-the 1st lecture- Yoshitaka Fujita Osaka University. Snake of March 16-20, 2015

Transcription

1 -the 1st March 16-20, 2015 Yoshitaka Fujita Osaka University Snake of Sizes 1

2 1.4 billion light years 1 fm 量子力学 Quantum Mechanics Molecule ミクロの世界 Micro World ニュートン力学 Newton Mechanics マクロの世界 Macro World The Nature is alive! ( 自然は生きている!) La Clusaz 2

3 地層のでき方 - 小学 6 年理科 - 1) 侵食作用で 土砂が海や湖の底にたまります 2) 時には火山の爆発でも地層ができます 学学研のホームページより The Nature is alive! ( 自然は生きている!) Pushed up from the bottom of the Sea to the top of the Mountain! Explained by Plate Tectonics! La Clusaz 3

4 Continental Drift -Plate tectonics- 225 My ago 200 My ago first idea by Alfred Wegener 150 My ago 65 My ago Present day 現在 Eruption of Kilauea, Hawaii (1970 s) 地熱 : ウラン等 放射性元素の核分裂の熱 Terrestrial heat: originates from Radio Activity like 235 U 4

5 Supernova Cycle Nuclear Chart (Nuclear Landscape) U: Z=92 Proton Z r-process Neutron N 5

6 Layer Structure of Nature (by Glashow) Quark Only Particle Four Forces (Interactions)! 1 fm 1.4 billion light years Conservation Lows are valid! Molecule How things are divided? 10-9 m m m m <10-18 m a molecule into atoms an atom into electrons and a nucleus a nucleus into protons and neutrons a proton and a neutron into quarks how about quarks? 6

7 Powers of Ten 10 のべき乗 first idea by Charles & Ray Eames present photos by B. Bryson (CA, USA) from the web site *starting from the Japanese Tea Garden in San Francisco Let s visit the Micro world Size of the Human being (~1 m) Size of the Quark (100 am = m) m n p f a

8 Scale : 10 0 m (1 辺 1 m) Scale : 10-2 m (1 辺 1 cm) 8

9 Scale : 10-4 m (1 辺 100 m) Scale : 10-6 m (1 辺 1 m) 花粉の上のウイルス 9

10 Scale : 10-7 m (1 辺 100 nm) Scale : 10-8 m (1 辺 10 nm) ウイルス DNA 二重ラセン構造 10

11 Scale : m (1 辺 100 pm) 原子の周りの電子雲 Scale : m (1 辺 1 pm) 11

12 Scale : m (1 辺 10 fm) Size of Nuclei: 1/10 4 of Atoms! to overcome the repulsive force of EM int., a strong nuclear (strong) force is needed! Protons Neutrons in 12 C Snake of Sizes The Layer Structure of Nature (Snake of Uroboros) 12

13 The History of the Universe Big Bang Immediately after the 1st Stars were born, the history of the Nuclear Physics started! How things are divided? 10-9 m m m m <10-18 m a molecule into atoms an atom into electrons and a nucleus a large difference in size here! a nucleus into protons and neutrons a proton and a neutron into quarks how about quarks? 13

14 ***How Do We See Nuclei? Nuclear Chart (Nuclear Landscape) A<300 Proton Z Neutron N 14

15 Neutron Star (Vela pulsar) kg/m 3 (nucleus : kg/m 3 ) Nuclear Chart (Nuclear Landscape) Proton Z stable nuclei: 256 known nuclei: ~2,900 T 1/2 is known: ~2,500 mass is known: ~1,800 unstable nuclei: ~7,000 each nucleus is unique (a large variety!) Neutron N 15

16 Uniqueness of Nuclei Nucleus : Unique Quantum System where 3 interactions out of 4 are active! Strong, Weak, EM (Gravitational force is too weak!) Nucleus : Quantum Finite Many-body System consisting of two Fermions 4-fundamental interactions (forces) Interactions Example Transmitter Strong int.* Nuclear Force Meson* (Gluon) EM int. # Coulomb Force Photon # Weak int.* Beta-decay W-, Z-boson* Gravitational # Apple falls! Graviton # *short-range #long-range *with mass #mass-less 16

17 Long and short-range forces 1-dimentional Universe light distance R no spreading 2-dimentional Universe 1-dim. spread 3-dimentional Universe 2-dim. spread brightness of a star 1/R 2 i.e., inversely prop. to the expansion of the space Scale : m (1 辺 10 fm) Size of Nuclei: 1/10 4 of Atoms! to overcome the repulsive force of EM int., a strong nuclear (strong) force is needed! Protons Neutrons in 12 C 17

18 Energy: Infrared, Visible light, Ultraviolet Einstein s light quantum theory (hypothesis) E = h p = h /c :frequency : wave-lengh & = c/ LED Handy Lump : ~3 ev Color Wave-length Energy Infrared 1,000 nm 1.2 ev Red ~ Yellow ~ Green ~ Blue ~ Purple ~ Ultraviolet ~ Hydrogen atom electron Coulomb Energy Helium Nucleus Proton Z=2, Neutron N=2 proton neutron proton r = m Very much Useful centralized relationship system! We get neutron proton r = m (1 fm) A system made in Harmony (self-consistent)! By solving the Schrödinger eq ev Off course larger! Strong force should be much stronger! 18

19 How are Nuclei defined? *Quantum Finite Many-body system of two Fermions => quantum numbers are important L, S, J, K, T => selection rules of Q-numbers are importnat *Conservation Laws Energy Momentum Angular momentum *Studied by Measuring Decays, Reactions -decay, -decay, Nuclear Reactions ***Elements and Nuclei? 19

20 Elements Necessary for Life large amount needed small amount needed probably needed by Y. Mochizuki ABUNDANCE (Si = 10 6 ) H, He C, O Solar Abundance Fe,Ni solar abundance distribution Solar abundance reflects the Nuclear Structure! MASS NUMBER Ba Pb 20

21 The Big Bang,Big Bang から現在まで the beginning of the Universe 13.7 By ago! Element Necessary for Life by Y. Mochizuki 21

22 Supernova Cycle Temperature T ~ 10 7 K MAJOR FEATURES OF OUR SUN T= ~10 7 K at the core = ~1 kev 22

23 1 H (p) 4 He: Nuclear Reaction in a Star 弱い相互作用が関与する 崩壊 (Weak processes control the reaction rate!) Maxwell distribution velocity <v 2 >=3kT/m kinetic energy <K>=(3/2)kT 10 4 K~ 1 ev 10 7 K~ 1 kev 10 9 K~100 kev 23

24 Mass, Energy, Binding Energy Mass & Energy (Einstein s relationship) E = mc 2 Total energy (mass) of a Nucleus A Z N E T = Z x m p + N x m n - BE *a strongly coupled system has less energy! Element Necessary for Life by Y. Mochizuki 24

25 CNO cycle (catalytic cycle by CNO) start Contributions from Strong Electro-Magnetic and Weak Interactions 4x 1 H +2e are combined +! CNO works as the catalyst CNO cycle (catalytic cycle by CNO) start Only the Weak Interaction can change Elements within the same A! 4x 1 H +2e + CNO works as the catalyst 25

26 Supernova Cycle Temperature T ~ 10 8 K Nucleosynthesis by Y. Mochizuki s-process steller burning r-process Big Bang 26

27 Element Necessary for Life by Y. Mochizuki Onion Structure in a Red Giant 27

28 Can Betelgeuse in Orion be a SN? オリオン座の 1 等星ペテルギウスで 超新星爆発に向かうと見られる兆候が観測されている ( 朝日 2010 年 1 月 ) Betelgeuse: Red Giant in Orion Rigel: Blue Giant in Orion 約 600 光年の距離にあるペテルギウスの表面がでこぼこになっている様子 (NASA) Supernova Cycle 28

29 Element Necessary for Life by Y. Mochizuki Nucleosynthesis by Y. Mochizuki s-process steller burning r-process Big Bang 29

30 Maxwell distribution velocity <v 2 >=3kT/m kinetic energy <K>=(3/2)kT 10 4 K~ 1 ev 10 7 K~ 1 kev 10 9 K~100 kev s are created by pair creation! Crucial Weak Processes during the Collapse mainly by & (A,Z)=nuclei in the Cr, Mn, Fe, Co, Ni region pf -shell Nuclei! K.L &G.M-P Rev.Mod.Phys.75( 04)819 30

31 Layer Structure of Nature (by Glashow) Quark 1.4 billion light years Particle 1 fm Molecule Cycling of Elements Big Bang H, He, Li first generation of (heavy) stars C Fe and some heavy elements SN RG Elements up to U 31

32 Big Bang Cycling of Elements first generation (heavy) stars Red super giant Supernova H, He, Li C Fe, Ni Some heavy elements Elements up to U later generation stars Who am I? Light elements are synthesized in STARS. Heavier Nuclear elements : in Physics Red Giants,! and in Supernovae. They spread at the time of Supernova Explosion. From the Star Astrophysics Dusts, our Earth! was born. Biology! Life was created eventually! Therefore, YOU are the CHILDEN of STARS! 32

33 Who am I? Light elements are synthesized in STARS. Heavier Nuclear elements : in Physics Red Giants,! and in Supernovae. They spread at the time of Supernova Explosion. Astrophysics! From the Star Dusts, our Earth was born. Biology! Life was created eventually! YOU shoulder all the history of the UNIVERSE! ( すべての宇宙の歴史があなたへと続く!) Snake of Sizes 33