Stars, by definition, are astronomical objects consisting of luminous spheroids of plasma held together by their own gravity; they store most of the baryonic matter that forms galaxies.
There are two main physical levels that govern the dynamic behavior of stars, both at the macroscopic and microscopic levels. Curious to know more about the dynamics of stellar evolution? Keep watching!!

Check it out: Stellar Classification: Types of Stars!
https://youtu.be/ab_5MNP2OfQ
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Star formation

Stars form inside what are called molecular clouds, these are relatively dense regions of interstellar gas and dust with extremely cold temperatures in which the interstellar gas takes a molecular form, in other words , gaseous atoms bond together to form molecules and that is why these clouds are called molecular clouds. The most common molecules inside these clouds are carbon monoxide and hydrogen, and the extremely cold temperatures cause the gas molecules to form clusters of high densities, the star eventually forming when these densities reach a certain limit. The density of these regions makes them opaque to visible light and this is why they are called dark nebulae; in order to observe or study them, astronomers use infrared telescopes and radio telescopes.
The beginning of star formation occurs when the densest parts of the nebula's dark core collapse under their own gravity. The masses of these nuclei reach approximately (10 to the power of 4) the solar masses and they are mainly in the form of gas and dust. Keeping in mind that the core of the dark nebula is denser than the outer cloud itself, it is obvious that the cores collapse first. When the inner cores collapse under their own gravity, they disintegrate into clusters approximately 0.1 parsecs in diameter and (10 to 50) solar masses. Then the clusters form protostars in a process that takes about ten million years.
You may be wondering how astronomers know these facts if the star's birth takes place in the center of a dark nebula that is opaque to visible light? And the answer is simple: most dark nebula cores have infrared sources that provide evidence of the energy released by protostar collisions. Additionally, young stars are usually found surrounded by gas clouds, which are the remnants of the dark nebula.

Protostars

Once a dust clump freely decays from the dark core of the nebula, it becomes a gravitationally bound body with its unique gravity and characteristics and is called a protostar. Free gas falls into the center of the protostar as it forms, kinetic energy is released as heat by this incoming gas; causing an increase in the temperature and pressure of the center of the protostar. At some point, when the core temperature reaches thousands of degrees, the protostar becomes a source of infrared energy. With the help of the Hubble Space Telescope, several candidate protostars have been discovered in the Orion Nebula.
During the initial collapse of the dust cluster, the cluster is transparent and the time interval of collapse is relatively short. However, as the cluster adapts to its own gravity, it becomes denser and therefore more opaque to many types of radiation. One of them is infrared radiation trapped inside the dense cluster and increasing the temperature and pressure of the core. At some point, internal pressure prevents free gas from falling into the center of the core. Therefore, the protostar becomes more stable as dynamic equilibrium between internal pressure and incoming gas is achieved. The protostar represents only about 1% of the total mass of the main sequence star. However, the star's envelope continues to grow from the material which easily accumulates due to the angular momentum of the protostar causing it to change from an irregular shape to a rotating form. disk.

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Credits: Ron Miller
Credits: NASA/Shutterstock/Storyblocks/Elon Musk/SpaceX/Esa
Credits: Flickr

Video chapters:
00:00 Presentation
01:23 Star formation
03:27 Protostars
07:02 The fate of the stars

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