The suns life
Storyboard Text
- Slide: 1
- Stellar Nebula
- Fun Fact: The first mention of a true nebula can be found in the Book of Fixed Stars, written by the Persian astronomer Abd al-Rahman al-Sufi in 964.
- In the early stage of a star's life cycle, stars are formed within a nebula. Gravity causes dust particles and gases, primarily hydrogen and helium, to cluster together. As this clumping continues, gravitational forces increase, leading to a rise in temperature as the material begins to transform into a protostar.
- Slide: 2
- Protostar
- Once the core of the nebula gets hot enough, nuclear fusion will occur, and a new star is born.
- Slide: 3
- Main Sequence Star
- Fun Fact: Approximately 90% of the stars in the universe, including our sun, are main sequence stars.
- Slide: 4
- Red Giant
- Did you know? VY Canis Majoris (VY CMa) holds the title of the largest known red giant star!
- When a star runs out of hydrogen, it enters the red giant stage, expanding to many times its original size. This marks the beginning of the star's decline, as it lacks the fuel needed for continued nuclear fusion. Once the remaining hydrogen and helium are depleted, fusion ceases, and the star begins to collapse in on itself.
- Slide: 5
- Planetary Nebula
- Fun Fact: Young planetary nebulae are the densest, but as they age and expand, their density decreases.
- This stage begins when stars start to collapse under their own gravity due to the depletion of fusion energy that keeps them stable. A planetary nebula is essentially a cloud formed from the outer layers shed by a dying star.
- Slide: 6
- Once a stellar nebula transforms, it becomes a star. Main sequence stars can burn for billions of years until they exhaust their hydrogen, maintaining a balance between gravitational forces that compress the star and the heat that causes it to expand.
- White Dwarf
- Here's a fun fact: Approximately 97% of all stars in the Milky Way will eventually evolve into white dwarfs.
- A white dwarf is the core remnant of a dead star, consisting of a mixture of carbon, helium, and oxygen surrounded by energetic electrons. These electrons provide the pressure needed to support the white dwarf and prevent it from collapsing further. However, this isn’t the final stage of a star's life; a white dwarf will gradually cool over billions of years until it ultimately becomes a black dwarf.
Over 30 Million Storyboards Created
No Downloads, No Credit Card, and No Login Needed to Try!
