File:The life of Sun-like stars.jpg
Summary
Born from clouds of <a href="//commons.wikimedia.org/wiki/Category:Gases" title="Category:Gases">gas</a> and <a href="//commons.wikimedia.org/wiki/Category:Dust" title="Category:Dust">dust</a>, stars like our <a href="//commons.wikimedia.org/wiki/Sun" title="Sun">Sun</a> spend most of their lifetime slowly burning their primary nuclear fuel, <a href="//commons.wikimedia.org/wiki/Hydrogen" title="Hydrogen">hydrogen</a>, into the heavier element <a href="//commons.wikimedia.org/wiki/Helium" title="Helium">helium</a>. After leading this bright and shiny life for several billion years, their fuel is almost exhausted and they start swelling, pushing the outer layers away from what has turned into a small and very hot core. These “middle-aged” stars become enormous, hence cool and red — <a href="//commons.wikimedia.org/wiki/Category:Red_giants" title="Category:Red giants">red giants</a>. All red giants exhibit a slow oscillation in brightness due their rhythmic “breathing” in and out, and one third of them are also affected by additional, slower and mysterious changes in their luminosity. After this rapid and tumultuous phase of their later life, these stars do not end in dramatic explosions, but die peacefully as <a href="//commons.wikimedia.org/wiki/Category:Planetary_nebulae" title="Category:Planetary nebulae">planetary nebulae</a>, blowing out everything but a tiny remnant, known as <a href="//commons.wikimedia.org/wiki/Category:White_dwarfs" title="Category:White dwarfs">white dwarf</a>.
Licensing
Lua error in package.lua at line 80: module 'strict' not found.
File history
Click on a date/time to view the file as it appeared at that time.
| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 17:46, 14 January 2017 | | 6,500 × 4,592 (7.96 MB) | 127.0.0.1 (talk) | Born from clouds of <a href="//commons.wikimedia.org/wiki/Category:Gases" title="Category:Gases">gas</a> and <a href="//commons.wikimedia.org/wiki/Category:Dust" title="Category:Dust">dust</a>, stars like our <a href="//commons.wikimedia.org/wiki/Sun" title="Sun">Sun</a> spend most of their lifetime slowly burning their primary nuclear fuel, <a href="//commons.wikimedia.org/wiki/Hydrogen" title="Hydrogen">hydrogen</a>, into the heavier element <a href="//commons.wikimedia.org/wiki/Helium" title="Helium">helium</a>. After leading this bright and shiny life for several billion years, their fuel is almost exhausted and they start swelling, pushing the outer layers away from what has turned into a small and very hot core. These “middle-aged” stars become enormous, hence cool and red — <a href="//commons.wikimedia.org/wiki/Category:Red_giants" title="Category:Red giants">red giants</a>. All red giants exhibit a slow oscillation in brightness due their rhythmic “breathing” in and out, and one third of them are also affected by additional, slower and mysterious changes in their luminosity. After this rapid and tumultuous phase of their later life, these stars do not end in dramatic explosions, but die peacefully as <a href="//commons.wikimedia.org/wiki/Category:Planetary_nebulae" title="Category:Planetary nebulae">planetary nebulae</a>, blowing out everything but a tiny remnant, known as <a href="//commons.wikimedia.org/wiki/Category:White_dwarfs" title="Category:White dwarfs">white dwarf</a>. |
- You cannot overwrite this file.
File usage
The following page links to this file:
