Accretion Disk Density & Fusion: What You Need to Know

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SUMMARY

An accretion disk can achieve sufficient density to initiate fusion, requiring approximately 100 Jupiter masses to trigger hydrogen fusion, which is the threshold for forming a brown dwarf star. However, an accretion disk does not stabilize into a disk-shaped star and will instead burn rapidly, leading to a nova event. Additionally, if the mass of the accretion disk causes a white dwarf to exceed the Chandrasekhar limit, carbon fusion occurs, resulting in a Type 1A supernova.

PREREQUISITES
  • Understanding of accretion disk dynamics
  • Knowledge of fusion processes in astrophysics
  • Familiarity with the Chandrasekhar limit
  • Concept of brown dwarf stars
NEXT STEPS
  • Research the conditions for hydrogen fusion in astrophysical objects
  • Study the characteristics and lifecycle of brown dwarf stars
  • Explore the mechanisms behind nova events
  • Investigate the physics of Type 1A supernovae and their implications
USEFUL FOR

Astronomers, astrophysics students, and anyone interested in stellar formation and the lifecycle of celestial bodies.

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Can an accretion disk get dense enough to start fusion? How dense does something have to be in order to start fusion?

Does it depend on the material?

is there a way of measuring the density of accretion disks?
 
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It takes about 100 Jupiter masses to trigger hydrogen fusion. This is the lower limit for a brown dwarf star. Small is not bad, though, such a star can burn steadily for 100 billion years.
 
Yes, but the accretion disk will not form a disk-shaped star- it will fail to reach a stable equilibrium, like stars do, and instead just burn off super fast. This event is known as a nova.

If the accretion disk gets massive enough that a white dwarf passes the Chandrasekhar limit, carbon fusion occurs and the event is known as a Type 1A supernova.
 

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