1. At the Heart of a Supernova Sarah Silva Program Manager Sonoma State University E/PO

3. Why study supernovae? Explain standards connection here – origin of chemical elements Blow up balloons

4. Supernova !

5. Stripchart activity Give them the cut up chart and ask them to put it in order here Discuss results and misconceptions Add color coding to stripchart for different wavelength bands

6. Life Cycle of a Supernova

7. Stellar evolution made simple Stars like the Sun go gentle into that good night More massive stars rage, rage against the dying of the light Puff! Bang! BANG!

8. Magnetic Globe Demo

9. Connection between earth and NS What do you think is the connection? Do the earth’s magnetic poles make any light? (insert aurora picture here to popup after question is asked) What is similar? What is different? What is strength of magnetic fields of both? (then tell them after they guess)

10. Strength of field of NS Needs new picture here to show lines going through spheres with different areas Need a good analogy – earth field can turn a compass needle, NS field can turn a ?? (10 Ocean liners in a big compass)

11. Pulsar movie slide goes here Show pulsing crab movie Ask questions about what is happening

12. At the Heart of a Supernova Experiment: Using the materials provided; design and create a model of a pulsing neutron star. Describe it on the page provided. Suggested Materials: 2 Diodes Tape Small batteries (3 V) Modeling clay Aluminum foil String or rubber band You have 20 minutes to put your pulsar together and answer questions 18-27.

13. Group model show Have everyone show their models and explain how the pulses are made Let everyone discuss results Give prize for the best one

14. Neutron Stars and Pulsars

15. If neutron stars are made of neutral particles, how can they have magnetic fields? Neutron stars are not totally made of neutrons-- the interiors have plenty of electrons, protons, and other particles. These charged particles can maintain the magnetic field. Plus, a basic property of magnetism is that once a magnetic field is made, it cannot simply disappear. Stars have magnetic fields because they are composed of plasma, very hot gas made of charged particles.

16. Cas A Use chandra picture of Cas A with NS in center to illustrate one that does not pulse Discuss what it takes to make them pulse

17. Crab nebula and pulsar X-ray/Chandra

18. Reprise: the Life Cycle Sun-like Stars Massive Stars

19. Origin of the chemical elements Hydrogen fuses in outer shell around the core Heavier elements up to Iron fuse in inner shells Energy is released during each fusion reaction which keeps the star from collapsing

20. Origins pt. 2 When nuclear fuel runs out, star implodes, sending outer layer out to form supernova remnant Energy in the explosion is used to create heavier elements than iron Heavier elements are seen in remnant Needs picture

21. Supernova Educator Guide

22. Brought to you by: the NASA E/PO Program at Sonoma State University Our goal: educate the public about current and future NASA high energy (x-ray and gamma- ray) astrophysics/astronomy missions. Led by Prof. Lynn Cominsky Swift GLAST XMM-Newton

23. Resources E/PO at SSU: http://epo.sonoma.eduhttp://epo.sonoma.edu XMM-Newton Education and Public Outreach site: http://xmm.sonoma.eduhttp://xmm.sonoma.edu Supernova and Magnetic Globe –http://xmm.sonoma.edu/edu/supernovahttp://xmm.sonoma.edu/edu/supernova GLAST Education and Public Outreach site: http://glast.sonoma.edu http://glast.sonoma.edu Downloadable GLAST materials for: –http://glast.sonoma.edu/teachers/teachers.htmlhttp://glast.sonoma.edu/teachers/teachers.html My Email: sarah@universe.sonoma.edu

24. Extra Slides beyond this point.

25. Molecular clouds and protostars Giant molecular clouds are very cold, thin and wispy– they stretch out over tens of light years at temperatures from 10-100K, with a warmer core They are 1000s of time more dense than the local interstellar medium, and collapse further under their own gravity to form protostars at their cores BHR 71, a star-forming cloud (image is ~1 light year across)

26. Protostars Orion nebula/Trapezium stars (in the sword) About 1500 light years away HST / 2.5 light years Chandra/10 light years

27. Stellar nurseries Pillars of dense gas Newly born stars may emerge at the ends of the pillars About 7000 light years away HST/Eagle Nebula in M16

28. Classifying Stars Hertzsprung-Russell diagram Stars spend most of their lives on the Main Sequence

29. Pro Fusion or Con Fusion? The core of the Sun is 15 million degrees Celsius Fusion occurs 10 38 times a second Sun has 10 56 H atoms to fuse 10 18 seconds = 32 billion years 2 billion kilograms converted every second Sun’s output = 50 billion megaton bombs per second

30. 10 18 seconds is a long time… but it’s not forever. What happens then? Don’t Let the Sun Go Down on Me

31. The Beginning Of The End: Red Giants After Hydrogen is exhausted in core... Energy released from nuclear fusion counter-acts inward force of gravity. Core collapses, and kinetic energy of collapse converted into heat. This heat expands the outer layers. Meanwhile, as core collapses, Increasing Temperature and Pressure...

32. More Fusion ! At 100 million degrees Celsius, Helium fuses: 3 ( 4 He) --> 12 C + energy (Be produced at an intermediate step) (Only 7.3 MeV produced) Energy sustains the expanded outer layers of the Red Giant

33. A Burst By Any Other Name… Neutron star: dense core leftover from a supernova Possess incredibly strong magnetic fields Soft Gamma Ray Repeater: violent energy release due to starquake Accretion: neutron star draws matter off binary companion Matter piles up, undergoes fusion: bang! Cycle repeats: X-Ray Burster

34. What is XMM-Newton? A joint NASA-European Space Agency (ESA) orbiting observatory, designed to observe high-energy X-rays emitted from exotic astronomical objects such as pulsars, black holes, and active galaxies. XMM Newton Science Goals –When and where are the chemical elements created? –How does nature heat gas to X-ray emitting temperatures? Launched in 1999!

35. What is GLAST? GLAST: Gamma-Ray Large Area Space Telescope Planned for launch in 2007 GLAST has two instruments: –Large Area Telescope (LAT) –GLAST Burst Monitor (GBM) GLAST will look at many different objects within the energy range of 10keV to 300GeV. LAT GBM

36. Backups follow

37. Magnetic Fields Across the Universe

38. Main Sequence Stars Stars spend most of their lives on the “main sequence” where they burn hydrogen in nuclear reactions in their cores Burning rate is higher for more massive stars - hence their lifetimes on the main sequence are much shorter and they are rather rare Red dwarf stars are the most common as they burn hydrogen slowly and live the longest Often called dwarfs (but not the same as White Dwarfs) because they are smaller than giants or supergiants Our sun is considered a G2V star. It has been on the main sequence for about 4.5 billion years, with another ~5 billion to go

39. HR Diagram

40. How stars die Stars that are below about 8 M o form red giants at the end of their lives on the main sequence Red giants evolve into white dwarfs, often accompanied by planetary nebulae More massive stars form red supergiants Red supergiants undergo supernova explosions, often leaving behind a stellar core which is a neutron star, or perhaps a black hole

41. Fate of high mass stars After Helium exhausted, core collapses again until it becomes hot enough to fuse Carbon into Magnesium or Oxygen. 12 C + 12 C --> 24 Mg OR 12 C + 4 H --> 16 O Through a combination of processes, successively heavier elements are formed and fused.

42. Heavy Elements from Large Stars Large stars also fuse Hydrogen into Helium, and Helium into Carbon. But their larger masses lead to higher temperatures, which allow fusion of Carbon into Magnesium, etc.