Stellar Evolution
Learning Objectives
- Students will be able to describe the life cycle of stars from birth to death
- Students will be able to explain the different end states: white dwarf, neutron star, black hole
- Students will be able to understand supernova explosions and their role in the universe
Core Concepts
- Star birth and formation
- Stellar death
- Supernovae
- Remnants
Formulas
$$M_{Ch} = 1.4 \, M_{\odot}$$
Chandrasekhar limit for white dwarf stability
$$R_s = \frac{2GM}{c^2}$$
Schwarzschild radius determining black hole event horizon
Units
| Solar mass | M_☉ |
Interesting Fact
A neutron star is so dense that a teaspoon would weigh as much as a mountain on Earth
Key Scientist
Subrahmanyan Chandrasekhar
Determined the maximum mass of a white dwarf (Chandrasekhar limit)
Modern Research
Gravitational wave detections from neutron star mergers reveal new physics and provide evidence for the origin of heavy elements.
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