Life Cycle
Life Cycle 

Stars are shaped 


in billows of gas and residue, known as nebulae. Atomic responses at the inside (or center) of stars gives enough vitality to make them sparkle brilliantly for a long time. The careful lifetime of a star depends especially on its size. Extremely huge, gigantic stars consume their fuel a lot quicker than littler stars and may just last a couple of hundred thousand years. Littler stars, notwithstanding, will keep going for a few billion years, since they consume their fuel substantially more gradually.

Life Cycle of a Star
Life Cycle of a Star 
In the end, be that as it may, the hydrogen fuel that controls the atomic responses inside stars will start to run out, and they will enter the last periods of their lifetime. After some time, they will extend, cool and change shading to wind up red goliaths. The way they pursue past that relies upon the mass of the star.
Little stars, similar to the Sun, will experience a generally serene and delightful demise that sees them go through a planetary cloud stage to end up a white diminutive person, this in the long run chills off after some time leaving a dark-colored midget. Monstrous stars, then again, will encounter a most vigorous and vicious end, which will see their remaining parts dissipated about the universe in a colossal blast, called a supernova. When the residue clears, the main thing remaining will be a thick star known as a neutron star, these can frequently be quickly turning and are known as pulsars. In the event that the star which detonates is particularly huge, it can even shape a dark gap

Black Hole

In the end, in any case, the hydrogen fuel that controls the atomic responses inside stars will start to run out, and they will enter the last periods of their lifetime. After some time, they will grow, cool and change shading to wind up red monsters. The way they pursue past that relies upon the mass of the star.
Black Hole
 Black Hole 
Little stars, similar to the Sun, will experience a generally quiet and excellent demise that sees them go through a planetary cloud stage to wind up a white smaller person, this in the long run chills off after some time leaving a dark colored diminutive person. Monstrous stars, then again, will encounter a most vivacious and savage end, which will see their remaining parts dissipated about the universe in a huge blast, called a supernova. When the residue clears, the main thing remaining will be a thick star known as a neutron star, these can frequently be quickly turning and are known as pulsars. In the event that the star which detonates is particularly substantial, it can even shape a dark gap
Dark gaps can likewise twist the picture of worlds they go before. The gravity of the dark gap will twist the light we get from the far off universe despite the fact that it is excessively far away for it to suck any material into the dark gap. They calls this gravitational leasing (see the recreation on the right).
 Black Hole
Black Hole 
When set up, dark gaps can develop by devouring material, stars and even other dark gaps around them. After some time, super-enormous dark openings can create, and it is felt that these hide at the focal point of cosmic systems.


Red Giant Stars

Facts, Definition & the Future of the Sun
A red giant star is a dying star in the last stages of stellar evolution. In only a few billion years, our own sun will turn into a red giant star, expand and engulf the inner planets, possibly even Earth. What does the future hold for the light of our solar system and others like it?
Forming a giant
Most of the stars in the universe are main sequence stars — those converting hydrogen into helium via nuclear fusion. A main sequence star may have a mass between a third to eight times that of the sun and eventually burn through the hydrogen in its core. Over its life, the outward pressure of fusion has balanced against the inward pressure of gravity. Once the fusion stops, gravity takes the lead and compresses the star smaller and tighter.
Temperatures increase with the contraction, eventually reaching levels where helium is able to fuse into carbon. Depending on the mass of the star, the helium burning might be gradual or might begin with an explosive flash.
Red Giant Stars
Red Giant Stars
Although fusion is no longer taking place in the core, the rise in temperature heats up the shell of hydrogen surrounding the core until it is hot enough to start hydrogen fusion, producing more energy than when it was a main sequence star," the Australia Telescope National Facility says on their website.
Red giant stars reach sizes of 100 million to 1 billion kilometers in diameter (62 million to 621 million miles), 100 to 1,000 times the size of the sun today. Because it spread the energy across a larger area, surface temperatures are actually cooler, reaching only 2,200 to 3,200 degrees Celsius (4,000 to 5,800 degrees Fahrenheit), a little over half as hot as the sun. This temperature change causes stars to shine in the redder part of the spectrum, leading to the name red giant, though they are often more orangish in appearance.
In 2017, an international team of astronomers identified the surface of the red giant π Gruis in detail using the European Southern Observatory's Very Large Telescope. They found that the red giant's surface has just a few convective cells, or granules, that are each about 75 million miles (120 million kilometers) across. By comparison, the sun has about two million convective cells about 930 miles (1,500 km) across.
red moon
red moon
Stars spend approximately a few thousand to 1 billion years as a red giant. Eventually, the helium in the core runs out and fusion stops. The star shrinks again until a new helium shell reaches the core. When the helium ignites, the outer layers of the star are blown off in huge clouds of gas and dust known as planetary nebulae. These shells are much larger and fainter than their parent stars.
The core continues to collapse in on itself. Smaller stars such as the sun end their lives as compact white dwarfs. The material of larger, more massive stars fall inward until the star eventually becomes a supernova, blowing off gas and dust in a dramatic, fiery death.
high-mass star
 high-mass star
 high-mass star

High-mass stars

 experience a comparative procedure to low-mass stars in the first place, then again everything happens a lot quicker. They have a hydrogen combination center, however a significant part of the hydrogen combination happens with the CNO cycle. After it depletes the hydrogen, similar to low-mass stars, a helium center with a hydrogen shell shapes, at that point a carbon center, with helium and hydrogen shells. At that point not at all like low-mass stars, they have an enough mass that gravity gets the center raising the temperature and carbon can intertwine into neon, at that point neon into oxygen, at that point oxygen into silicon, at that point iron. Each phase of consuming keeps going a shorter time than the past one. For instance, in a 25 sun based mass star, hydrogen consuming would take around 7 × 106 years, helium consuming 7 × 105 years, carbon consuming, 600 years, neon consuming 1 year, oxygen consuming a half year and silicon consuming one day.
high-mass star
 high-mass star