![]() But due to the lack of gravity, low-mass stars are unable to heat up their central region, and carbon and oxygen cannot continue thermonuclear “burning”. ![]() After burning out the helium, the super-dense core turns into a white dwarf, and the outer shell expands and is dispersed into space. This stage passes ten times faster than the hydrogen burning stage and takes about 10% of the entire active life time of the star. In this case, the shell inflates so much that a red giant is born as a result. In small objects like our Sun, the core heats up to a temperature of about 100 million degrees Celsius, after which the helium begins to turn into carbon and oxygen. When the hydrogen inside the star runs out, it moves to the next stage, where its further fate depends only on the mass. While the hydrogen is burning, the star is in the main stage of its life, which encompasses about 90% of its existence. Then the reaction of converting hydrogen into helium begins. At the first stage of development, when it is formed from a gas cloud, the temperature in the stellar core rises to several million degrees. Today, science knows that the life span of any star is determined by its mass. But there are still no clear answers to the main questions that were pondered by ancient philosophers: how is our world organized and who are we in it? Looking into the sky, we try to solve the great mysteries of the universe - just like primitive people did. ![]() Scientific progress has made possible what 100 years ago seemed like an unrealistic dream, a fantasy. Humanity has already crossed the threshold of the third millennium. ![]()
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