The Lives of Stars

1. The Lives of Stars EXAM #3 – WILL NOT BE APRIL 5th it has been re-scheduled for THURSDAY APRIL 12th4/12 (Wednesday) Tailgate Party (aka exam review) For Exam #3 Wed April 11th Observing Logs Due IN CLASS May 1st

2. Topics that will be on the test!! Formation of the Solar System Sun Size Greenhouse Effect Apparent and Absolute Magnitude HR Diagram Stellar Formation and Lifetime Binary Stars Stellar Evolution

3. Recall from the HR- Diagram Red Giants are: Main Sequence stars are: White Dwarf stars are:

4. Stars condense from clouds of gas and dust (the interstellar medium) that exist throughout the disk of the galaxy Interstellar medium Gas = Hydrogen Dust = Carbon and Silicon

5. Becoming a Star Step 1 – Cloud collapses • Why do these clouds of gas and dust collapse? • One idea is that a shockwave from the explosion at the death of a star known as a supernova cause the gas and dust cloud to become unstable and start to collapse

6. Becoming a Star Step 1 – Cloud collapses • As the cloud collapses, the center becomes very very hot and very very dense -

7. Becoming a Star Step 2 – Fusion • As the gas cloud collapses due to gravitational forces, the core becomes hotter and the density inside the core increases • Eventually, the temperature and density reach a point where nuclear fusion can occur

8. Fusion is the combining together of light atoms, into heavier atoms For all Main Sequence stars,the temperature and density in their cores are so great that Hydrogen atoms combine to make Helium atoms and release energy – a process known as thermonuclear fusion 4H  He + energy

9. Becoming a Star Step 3 – BalanceAll Main Sequence stars are in hydrostatic equilibrium • Fusion producesradiation (light)thatcreates an outward pressure • Duringhydrostatic equilibriumthere is abalancebetween thegravitational collapseof the star pushing inward and the outwardpressureproduced by photons from nuclear fusion in the core.

10. It’s a matter of balance. • This balance is calledhydrostatic equilibrium • gravity ( )wants to collapse the star, but pressure ( )pushes outward against the collapsing material Fusion: 4H  He + energy(light)

11. All Main Sequence stars are in hydrostatic equilibrium because nuclear fusion of hydrogen is producing enough outwardpressureto balancegravitational collapse.

12. It takes a few million years to get there but - stars spend most of their life time as a Main Sequence star

13. Stars spend most of their life time as a Main Sequence star • 90% of the whole life of all stars is spent on the Main Sequence • 90% of all stars are found on the Main Sequence

14. Stars often form in pairs called “Binary Stars” • These stars can orbit each other much like a star and a planet, and in some cases the stars pass in front of each other - we call these “Eclipsing Binary” stars

15. Tutorial: Binary Stars LT (handout) • Work with a partner! • Read the instructions and questions carefully. • Discuss the concepts and your answers with one another. Take time to understand it now!!!! • Come to a consensus answer you both agree on. • If you get stuck or are not sure of your answer, ask another group.

16. In which case will you receive the most light on Earth? C A B

17. Which of these is physically wrong if they are all main sequence stars? C A B

18. In which case will you receive the most light on Earth? • When a A spectral class main-sequence star is in front of a red giant. • When an M spectral class main-sequence star is in front of a O spectral class main sequence star. • When a M spectral class main-sequence star is in front of a G spectral class star. • When a K spectral class main-sequence star is in front of a red giant.

19. STELLAR LIFETIMES • Which will have a greater core temperature and density – a high mass star or a low mass star? • Which will then have a greater fusion rate? • Which will use up its fuel more quickly? • What is the fuel?

20. STELLAR LIFETIMES • Consider a main sequence star with 10 times the mass of the Sun • It will • have higher temps and pressures at the core • have greater fusion rates - consumes fuel at 1000 times the rate of the sun • be 1000 times as bright and last 1/100 as long • “Burn bright, die young.”

21. LIFETIMES • Bright O-type stars live very short lives (about 10 million years) • Very small stars live a long time (100 billions of years) • Our SUN: will live a total of about 10 billion years (half used up)

22. The more massive a star, the faster it goes through its main sequence phase

23. Tutorial: Star Formation and Lifetimes (p.81) • Work with a partner! • Read the instructions and questions carefully. • Discuss the concepts and your answers with one another. Take time to understand it now!!!! • Come to a consensus answer you both agree on. • If you get stuck or are not sure of your answer, ask another group.

24. How does the Sun produce the energy that heats our planet? • The gases inside the Sun are burning and producing large amounts of energy. • Hydrogen is combined into helium, giving off large amounts of energy. • Gas inside the Sun heats up when compressed, giving off large amounts of energy. • Heat trapped by magnetic fields in the Sun is released as energy. • The core of the sun has radioactive atoms that give off energy as they decay.

25. Consider the information given below about the lifetime of three main sequence stars A, B, and C. - Star A will be a main sequence star for 45,000 million years. - Star B will be a main sequence star for 70 million years. - Star C will be a main sequence star for 2 million years.Which of the following is a true statement about these stars?

26. Star A has a mass of 5 solar masses and Star B has a mass of 10 solar masses. How will the fusion rate of Star A compare to the fusion rate of Star B? • Star A’s fusion rate will be more than two times slower than that of Star B. • Star A’s fusion rate will be two times slower than that of Star B. • Star A’s fusion rate will be the same as that of Star B. • Star A’s fusion rate will be two times faster than that of Star B. • Star A’s fusion rate will be more than two times faster than that of Star B.

27. Stars spend most of their life cycles on the Main Sequence • Main Sequence stars are in hydrostatic equilibrium because nuclear fusion is turning hydrogen into helium and producing enough outward pressure to balance gravitational collapse. • 90% of all stars are found on the Main Sequence • 90% of the whole life of all stars is spent on the Main Sequence • BUT – What happens when the hydrogen runs out?