2. 宇宙的最初三分鐘

3. 宇宙的起源 ? 宇宙是永恒存在的，還是有起始的？

4. 穩恆態宇宙 The Steady-State Theory Quasi-steady state cosmology (QSS)

5. Entropy ( 熵 ) For any closed system Where S is entropy Universe is a closed system

6. 大爆炸假說 (The Big-bang) 宇宙目前約 140 億歲 由一個密度極大且溫度極高的狀態演變 而來的。 在這個起始狀態中，宇宙的物質和能量 的溫度和密度極高。

7. At t<=0 Gravitational singularity Quantum tunnelling

8. Gravitational singularity ( 引力奇點 ) The Big Bang cosmological model at the start of time (t=0). the density of the universe and the curvature of space-time infinite. Predicted in Relativity

9. Quantum tunnelling ( 穿隧效應 ) 宇宙是由 “ 無 ” 誕生的嗎？ 宇宙是從沒有時間、沒有空間、沒有物 質，也沒有能量的 “ 無 ” 開始，因量子力 學的 “ 穿隧效應 ” 而突然誕生的。

10. Fundamental Force Strong interaction Mediator : Gluon Relative Magnitude : 1 Behavior : 1/r 7 Range : 1.4 x 10 -15 m

11. Fundamental Force Electromagnetic interaction Mediator : Photon Relative Magnitude : 1/137 Behavior : 1/r 2 Range : ∞

12. Fundamental Force Weak interaction Mediator : W and Z bosons Relative Magnitude : 10 -13 Behavior : 1/r 5 to 1/r 7 Range : 10 -18 m

13. Fundamental Force Gravitational interaction Mediator : Graviton (perhaps) Relative Magnitude : 10 -39 Behavior : 1/r 2 Range : ∞

14. Planck time (0<t<=10 -43 s) all four fundamental forces were unified and elementary particles did not exist It is meaningless to speak of durations shorter than Planck time there is no generally accepted theory that unifies quantum mechanics and relativistic gravity p.s. 張 sir 話太深

15. T~10 -43 s 10 32 K. No electrons, atoms. matter and antimatter existed in almost equal amounts All but gravitational force were unified

16. Phase Transition Example: ice water steam Phase transition: ice water Phase transition: water steam

17. Phase transitions in the early Universe GUT phase transition: As the temperature drops below ~ 10 29K, GUT force separates into the strong nuclear force and the electroweak force T > 1029K: GUT T < 1029K: electroweak force, strong nuclear force One of the candidates for inflation Other candidates: specifically designed inflaton fields

18. Phase transitions in the early Universe Electroweak phase transition: As the temperature drops below ~ 10 15K, the electroweak force separates into electromagnetism and the weak nuclear force T > 1015K: electroweak force T < 1015K: electromagnetism, weak nuclear force but to moderate a phase transition to trigger inflation

19. GUT Phase transition 10 -35 s < T < 10 -32 s 10 28 K, 10 -25 meters baryonic matter formedbaryonic all that existed during this time were quarks. rapid inflation expanded to nearly 10 +25 meters Strong Nuclear force separated from ElectroWeak force

20. T~ 10 -11 s T~ 10 -11 s the time it takes light to travel half-way across an eraser at the top of a pencil 10 16 K EM-force and Weak force separated

21. T~10 -6 s T~10 -6 s (light travels 3 football fields) 10 13 K cooled enough to form leptons (e.g. neutrinos, electrons) baryons, e.g. protons, neutrons Mesons

22. T~ 1 s 10 10 K not hot enough to form P,N Too hot to form atoms 1000 times hotter than the core of the sun. for every 1000 protons, there were 223 neutrons. free neutrons undergo beta decay

23. T~3 mins 10 9 K light atomic nuclei could form mainly of just one, two, three, or four particles H-1, H-2, H-3, He-3, He-4, Li-7 # of neutrons / # of protons = 0.164

24. Big Bang Nucleosynthesis It only lasted for about three minutes No elements heavier than beryllium formed

25. Reference (Wikipedia) http://zh.wikipedia.org/wiki/%E5%9F%BA%E6%9C%AC%E7 %9B%B8%E4%BA%92%E4%BD%9C%E7%94%A8http://zh.wikipedia.org/wiki/%E5%9F%BA%E6%9C%AC%E7 %9B%B8%E4%BA%92%E4%BD%9C%E7%94%A8 http://en.wikipedia.org/wiki/The_Big_Bang http://en.wikipedia.org/wiki/Static_universe http://en.wikipedia.org/wiki/Steady_state_theory http://en.wikipedia.org/wiki/Quasi-steady_state_cosmology http://en.wikipedia.org/wiki/Fundamental_particles

26. Reference http://en.wikipedia.org/wiki/Fundamental_force http://en.wikipedia.org/wiki/Strong_interaction http://en.wikipedia.org/wiki/Weak_interaction http://en.wikipedia.org/wiki/Electromagnetism http://en.wikipedia.org/wiki/Gravity

27. Reference http://en.wikipedia.org/wiki/Planck_epoch http://en.wikipedia.org/wiki/Cosmic_microwave_b ackground_radiationhttp://en.wikipedia.org/wiki/Cosmic_microwave_b ackground_radiation

28. Reference http://en.wikipedia.org/wiki/Hydrogen http://en.wikipedia.org/wiki/Deuterium http://en.wikipedia.org/wiki/Tritium http://en.wikipedia.org/wiki/Helium

29. References (Articles & Lectures) Errors in the Steady State and Quasi-SS Models: http://www.astro.ucla.edu/~wright/stdystat.htm Astronomy 201 Cosmology - Lecture 41: http://www.aip.de/People/MSteinmetz/classes/Cosmology_ 201/PDF/Lecture_41.pdfhttp://www.aip.de/People/MSteinmetz/classes/Cosmology_ 201/PDF/Lecture_41.pdf History of The Universe : http://home.cwru.edu/~sjr16/advanced/cosmos_history.ht mlhttp://home.cwru.edu/~sjr16/advanced/cosmos_history.ht ml

30. References (Articles & Lectures) 宇宙的起源 http://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/001.htmlhttp://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/001.html 宇宙誕生的最初三分鐘 http://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/002.htmlhttp://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/002.html 宇宙有始無終 http://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/003.htmlhttp://big5.china.com/gate/big5/tech.china.com/zh_cn/scie nce/universe/inside/003.html

31. Reference (Books) 最初三分鐘 大霹靂之後 The First Three Minutes By Steven Weinberg University Physics Sixth Edition By Francis W.Sears, Mark W. Zemansky, Hugh D.Young

32. ~The End~