2. 16.1 Stellar Nurseries Our goals for learning: – Where do stars form? – Why do stars form? © 2014 Pearson Education, Inc.

3. Where do stars form? © 2014 Pearson Education, Inc.

4. Stellar Evolution Stars are like people in that they are born, grow up, mature, and die. A star ’ s mass determines what life path it will take. We will divide all stars into three groups: – Low Mass (0.08 M  < M < 2 M  ) – Intermediate Mass (2 M  < M < 8 M  ) – High Mass (M > 8 M  ) The H-R Diagram makes a useful roadmap for following stellar evolution.

5. Stellar Evolution The life of any star can be described as a battle between two forces: – GravityPressure – Gravity vs. Pressure Gravity always wants to collapse the star. Pressure holds up the star. – the type of star is defined by what provides the pressure Remember Newton ’ s Law of Gravity – the amount of gravitational force depends on the mass – gravitational potential energy is turned into heat as a star collapses

6. Star-Forming Clouds Stars form in dark clouds of dusty gas in interstellar space. The gas between the stars is called the interstellar medium. © 2014 Pearson Education, Inc.

7. Composition of Clouds We can determine the composition of interstellar gas from its absorption lines in the spectra of stars. 70% H, 28% He, 2% heavier elements in our region of Milky Way © 2014 Pearson Education, Inc.

8. Molecular Clouds Most of the matter in star-forming clouds is in the form of molecules (H 2, CO, etc.). These molecular clouds have a temperature of 10–30 K and a density of about 300 molecules per cubic centimeter. © 2014 Pearson Education, Inc.

9. Molecular Clouds Most of what we know about molecular clouds comes from observing the emission lines of carbon monoxide (CO). © 2014 Pearson Education, Inc.

10. Interstellar Dust Tiny solid particles of interstellar dust block our view of stars on the other side of a cloud. Particles are < 1 micrometer in size and made of elements like C, O, Si, and Fe. © 2014 Pearson Education, Inc.

11. Interstellar Reddening Stars viewed through the edges of the cloud look redder because dust blocks (shorter- wavelength) blue light more effectively than (longer-wavelength) red light. © 2014 Pearson Education, Inc.

12. Interstellar Reddening Long-wavelength infrared light passes through a cloud more easily than visible light. Observations of infrared light reveal stars on the other side of the cloud. © 2014 Pearson Education, Inc.

13. Observing Newborn Stars Visible light from a newborn star is often trapped within the dark, dusty gas clouds where the star formed. © 2014 Pearson Education, Inc.

14. Observing Newborn Stars Observing the infrared light from a cloud can reveal the newborn star embedded inside it. © 2014 Pearson Education, Inc.

15. Observing Newborn Stars

16. Glowing Dust Grains Dust grains that absorb visible light heat up and emit infrared light of even longer wavelength. © 2014 Pearson Education, Inc.

17. Glowing Dust Grains Long-wavelength infrared light is brightest from regions where many stars are currently forming. © 2014 Pearson Education, Inc.

18. Why do stars form? © 2014 Pearson Education, Inc.

19. Gravity versus Pressure Gravity can create stars only if it can overcome the force of thermal pressure in a cloud. Emission lines from molecules in a cloud can prevent a pressure buildup by converting thermal energy into infrared and radio photons. © 2014 Pearson Education, Inc.

20. Mass of a Star-Forming Cloud A typical molecular cloud (T~ 30 K, n ~ 300 particles/cm 3 ) must contain at least a few hundred solar masses for gravity to overcome pressure. Emission lines from molecules in a cloud can prevent a pressure buildup by converting thermal energy into infrared and radio photons that escape the cloud. © 2014 Pearson Education, Inc.

21. Resistance to Gravity A cloud must have even more mass to begin contracting if there are additional forces opposing gravity. Both magnetic fields and turbulent gas motions increase resistance to gravity. © 2014 Pearson Education, Inc.

22. Fragmentation of a Cloud Gravity within a contracting gas cloud becomes stronger as the gas becomes denser. Gravity can therefore overcome pressure in smaller pieces of the cloud, causing it to break apart into multiple fragments, each of which may go on to form a star. © 2014 Pearson Education, Inc.

23. Fragmentation of a Cloud This simulation begins with a turbulent cloud containing 50 solar masses of gas. © 2014 Pearson Education, Inc.

24. Fragmentation of a Cloud The random motions of different sections of the cloud cause it to become lumpy. © 2014 Pearson Education, Inc.

25. Fragmentation of a Cloud Each lump of the cloud in which gravity can overcome pressure can go on to become a star. A large cloud can make a whole cluster of stars. © 2014 Pearson Education, Inc.

26. Isolated Star Formation Gravity can overcome pressure in a relatively small cloud if the cloud is unusually dense. Such a cloud may make only a single star. © 2014 Pearson Education, Inc.

27. Thought Question What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A.It would continue contracting, but its temperature would not change. B.Its mass would increase. C.Its internal pressure would increase. © 2014 Pearson Education, Inc.

28. Thought Question What would happen to a contracting cloud fragment if it were not able to radiate away its thermal energy? A.It would continue contracting, but its temperature would not change. B.Its mass would increase. C.Its internal pressure would increase. © 2014 Pearson Education, Inc.

29. The First Stars Elements like carbon and oxygen had not yet been made when the first stars formed. Without CO molecules to provide cooling, the clouds that formed the first stars had to be considerably warmer than today's molecular clouds. The first stars must therefore have been more massive than most of today's stars, for gravity to overcome pressure. © 2014 Pearson Education, Inc.

30. Simulation of the First Star Simulations of early star formation suggest the first molecular clouds never cooled below 100 K, making stars of ~100M Sun. © 2014 Pearson Education, Inc.

31. What have we learned? Where do stars form? – Stars form in dark, dusty clouds of molecular gas with temperatures of 10–30 K. – These clouds are made mostly of molecular hydrogen (H 2 ) but stay cool because of emission by carbon monoxide (CO). Why do stars form? – Stars form in clouds that are massive enough for gravity to overcome thermal pressure (and any other forms of resistance). – Such a cloud contracts and breaks up into pieces that go on to form stars. © 2014 Pearson Education, Inc.

32. 16.2 Stages of Star Birth Our goals for learning: – What slows the contraction of a star-forming cloud? – What is the role of rotation in star birth? – How does nuclear fusion begin in a newborn star? © 2014 Pearson Education, Inc.

33. What slows the contraction of a star- forming cloud?

34. Trapping of Thermal Energy As contraction packs the molecules and dust particles of a cloud fragment closer together, it becomes harder for infrared and radio photons to escape. Thermal energy then begins to build up inside, increasing the internal pressure. Contraction slows down, and the center of the cloud fragment becomes a protostar. © 2014 Pearson Education, Inc.

35. Growth of a Protostar Matter from the cloud continues to fall onto the protostar until either the protostar or a neighboring star blows the surrounding gas away. © 2014 Pearson Education, Inc.

36. What is the role of rotation in star birth?

37. Evidence from the Solar System The nebular theory of solar system formation illustrates the importance of rotation. © 2014 Pearson Education, Inc.

38. Conservation of Angular Momentum The rotation speed of the cloud from which a star forms increases as the cloud contracts. © 2014 Pearson Education, Inc.

39. Rotation of a contracting cloud speeds up for the same reason a skater speeds up as she pulls in her arms.

40. Flattening Collisions between particles in the cloud cause it to flatten into a disk.

41. Collisions between gas particles in cloud gradually reduce random motions.

42. Collisions between gas particles also reduce up and down motions.

43. The spinning cloud flattens as it shrinks.

44. Formation of Jets Rotation also causes jets of matter to shoot out along the rotation axis.

45. Jets are observed coming from the centers of disks around protostars.

47. Thought Question What would happen to a protostar that formed without any rotation at all? A.Its jets would go in multiple directions. B.It would not have planets. C.It would be very bright in infrared light. D.It would not be round. © 2014 Pearson Education, Inc.

48. Thought Question What would happen to a protostar that formed without any rotation at all? A.Its jets would go in multiple directions. B.It would not have planets. C.It would be very bright in infrared light. D.It would not be round. © 2014 Pearson Education, Inc.

49. Star Formation As the protostar heats up, enough thermal energy is radiated away from surface to allow collapse to continue. – energy is transported to surface first via convection – as core gets even hotter, transport via radiation takes over The protostar must rid itself of angular momentum, or it will tear itself apart – magnetic fields drag on the protostellar disk – fragmentation into binaries Fusion reactions begin when core reaches 10 7 K

50. How does nuclear fusion begin in a newborn star? © 2014 Pearson Education, Inc.

51. From Protostar to Main Sequence A protostar looks starlike after the surrounding gas is blown away, but its thermal energy comes from gravitational contraction, not fusion. Contraction must continue until the core becomes hot enough for nuclear fusion. Contraction stops when the energy released by core fusion balances energy radiated from the surface—the star is now a main-sequence star. © 2014 Pearson Education, Inc.

52. Birth Stages on a Life Track A life track illustrates a star's surface temperature and luminosity at different moments in time. © 2014 Pearson Education, Inc.

53. Assembly of a Protostar Luminosity and temperature grow as matter collects into a protostar. © 2014 Pearson Education, Inc.

54. Convective Contraction Surface temperature remains near 3000 K while convection is main energy transport mechanism. © 2014 Pearson Education, Inc.

55. Radiative Contraction Luminosity remains nearly constant during late stages of contraction, while radiation transports energy through star. © 2014 Pearson Education, Inc.

56. Self-Sustaining Fusion Core temperature continues to rise until star begins fusion and arrives on the main sequence. © 2014 Pearson Education, Inc.

57. Life Tracks for Different Masses Models show that Sun required about 30 million years to go from protostar to main sequence. Higher-mass stars form faster. Lower-mass stars form more slowly. © 2014 Pearson Education, Inc.

58. What have we learned? What slows the contraction of a star-forming cloud? – The contraction of a cloud fragment slows when thermal pressure builds up because infrared and radio photons can no longer escape. What is the role of rotation in star birth? – Conservation of angular momentum leads to the formation of disks around protostars. © 2014 Pearson Education, Inc.

59. What have we learned? How does nuclear fusion begin in a newborn star? – Nuclear fusion begins when contraction causes the star's core to grow hot enough for fusion. © 2014 Pearson Education, Inc.

60. 16.3 Masses of Newborn Stars Our goals for learning: – What is the smallest mass a newborn star can have? – What is the greatest mass a newborn star can have? – What are the typical masses of newborn stars? © 2014 Pearson Education, Inc.

61. What is the smallest mass a newborn star can have? © 2014 Pearson Education, Inc.

62. Missing the Main Sequence If the protostar has a mass < 0.08 M  : – It does not contain enough gravitational energy to reach a core temperature of 10 7 K – No fusion reactions occur – The star is stillborn! Brown Dwarfs We call these objects Brown Dwarfs. They are very faint, emit infrared, and have cores made of Hydrogen – degenerate cores

63. The First Brown Dwarf Discovery

64. Fusion and Contraction Fusion will not begin in a contracting cloud if some sort of force stops contraction before the core temperature rises above 10 7 K. Thermal pressure cannot stop contraction because the star is constantly losing thermal energy from its surface through radiation. Is there another form of pressure that can stop contraction? © 2014 Pearson Education, Inc.

65. Degeneracy Pressure: The laws of quantum mechanics prohibit two electrons from occupying the same state in same place. © 2014 Pearson Education, Inc.

66. Thermal Pressure: Depends on heat content. Is the main form of pressure in most stars. Degeneracy Pressure: Particles can't be in same state in same place. Doesn't depend on heat content.

67. Brown Dwarfs Degeneracy pressure halts the contraction of objects with < 0.08M Sun before core temperature becomes hot enough for fusion. Starlike objects not massive enough to start fusion are brown dwarfs. © 2014 Pearson Education, Inc.

68. Brown Dwarfs A brown dwarf emits infrared light because of heat left over from contraction. Its luminosity gradually declines with time as it loses thermal energy. © 2014 Pearson Education, Inc.

69. Brown Dwarfs in Orion Infrared observations can reveal recently formed brown dwarfs because they are still relatively warm and luminous. © 2014 Pearson Education, Inc.

70. What is the greatest mass a newborn star can have? © 2014 Pearson Education, Inc.

71. Radiation Pressure Photons exert a slight amount of pressure when they strike matter. Very massive stars are so luminous that the collective pressure of photons drives their matter into space. © 2014 Pearson Education, Inc.

72. Upper Limit on a Star's Mass Models of stars suggest that radiation pressure limits how massive a star can be without blowing itself apart. Maximum thought to be around 150M Sun, but new observations indicate some may be even larger! © 2014 Pearson Education, Inc.

73. Stars more massive than 150M Sun would blow apart. Stars less massive than 0.08M Sun can't sustain fusion. Temperature Luminosity

74. What are the typical masses of newborn stars? © 2014 Pearson Education, Inc.

75. Demographics of Stars Observations of star clusters show that star formation makes many more low- mass stars than high-mass stars. © 2014 Pearson Education, Inc.

76. What have we learned? What is the smallest mass a newborn star can have? – Degeneracy pressure stops the contraction of objects <0.08M Sun before fusion starts. What is the greatest mass a newborn star can have? – Stars greater than about 150M Sun would be so luminous that radiation pressure would blow them apart. – New observations may require raising this limit. © 2014 Pearson Education, Inc.

77. What have we learned? What are the typical masses of newborn stars? – Star formation makes many more low-mass stars than high-mass stars. © 2014 Pearson Education, Inc.

78. Life on the Main Sequence Where a star lands on the MS depends on its mass – O dwarfs (O V) are most massive – M dwarfs (M V) are least massive MS stars convert H  He in their cores The star is stable, in balance – Gravity vs. pressure from H fusion reactions

79. Life on the Main Sequence The internal structure is different for MS stars of different masses. How long do these stars stay on the MS? Until they burn up their fuel (H)!! Massive stars have more fuel, but they are also brighter, so they use it up faster.

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

81. The Main Sequence The majority of the star’s life is spent on the Main Sequence In the next chapter we will look at how stars leave the main sequence and further discuss the difference between high and low mass stars in the way they die and what they leave behind