Chapter 10 Our Star, The Sun

1. Chapter 10Our Star, The Sun

2. Star Types

3. Red Dwarf Systems • Habitable zone would be small and close to the star • Tidal lock likely • Dwarfs are more variable than G-stars • Sunspots drop light by 40%

4. The first scientific theories involved chemical reactions or gravitational collapse. Chemical burning ruled out…it can not account for the Sun’s luminosity Conversion of gravitational potential energy into heat as the Sun contracts would only keep the Sun shining for ~30 million years Late 19th-century geological research indicated the Earth was older than that The Sun’s Energy Source

5. The Time Machine (1895) • Reflected the current ideas of geological time • After messing with the Morlocks, the Traveler goes 30 million years into the future • Finds the Earth’s rotation slowed, the Sun weak and dully red, close to burning out.

6. Bishop Ussher • Church of Ireland Archbishop of Armagh and Primate of All Ireland between 1625–56 • He calculated the beginning of creation as Sunday, October 23, 4004 BC based on he then-widely held belief that the Earth's potential duration was 6,000 years. • 4,000 years before the birth of Christ and 2,000 after (note we have now passed that mark) • This corresponds to the six days of Creation, on the grounds that "one day is with the Lord as a thousand years, and a thousand years as one day" (2 Peter 3:8)

7. This was a consensus number • Jose benHalafta (2nd Century Rabbinical Scholar) 3896 BC • Bede (7th Century Monk) 3952 BC • Scaliger (16th Century Scholar) 3949 BC • Johannes Kepler (17th Century Astronomer) 3992 BC • Sir Isaac Newton (17th Century Genius) c. 4000 BC • John Lightfoot (17th Century Vice-Chancellor of Cambridge) 3929 BC

8. But things were changing…. • Geology was developing as a science…. • While early geologists had no way of measuring absolute time, it was pretty clear that it took a “long” time to deposit visible strata. • The approach was to count up the layers and guess at how fast they could be laid down • The total column of sediment was about 50,000 yards! • The early estimate was about 96 million years.

9. Early evolutionists (ca ~1860s) thought that 100 million years was way too short for the workings of natural selection. • Geneticists have subsequently measured the rate of genetic divergence of species, using the molecular clock, to date the last universal ancestor of all living organisms no later than 3.5 to 3.8 billion years ago.

10. Enter Lord Kelvin • William Thomson was a brilliant mathematician and physicist • Professor at 22 • Fellow of the Royal Society at 24 • Made a Lord in 1892 • Buried next to Isaac Newton • He made major contributions all his life. • Revolutionized the science of thermodynamics • Worked out the Kinetic theory with Joule • Was central to establishing transatlantic telegraph communications. • Made substantial contributions to electrical theory and measurement. • And he dabbled in Earth science.

11. Enter Lord Kelvin • Determining the age of the Earth had become BIG science. • Both the evolutionists and geologists thought that their sciences required “long” periods of time. • Kelvin thought that thermodynamics could put some limits on the age of the solar system.

12. Start with the Sun • The Sun is shining…..right? • That energy must come from somewhere. • The only plausible source for the was internal, derived from the gravitational potential energy released during its accretion. • It is easy from Newton to calculate the energy released from accretion and from gravitational contraction. • The resulting estimate was that the Sun could shine for about 100 million years (later reduced to 20 My).

13. Now the Earth • Assume: • the Earth was initially molten. • the planet is rigid • its physical properties are homogeneous • no undiscovered source of energy • The initial heat of the Earth should diffuse out and produce a temperature gradient. • The slope of the gradient is a function of the age of the cooling….i.e. the age of the Earth.

14. Now the Earth • He estimated the gradient at about 1/50th of a degree Fahrenheit per foot(or about 36 degrees Celsius per kilometer). • Not bad…..modern measurements are 25-30° C/km • He estimated Earth’s initial temperature (7,000 degrees Fahrenheit, or 3,900 degrees C) from melting experiments on rocks. • Also not bad, modern estimates of core temperature are 7,000K. • This gave an age for the Earth of between 24 million and 400 million years given the uncertainties in the geothermal gradient and thermal conductivity. • If you repeat this calculation using modern numbers for the gradient and conductivity, you get between 24-96 My.

15. Why was Kelvin Wrong? • This drove the 19th century geologists crazy! • “I am as incapable of estimating and understanding the reasons which you physicists have for limiting geological time as you are incapable of understanding the geological reasons for our unlimited estimates.” (Sir Andrew Ramsay, 1867) • But Kelvin had made a fundamental mistake in his assumptions. • Most people thought it was the “no undiscovered source of energy” assumption, but no…..

16. Enter John Perry • He was a professor at what is now Imperial College London. • He had spent several years as Kelvin’s assistant • He had the idea that the Earth’s interior was partially fluid and convection, not conduction was the primary mode of heat transport • Convention would be much more efficient heat transport, so the core could be much hotter, longer than with convection. • He privatively raised these ideas with Kelvin and got blown off.

17. Enter John Perry • Perry published in 1896 and showed that if the Earth has a conducting lid of 50 kilometers’ thickness, with a convecting fluid underneath, then the thermal gradients near the surface are consistent with any age up to 2 billion or 3 billion years.

18. Radioactivity is actually a Red Herring in this debate • Of course, about this time radioactivity as a heat source is discovered (Curie, 1903) • Ernest Rutherford proposed 1904 that it was radioactive heat that was actually responsible for a much older Earth than Kelvin had supposed • BUT, if you keep Kelvin’s conduction model, radioactivity doesn’t have much effect.

19. But Radioactivity was Ultimately the Solution • Rutherford was on to something • There are 339 isotopes of 84 elements found in nature • 269 are stable (calcium has 6 stable isotopes, Tin has 10) • 70 are radioactive • In 1904, Rutherford suggested that the alpha particles released by radioactive decay of radium could be trapped in a rocky material as helium atoms. • One of the first rocks dated that way came back with a 40 million year age. • By the end of 1905 dates for 26 separate rock samples ranged from 92 to 570 million years

20. Development of nuclear physics led to the correct answer the Sun generates energy via nuclear fusion reactions the mass lost is transformed into energy Einstein’s equation: E = mc2 this will provide enough energy for the Sun to shine for 10 billion years The Sun’s Energy Source

21. Why does fusion occur in the Sun’s core ? • Nuclear fusion • a reaction where heavier nuclei are created by combining (fusing) lighter nuclei. • all nuclei are positively charged • Electromagnetic force causes nuclei to repel each other. • Remember the nucleus is full of protons! Like charges repel! • for fusion to occur, nuclei must be moving fast enough to overcome E-M repulsion • this requires high temperatures & pressures! • When nuclei touch, the nuclear force binds them together

22. The proton-proton chain , showing the process of hydrogen fusing into helium.

23. The first important thing to know is that it is a sequence of events. You can’t have 4 protons colliding at the same time to give you helium. That’s not what happens.

24. You’ll see a figure like this -- but don’t get confused! This is the summary of all the steps. IN 4 protons OUT Helium nucleus 2 photons - gamma rays! 2 positrons 2 neutrinos • Add up the mass of the helium and positrons. Add up the mass of the 4 protons. They are different! • Total mass of the products is 0.7% lower than the total mass of the inputs. • Where did that mass go? Converted to energy. E = mc2 • In the Sun every second 600 million tons H  596 million tons He • 4 million tons each second gets converted to energy via E = mc2

26. Up until Iron it atoms require LESS mass (i.e. binding energy) per particle. The result is that mass is converted to energy and released with fusion It works the same way with fission moving down the atomic mass number

27. Solar wind: A flow of charged atoms from the surface of the Sun

28. Corona: Outermost layer of solar atmosphere ~1 million ºC Very hot, but very diffuse. You would not be burned by the corona.

29. Chromosphere: Middle layer of solar atmosphere ~ 104 - 105 ºC

30. Photosphere: Visible surface of Sun About 5500 ºC

31. Convection Zone: Now we’re underneath the visible surface. Here, energy is transported upward by rising hot gas. Hotter gas rises, cooler gas falls.

32. Radiation Zone: Energy transported upward by photons. More about this later….

33. Core: Energy generated by nuclear fusion ~ 15 million ºC In our Sun, it is the only place with high enough temperature and high enough density to have nuclear fusion occur!

34. Why is the Sun so stable for such a long time? Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity Energy provided by fusion maintains the pressure

35. Think about this: Life on Earth needs a stable Sun in order to survive and evolve. How could the Sun have been so stable for so long? Well, what would happen inside the Sun if the core were to get hotter, and so boost the production of energy from fusion? A. The core would expand and keep getting hotter and hotter. B. The core would expand and then cool. C. The Sun would blow up like a hydrogen bomb.

36. Solar Thermostat Equilibrium Restored Core Temperature Increases So Fusion Rate goes back to normal. Fusion Rate Increases But as it expands, pressure and temp decrease! More pressure from below pushing against gravity, so core expands.

37. What do we mean when we say that the Sun is in gravitational equilibrium? • The Sun maintains a steady temperature. • This is another way of stating that the Sun generates energy by nuclear fusion. • The Sun always has the same amount of mass, creating the same gravitational force. • There is a balance within the Sun between the outward push of heat created by fusion and the inward pull of gravity. • The hydrogen gas in the Sun is balanced so that it never rises upward or falls downward.

38. How does the energy from fusion get out of the Sun?Depends on if the energy is in the radiation zone or the convection zone.

39. Energy Flows Convection Radiation Note that the about a million years for energy to diffuse out of the Sun’s core

40. Solar “Granulation” Blobs on photosphere are where hot gas is reaching surface

41. Sunspots Sunspots occur in pairs; the pairs cluster into groups; and they rotate with the Sun Sunspots come and go over an 11-year cycle.

43. What are sunspots? magnetic field slows down convection; Less heat is transported to surface; so that part of photosphere is cooler

44. Cause: Differential Rotation The Sun does not rotate as a solid body (like the Earth.) The equator rotates faster than the poles. Period of Rotation: 25 days (equator) 30 days (poles)

45. Solar Activity • The photosphere of the Sun is covered with sunspots. • Sunspots are not constant; they appear & disappear. • They do so in a cycle. • It repeats every 11 yrs. • Sun’s magnetic field switches polarity every 11 yrs • so the entire cycle repeats every 22 yrs

47. Sunspot Cycle