What are the steps of evolution of star and sun like star? What's difference
Since the sun is a star, no difference
Since this is not my area of expertise, I searched Google under the key words "evolution of a star" to get these possible sources:
https://www.google.com/search?client=safari&rls=en&q=evolution+of+a+star&ie=UTF-8&oe=UTF-8
In the future, you can find the information you desire more quickly, if you use appropriate key words to do your own search. Also see http://hanlib.sou.edu/searchtools/.
http://www.hackcollege.com/blog/2011/11/23/infographic-get-more-out-of-google.html
Don't just copy the material. Express the ideas in your own words. Although this will take more time and effort, you will learn more.
The steps of stellar evolution are generally the same for stars of various sizes, including our Sun. However, the specifics and duration of each step can vary depending on the mass of the star. Here are the generalized steps of stellar evolution for a star like our Sun:
1. Nebula: A stellar nursery begins with the gravitational collapse of a dense cloud of gas and dust called a nebula. This collapse sets the stage for the birth of a star.
2. Protostar: The nebula continues to collapse under its own gravity, forming a protostar. In this stage, the protostar is not yet undergoing nuclear fusion but is getting hotter and denser.
3. Main Sequence: The protostar eventually reaches a critical temperature (~10 million degrees Celsius) and pressure, which triggers the process of nuclear fusion. At this point, the star becomes a main sequence star, where hydrogen nuclei fuse to form helium in its core. This fusion releases an enormous amount of energy, which counteracts the force of gravity and keeps the star stable.
4. Red Giant: As the star ages and consumes its hydrogen fuel, the nuclear fusion reactions slow down, causing the core to contract and the outer layers to expand. The star's outer shell becomes less dense, and it swells to form a red giant. During this phase, the star fuses helium into heavier elements in its core.
5. Planetary Nebula: Eventually, the red giant expels its outer layers, creating a glowing shell of gas and dust called a planetary nebula. The star sheds most of its mass, exposing its core.
6. White Dwarf: After the planetary nebula phase, the remaining core collapses inward due to gravity. If the core mass is less than about 1.4 times the mass of the Sun (known as the Chandrasekhar limit), it forms a white dwarf. White dwarfs are extremely dense and hot but no longer undergo nuclear fusion. They slowly cool down over billions of years.
While most stars follow these general steps, stars with higher masses can undergo different phases, such as becoming a red supergiant or even exploding in a supernova.
In summary, the main difference between the evolution of our Sun (a star of intermediate size) and more massive stars lies in their final stages. Our Sun is expected to end its life as a white dwarf, while more massive stars can end up as neutron stars or black holes after a supernova explosion.