Difference between revisions of "Stellar Structure"
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*For a star that loses its energy source and begin to collapse, how does its virialization time scale compare to its collapsing time scale? | *For a star that loses its energy source and begin to collapse, how does its virialization time scale compare to its collapsing time scale? | ||
*What causes limb darkening? Why is it colour dependent? Why is it more prominent in the blue than in IR? (MT) | *What causes limb darkening? Why is it colour dependent? Why is it more prominent in the blue than in IR? (MT) | ||
| + | *Why are giant stars giant? (SR) | ||
| + | *What is the pressure, density relation of a white dwarf? Derive the mass-radius relation of a white dwarf? (SR) | ||
| + | *Why do Cepheid variables vary - what is the physical mechanism? | ||
| + | |||
[[Astrophysics]] | [[Astrophysics]] | ||
Latest revision as of 17:10, 26 April 2009
- What are the equations of stellar structure?
- What is Betelguese? What is its spectral class?
- What is Sirius? What is its spectral class?
- What is the seperation between Sirius and its WD companion?
- How does the maximum mass of a WD made from hydrogen differ from one made of Carbon?
- For a star that loses its energy source and begin to collapse, how does its virialization time scale compare to its collapsing time scale?
- What causes limb darkening? Why is it colour dependent? Why is it more prominent in the blue than in IR? (MT)
- Why are giant stars giant? (SR)
- What is the pressure, density relation of a white dwarf? Derive the mass-radius relation of a white dwarf? (SR)
- Why do Cepheid variables vary - what is the physical mechanism?
