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Stars are just fascinating altogether with many facts. Stars are huge balls of Hydrogen and Helium that are formed in galaxies from great big clouds of gas and dust over billions….
The birth of a star begins when massive clouds of dust and gas start to collapse and break…. So you have learned about the birth of stars, and have also learned about our own star. Now, let us look into the life of a star and the stages…. With an infinite amount of stars in the universe, and the billions in our own galaxy, as we search through the stars that we can see with current technology, we….
Kids Fun Facts Corner 1.
Birth of stars and evolution to the main sequence
What is a Protostar? What determines the color of a star? What is the name of the force that creates the birth of a star?
- The Whole Truth (Shaw & Katie James, Book 1).
- The Formation of Stars | Wiley Online Books.
- Youngspeak in a Multilingual Perspective;
How Stars Are Born Video. Stars Stars are just fascinating altogether with many facts.
Stars | Science Mission Directorate
Stars are huge balls of Hydrogen and Helium that are formed in galaxies from great big clouds of gas and dust over billions… Read Full Article. The birth of a star begins when massive clouds of dust and gas start to collapse and break… Read Full Article. Star Lifecycle — Supernovas So you have learned about the birth of stars, and have also learned about our own star. Now, let us look into the life of a star and the stages… Read Full Article. Star Sizes With an infinite amount of stars in the universe, and the billions in our own galaxy, as we search through the stars that we can see with current technology, we… Read Full Article.
Figure 3: Orion Nebula. Megeath University of Toledo, Ohio. Compare this with our own solar neighborhood, where the typical spacing between stars is about 3 light-years. Only a small number of stars in the Orion cluster can be seen with visible light, but infrared images—which penetrate the dust better—detect the more than stars that are part of the group Figure 4.
Figure 4: Central Region of the Orion Nebula. The Orion Nebula harbors some of the youngest stars in the solar neighborhood. At the heart of the nebula is the Trapezium cluster, which includes four very bright stars that provide much of the energy that causes the nebula to glow so brightly. In these images, we see a section of the nebula in a visible light and b infrared. The four bright stars in the center of the visible-light image are the Trapezium stars. Notice that most of the stars seen in the infrared are completely hidden by dust in the visible-light image.
Schneider, E. Young, G. Rieke, A. Cotera, H.
Chen, M. Rieke, R. Thompson Steward Observatory, University of Arizona. Studies of Orion and other star-forming regions show that star formation is not a very efficient process. That is why we still see a substantial amount of gas and dust near the Trapezium stars.
The leftover material is eventually heated, either by the radiation and winds from the hot stars that form or by explosions of the most massive stars. We will see in later chapters that the most massive stars go through their lives very quickly and end by exploding. Whether gently or explosively, the material in the neighborhood of the new stars is blown away into interstellar space.
Older groups or clusters of stars can now be easily observed in visible light because they are no longer shrouded in dust and gas Figure 5. Figure 5: Westerlund 2. This young cluster of stars known as Westerlund 2 formed within the Carina star-forming region about 2 million years ago. Stellar winds and pressure produced by the radiation from the hot stars within the cluster are blowing and sculpting the surrounding gas and dust.
The nebula still contains many globules of dust.
Stars are continuing to form within the denser globules and pillars of the nebula. This Hubble Space Telescope image includes near-infrared exposures of the star cluster and visible-light observations of the surrounding nebula. Colors in the nebula are dominated by the red glow of hydrogen gas, and blue-green emissions from glowing oxygen. Although we do not know what initially caused stars to begin forming in Orion, there is good evidence that the first generation of stars triggered the formation of additional stars, which in turn led to the formation of still more stars Figure 6.
Figure 6: Propagating Star Formation. Star formation can move progressively through a molecular cloud.
The oldest group of stars lies to the left of the diagram and has expanded because of the motions of individual stars. Eventually, the stars in the group will disperse and no longer be recognizable as a cluster.
What Was It Like When Galaxies Formed The Greatest Number Of Stars?
The youngest group of stars lies to the right, next to the molecular cloud. This group of stars is only 1 to 2 million years old. The pressure of the hot, ionized gas surrounding these stars compresses the material in the nearby edge of the molecular cloud and initiates the gravitational collapse that will lead to the formation of more stars. The basic idea of triggered star formation is this: when a massive star is formed, it emits a large amount of ultraviolet radiation and ejects high-speed gas in the form of a stellar wind.
This injection of energy heats the gas around the stars and causes it to expand. When massive stars exhaust their supply of fuel, they explode, and the energy of the explosion also heats the gas. The hot gases pile into the surrounding cold molecular cloud, compressing the material in it and increasing its density. If this increase in density is large enough, gravity will overcome pressure, and stars will begin to form in the compressed gas. There are many molecular clouds that form only or mainly low-mass stars. Because low-mass stars do not have strong winds and do not die by exploding, triggered star formation cannot occur in these clouds.
There are also stars that form in relative isolation in small cores. Therefore, not all star formation is originally triggered by the death of massive stars. However, there are likely to be other possible triggers, such as spiral density waves and other processes we do not yet understand. Although regions such as Orion give us clues about how star formation begins, the subsequent stages are still shrouded in mystery and a lot of dust.
There is an enormous difference between the density of a molecular cloud core and the density of the youngest stars that can be detected. Direct observations of this collapse to higher density are nearly impossible for two reasons. First, the dust-shrouded interiors of molecular clouds where stellar births take place cannot be observed with visible light. Second, the timescale for the initial collapse—thousands of years—is very short, astronomically speaking.
The formation of stars
Since each star spends such a tiny fraction of its life in this stage, relatively few stars are going through the collapse process at any given time. Nevertheless, through a combination of theoretical calculations and the limited observations available, astronomers have pieced together a picture of what the earliest stages of stellar evolution are likely to be. The first step in the process of creating stars is the formation of dense cores within a clump of gas and dust Figure 7 a.
It is generally thought that all the material for the star comes from the core, the larger structure surrounding the forming star. Eventually, the gravitational force of the infalling gas becomes strong enough to overwhelm the pressure exerted by the cold material that forms the dense cores. The material then undergoes a rapid collapse, and the density of the core increases greatly as a result. During the time a dense core is contracting to become a true star, but before the fusion of protons to produce helium begins, we call the object a protostar. Figure 7: Formation of a Star.
These sketches are not drawn to the same scale.