The life of the sun as a star (Hero-Russell diagram)
Aerospace · Interactive
- DimensionsSubject to on-site plan
- PresentationInteractive
- PricingQuoted by manufacture spec
Purpose & Scientific Principle
By selecting stars of different masses and watching their different final destinations, we can understand the formation and evolution process of celestial bodies in the universe, and understand the splendid lives of stars of different masses.
How to Operate
(1) Birth: In the vast space, there are many extremely huge "clouds", which are composed of very thin gas and dust, the main component of which is the simplest chemical element-hydrogen. After that, the gas and dust in the nebula continued to gather together, driven by their own gravity. As a result, the cloud volume becomes smaller and smaller, the density becomes larger and larger, and the temperature continues to rise. When the temperature in the center of the cloud exceeds 7 million Kelvin, a reaction will occur where every four hydrogen nuclei will fuse into one helium nucleus, which is the so-called "thermonuclear fusion". At the same time, huge energy will be released, and a new star will be born.
(2) Burning of stars of different masses: For stars in the main sequence stage, their own gravity and the radiation pressure from the inside to the outside are evenly matched, so the stars neither shrink nor expand, are in a state of equilibrium, and their brightness remains basically unchanged. In addition, the time that stars of different masses are in the main sequence stage is also different from each other: extremely massive stars are like extremely large nuclear combustion furnaces. The thermonuclear fusion reaction inside is very violent, and the nuclear fuel is consumed very quickly and is burned out quickly. Therefore, such stars quickly enter the decline stage; on the contrary, the thermonuclear fusion inside small-mass stars proceeds relatively gently, and the nuclear fuel is consumed very slowly, so the decline time of such stars will be longer.
(3) Fate: Stars of different masses will have different fates when they enter the decay period.
①Stars with 0.6~2 times the solar mass will become red giants, then red giants with 0.6~1.44 times the solar mass will collapse into white dwarfs, and red giants with 1.44~2 times the solar mass will collapse into neutron stars.
②Stars with a mass greater than 2 times the sun will become supergiants. After reaching a certain critical point, they will explode as supernovae. The collapse of the explosion center will have different fates. 2~8 times the solar mass will collapse into a white dwarf, 8~25 times the solar mass will collapse into a neutron star, and more than 25 times the solar mass will collapse into a black hole.
What happens if a star dies? The exhibit focuses on showing the four final directions of stars of different masses after their death.
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