The Denouement of Blue Supergiants

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  • Thread starter Thread starter Simfish
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SUMMARY

Blue supergiants, such as Rigel and Deneb, evolve through distinct stages in the Hertzsprung-Russell (H-R) diagram, transitioning from main sequence stars to red supergiants like Betelgeuse. This evolution is characterized by a gradual increase in size and luminosity rather than a sudden transformation. The discussion clarifies that while Rigel and Deneb are currently blue supergiants, they will ultimately evolve into red supergiants, but the sun, due to its mass, will only become a red giant, not a red supergiant.

PREREQUISITES
  • Understanding of the Hertzsprung-Russell diagram
  • Knowledge of stellar evolution stages
  • Familiarity with the characteristics of blue supergiants and red supergiants
  • Basic concepts of stellar mass and its impact on life cycle
NEXT STEPS
  • Research the evolutionary pathways of blue supergiants in stellar astrophysics
  • Study the differences between red giants and red supergiants
  • Explore the life cycle of stars with varying masses, focusing on the end stages
  • Investigate the role of radiation pressure in stellar evolution
USEFUL FOR

Astronomy students, astrophysicists, and anyone interested in stellar evolution and the life cycles of massive stars.

Simfish
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Hi,

First of all, would very bright blue main sequence stars (for example, the stars in Orion's belt and Spica) first become a star like Rigel or Deneb, and then gradually move towards a star like Betelgeuse in the H-R diagram? Or will they suddenly envelope into a Betelgeuse-like star?

If yes to the first question, then my question is answered. If not, then I have another question.

What exactly were Rigel and Deneb and will they ultimately become a Betelgeuse?

Also, why do so many astronomy textbooks say that the sun will turn into a red supergiant in the last stages of its life? It's only going to have enough mass to become a red giant anyhow.

Thanks!

T_Simfish
 
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The gravitational attraction will not be enough to overcome the radiation pressure.
 

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