2. E2 Stellar radiation and stellar types

3. Fusion http://www.youtube.com/watch?v=gS1dpow PlE8&feature=relmfu

4. Life-cycle of a star

5. Video on life of a star

6. Birth of a Star All stars start life as a nebula of gas and dust. Over millions of years gravity pulls these closer together.

7. Gravitational force Birth of a star Nebula Pressure builds up and the core starts to heat up giving out infra red radiation.

8. Birth of a star Protostar Star The gravity eventually gets so big and the temperature gets so high that nuclear fusion starts, it becomes a star The dust and gas from the nebula is added to the protostar, it gains mass. As mass is gained gravity increases and the temperature within the protostar increases

9. Life of a star

10. Radiation Pressure From the energy of fusion Gravitational force From the mass of the material A Stable Star like our Sun Nuclear fusion 4 Hydrogen 1Helium + ENERGY (Grade A) Nuclear fusion 4 Hydrogen 1Helium + ENERGY (Grade A) The force of the radiation pressure from nuclear fusion is balanced with the gravitational force in a stable star. (Grade B)

11. Death of a Star Star like our SunA large Star

12. Star Red Giant White dwarf Black Dwarf Eventually a star the size of our sun becomes a Red Giant. The star keeps increasing in size until the gravitational force causes it to collapse into itself creating a White Dwarf This cools down to become a black dwarf.

13. Large Star Red Supergiant Supernova Neutron Star Pulsar Black Hole A larger star eventually becomes a super Red Giant. This then collapses, heats up and explodes in a supernova. The small core becomes a neutron star. This can turn into a pulsar If a star is large enough it’ll become a black hole.

15. Equilibrium between radiation pressure and gravity

16. Luminosity (symbol L) Luminosity is defined as the amount of energy radiated by the star per second (The power radiated by the star) Measured in Watts (J.s -1 )

17. Black-body radiation

18. Need to “learn” this!

19. Black-body radiation Black Body - any object that is a perfect emitter and a perfect absorber of radiation object does not have to appear "black" Stars behave approximately as black bodies

20. Black-body radiation The amount of energy per second (power) radiated from a star (its luminosity) depends on its surface area and absolute temperature according to L = σAT 4 where σ is the Stefan-Boltzmann constant (5.67 x 10 -8 W.m -2.K -4 )

21. Example The sun (radius R = 7.0 x 10 8 m) has a luminosity of 3.9 x 10 26 W. Find its surface temperature. From L = σAT 4 and A = 4πR 2 we find T = (L/σ 4πR 2 ) ¼ = 5800 K

22. Wien’s law – Finding the temp of a star λ max T = constant (2.9 x 10 -3 mK)

23. Example The sun has an approximate black-body spectrum and most of its energy is radiated at a wavelength of 5.0 x 10 -7 m. Find the surface temperature of the sun. From Wien’s law 5.0 x 10 -7 x T = 2.9 x 10 -3 T = 5800 K

24. Apparent brightness (symbol b) Apparent brightness is defined as the amount of energy per second per unit area of detector b = L/4πd 2 where d is the distance from the star (in m) L is the luminosity (in W)

25. Intensity at a distance from a light source (Apparent brightness) b = L/4πd 2 d

26. Apparent brightness - CCD Apparent brightness is measured using a charge-coupled device (used also in digital cameras) Read the final paragraph of page 495.

27. Apparent brightness and Luminosity Note that the apparent brightness b and luminosity L are proportional b = L/4πd 2 b α L α T 4

28. Spectral ClassColourTemperature/K OBlue25 000 – 50 000 BBlue - white12 000 – 25 000 AWhite7 500 – 12 000 FYellow - white6 000 – 7 500 GYellow4 500 – 6 000 KYellow - red3 000 – 4 500 MRed2 000 – 3 000 You need to remember the classes and their order How will you do this?

29. Spectral classes Oh be a fine girl….kiss me!

30. Let’s try some luminosity/brightness questions! Bummer.

31. More information from spectra The spectrum of a star can have dark absorption lines across it. Each dark line represents the absorption of light at a specific frequency by a chemical element in the star

32. Niels Bohr In 1913, a Danish physicist called Niels Bohr realised that the secret of atomic structure lay in its discreteness, that energy could only be absorbed or emitted at certain values. At school they called me “Bohr the Bore”!

33. The Bohr Model Bohr realised that the electrons could only be at specific energy levels (or states) around the atom.

34. The Bohr Model We say that the energy of the electron (and thus the atom) can exist in a number of states n=1, n=2, n=3 etc. (Similar to the “shells” or electron orbitals that chemists talk about!) n = 1 n = 3 n = 2

35. The Bohr Model The energy level diagram of the hydrogen atom according to the Bohr model n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 High energy n levels are very close to each other Energy eV -13.6 0 Electron can’t have less energy than this

36. The Bohr Model An electron in a higher state than the ground state is called an excited electron. High energy n levels are very close to each other n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 -13.6 Energy eV 0 electron

37. Atomic transitions If a hydrogen atom is in an excited state, it can make a transition to a lower state. Thus an atom in state n = 2 can go to n = 1 (an electron jumps from orbit n = 2 to n = 1) n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 -13.6 Energy eV 0 electron Wheeee!

38. Atomic transitions Every time an atom (electron in the atom) makes a transition, a single photon of light is emitted. n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 -13.6 Energy eV 0 electron

39. Atomic transitions The energy of the photon is equal to the difference in energy (ΔE) between the two states. It is equal to hf. ΔE = hf n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 -13.6 Energy eV 0 electron ΔE = hf

40. Atomic transitions An electron can also absorb a photon of the same energy and jump to a hjgher level. n = 1 (the ground state) n = 2 n = 3 n = 4 n = 5 -13.6 Energy eV 0 electron ΔE = hf

41. More information from spectra The absorption spectrum thus gives us information about a star’s chemical composition

42. Very hot stars Very hot stars do not show an absorption spectrum as all the gas is ionised so there are no bound electrons orbiting around the nuclei in the star. Thus absorption spectrums can also tell us something about the temperature of a star.

43. Doppler effect on spectra

44. Radial velocity

45. Rotation

46. Different types of stars

47. Binary stars

48. Spectroscopic binaries

49. Eclipsing binaries

51. Cepheids A type of variable start whose luminosity changes with time (more later!)

52. Red giants and red supergiants Large in size and red in colour. Large in size and red in colour. Large luminosity Large luminosity Since they are red, they are comparatively cool. Since they are red, they are comparatively cool. The source of energy is the fusion of some elements other than hydrogen. The source of energy is the fusion of some elements other than hydrogen.

53. Small and white in colour. Small and white in colour. Since they are white they are comparatively hot. Since they are white they are comparatively hot. Fusion is no longer taking place, and a white dwarf is just a hot remnant that is cooling down. Fusion is no longer taking place, and a white dwarf is just a hot remnant that is cooling down. White dwarfs

54. Hertzsprung – Russell diagram

55. The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. The point of classifying the various types of stars is to see is any patterns exists. A useful way of making the comparison is the H-R diagram. Each dot on the diagram represents a different star. The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear one. The vertical axis is the luminosity of the star. It should be noted that the scale is not a linear one. The horizontal axis is the spectral class of the star in the order OBAFGKM. This is the same as a scale of decreasing temperature. Once again the scale is not a linear one. The horizontal axis is the spectral class of the star in the order OBAFGKM. This is the same as a scale of decreasing temperature. Once again the scale is not a linear one. The result of such a plot is shown on the next slide The result of such a plot is shown on the next slide Hertzsprung – Russell diagram

56. Cepheids!

57. A large number of stars the fall on the line that goes from the top left to bottom right. This line is known as the MAIN SEQUENCE and stars that are on it are known as the main sequence stars. Our sun is a main sequence star. These stars are ‘normal’ stable stars- the only difference between them is their mass. They are fusing hydrogen to helium. The stars that are not on the main sequence can also be put into categories. A large number of stars the fall on the line that goes from the top left to bottom right. This line is known as the MAIN SEQUENCE and stars that are on it are known as the main sequence stars. Our sun is a main sequence star. These stars are ‘normal’ stable stars- the only difference between them is their mass. They are fusing hydrogen to helium. The stars that are not on the main sequence can also be put into categories. Hertzsprung – Russell diagram

58. Questions Page 504 Questions 1, 2, 3, 4, 5, 6, 7, 9.