin fusing helium while hydrogen fusion is transferred to the outer layers
This causes the star to swell to many times its original size and become cooler as the heat is distributed over a larger area
More massive stars will grow into supergiants, which are among the largest stars in the Universe
In this stage a star will maintain hydrostatic equilibrium by fusing heavier and heavier elements as the lighter ones run out. The largest stars can produce elements up to iron
Death and stellar remnants
Low mass stars like our Sun will eventually die by shedding their outer layers as a planetary nebula
The core will collapse into a white dwarf, which will eventually cool into a black dwarf
More massive stars will die in a tremendous explosion called a supernova
This happens when a massive stars begins to fuse iron. This absorbs energy and caused the core to violently collapse while the outer layers are ejected
The extreme heat produced by supernovae is responsible for the nucleosynthesis of elements heavier than iron, up to uranium
After a supernova, the core may compress into a neutron star or a black hole.
Neutron stars are much denser than white dwarfs, to the point where protons and electrons combine to form neutrons (hence the name)
Black holes are denser still, so much so that they produce an extremely strong gravitational force that even light cannot escape.