From Quarks to Neutron Stars T. Hatsuda Director RIKEN - - PowerPoint PPT Presentation

From Quarks to Neutron Stars

• T. Hatsuda

Director RIKEN Interdisciplinary Theoretical Science Research Group

OIST Seminar (July 11, 2016)

RIKEN （理研）

・ Largest National Institute in Japan

About 2000 scientists, 9 domestic campuses, 4 overseas branches

・ Founded 1917 ・ Basic researches on Physics, Chemistry, Engineering, Biology, Medical Science

http://www.riken.jp/en/about/ iTHES Wako iTHES Kobe

Interdisciplinary Theoretical Science (iTHES) Research Group

iTHES promotes interdisciplinary collaborations among theorists in fundamental physics, material science, biological science, computational science and mathematics.

iTHES: vertical & horizontal structure

Computational science K computer(AICS) Mathematical science Theory Labs. In RIKEN Physical Science Multi-scale problems in the Universe Life Science Multi-scale Problems in biology Material Science Multi-scale Problems in Condensed matters Advisory expt. Labs. in RIKEN

• T. Hatsuda (RNC)
• E. Hiyama (RNC)
• F. Nori (CEMS)
• A. Furusaki

(ILs/CEMS)

• S. Yunoki (Ils/CEMS/AICS)
• A. Mochizuki (ILs)
• Y. Sugita (ILs/AICS)
• S. Nagataki (ILs)

Ithes-phys Ithes-cond Ithes-bio Ithes-cs

• T. Nakajima (AICS)
• T. Miyoshi (AICS)

Ithes-math

iTHES PIs (Physics, Chemistry, Biology, Computational Science, Mathematics)

• P. Ghosh

Dissipative dynamics & photosynthesis à Kolkata

• N. Iizuka

String theory & Cond. Matter à Osaka

• T. Kanazawa

Nuclear theory & math. science

• N. Yamanaka

Particle theory & Comp. science à FEFU

• S. Wanajyo

Nuclear astrophysics → Sophia U.

• M. Taki
• Math. physics

& meta-materials

• K. Bliokh

Quantum optics & Mathematical phys. à CEMS

• R. Johannsson

Condense matter & Comp. physics àRakuten X.Y.Lu Quantum information &Material design à Huazhong Y.Kamiya Condensed matter & Compt. Physics à RIKEN SPDR

• W. Nishima

Molecular dynamics & bioinformatics à LANL

• K. Uriu

Theoretical biology & collective cellular Behaviors àKanazawa

• I. Yu

Molecular dynamics & system biology

• K. Meda

Applied mathematics & Metabolic network àKansei gakuin Beom Hyun Kim Material science & Compt. physics A.Tanaka String theory & Math. physics

• K. Kyutoku

Astrophysics & Compt. physics

• Y. Yokokura

Black hole & Information theory

• Y. Sakai

Computational biology & particle physics

• M. Hongo

Nuclear physics & Statistical mechanics

• K. Uchinomiya

Mathematical biology & statistical mechanics

iTHES連携研究者~ 50

• T. Oyamada

Quantum Chemistry & Comp. Science

iTHES Junior Researchers (recruited internationally)

• X. Plat
• Cond. math

& Comp. Science

• G. Baym (UIUC)

physsics

iTHES Senior Fellow

• F. Marchesoni (INFN)

astrophyiscs

• K. Aihara (U. Tokyo)

applied mathematics

• C. Beauchemin( Ryerson)

biology

In 2013, he (Tetsuo Hatsuda) joined the RIKEN research institute in Wako, Japan, and launched an interdisciplinary team of theoretical physicists, chemists and biologists to work out techniques that will accelerate all three fields. He hopes that the effort will stimulate more interdisciplinary work in the country. He says. “Theoretical science is a good starting point because it is easy for us to interact.” iTHES project reported in NATURE

From Quarks to Neutron Stars

Big Bang Universe

Standard Model of Elementary Particles

Dark Energy

Expanding Universe and Evolution of Matter

2700 K 1010 K 1012 K BIG BANG

Galaxy 1023[cm]

We are made of elementary particles

1012[cm] Solar system 102[cm] Human DNA 10-7 [cm] Atom 10-8 [cm] 10-13 [cm] Proton/Neutron < 10-17 [cm] 10-12 [cm] Nucleus

Known Elementary Particles Matter particles (spin=1/2) Gauge fields (spin=1)

Higgs field (spin=0)

Quarks Leptons Strong force EM force Weak force I II III

gluon photon

W-boson Z-boson e-neutrino electron mu-neutrino tau-neutrino muon tau

up down charm strange top bottom

nucleus r ～10 [fm] =10-12 [cm] r ～1 [fm]=10-13 [cm] r ～10 [km] Neutron star nucleon

Quantum Chromo Dynamics (QCD)

Fundamental theory for matter -

Light quarks

mu ~ 2 MeV md ~ 5 MeV ms ~ 90 MeV Heavy quarks mc ~ 1.3 GeV mb ~ 4.2 GeV mt ~ 171 GeV

I II III Characteristic strong int. scale ~ (1fm)-1 ~ 200 MeV Fundamental theory of strong int. ＝ Quantum Chromo Dynamics (QCD)

• M. Kobayashi
• T. Maskawa
• Y. Nambu

QCD = SU(3) quantum gauge theory for color charges （B, R, G)

• Y. Nambu

(1921-2015)

Key “quantum” aspect of QCD

• - Anti-screening of color charges --

Quark Confinement Asymptotic freedom

Millennium Problems by Clay Mathematics Institute (May 24, 2000)

Quark Confinement – Mathematical Challenge --

http://www.claymath.org/millennium-problems

• 1. Yang–Mills and Mass Gap
• 2. Riemann Hypothesis
• 3. P vs. NP Problem
• 4. Navier–Stokes Equation
• 5. Hodge Conjecture
• 7. Poincaré Conjecture
• 8. Birch and Swinnerton-Dyer Conjecture

Official description of Problem1 (A. Jaffe and E. Witten)

Lattice QCD

• - a clue to attach the challenge --
• well defined statistical system (finite a and L)
• gauge invariant
• fully non-perturbative

Monte Carlo simulations

• n supercomputers

quarks q

• n the sites

gluons Uμ

• n the links

L a

4-dim. Euclidean Lattice

• K. Wilson

(1936-2013)

Quark Confinement from Lattice QCD simulations V(r)

How atomic nucleus is formed ?

Original question asked by H. Yukawa (1935) Modern question to be answered from quarks & gluons

How atomic nucleus is formed ?

Original question asked by H. Yukawa (1935) Modern question to be answered from quarks & gluons

Ishii, Aoki, Hatsuda (2007)

Nuclear Force from QCD

石井理修 青木慎也 初田哲男

iPS Cell

山中伸弥 高橋和利

MEXT HPCI Program (2011-) Field 1 – Field 5

Nuclei Neutron star Proton & Neutron Proton accelerator J-PARC （KEK-JAEA） Rare Isotope factory RIBF （RIKEN） Gravitational wave detector KAGRA （U. Tokyo）

K computer (RIKEN)

QCD simulations Nuclear simulations Neutron star simulations R ~ 10-13 cm R ~ 10-12 cm R ~ 10 km

・ M～(1-2)M☉ ・ R ～10km ・ 0 < ρ < 10 ρ0 composition

・ nuclei ・ neutrons & protons ・ mesons (π, Ｋ) ・ hyperons (Λ, Σ-, Ξ-) ・ quarks (u,d,s) + leptons (e, μ)

Neutron Star as a giant nucleus

１９３２ Discovery of the neitron

• J. Chardwick

１９６８ Discovery of pulsar S. J. Bell and A. Hewish

Short history of NS obs.

１９７４ Discovery of binary neutron star R. A. Hulse and J.H. Taylor １９３４ Prediction of neutron star W. Baade and F. Zwicky (２０１Ｘ Discovery of gravitational wave from NS merger ） １９７９ Discovery of ＳＧＲ（magnetar？） １９８２ Discovery of millisecond pulsar D. Backer et al. ２０１０ Discovery of massive neutron star P. Detmorest et al. ２０１０ CAS-Ａ cooling curve C.O.Heinke and W.C.G.Ho ２０１6 Discovery of gravitational waves from BH merger (LIGO)

Neutron Star in Okinawa

Basic equations for neutron star

• 1. Tolman-Oppenheimer-Volkoff equationß General Relativity

(TOV）

• 2. Equation of state P=P(ε) ß Strong Int. (QCD)

EM int. （charge neutrality） Weak int. （β equilibrium）

(EOS）

Schematic Mass-Radius relation

From Yagi, Miake and Hatsuda, “Quark-Gluon Plasma”, Cambridge Univ. Press (2008)

・ M～(1-2)M☉ ・ R ～10km ・ 0 < ρ < 10 ρ0 composition

・ nuclei ・ neutrons & protons ・ mesons (π, Ｋ) ・ hyperons (Λ, Σ-, Ξ-) ・ quarks (u,d,s) + leptons (e, μ)

Neutron Star as a giant nucleus

Attractive Bose-Fermi Mixture

Quark-Gluon Plasma

〈qq〉 〈qq〉

chiral superfluid ⇔ color superconductor

QCD Phase diagram

⇔

Fermi-Bose mixture Induced superfluid

Quantum Simulation of QCD Matter by Cold Atoms ?

• K. Maeda, G. Baym & T. Hatsuda, Phys.Rev.Lett.103 (’09); Phys. Rev. A87 (2013)

K computer @RIKEN 10.51 PFLOPS, 705,024 CPU Cores

• T. Takiwaki

(iTHES Associate) World’s first successful supernova explosion in 3D simulation with neutrino transport (2013)

1000 km Club Nebula

Birth of NS : Supernova Explosion

NS merger à Gravitational wave

distance [km] neutrino energy density [log erg/cc]

Gravitational Wave Detectors (e.g. KAGRA)

Kyutoku (iTHES fellow) et al, PRL 107 (2011); PTEP (2013) hard EOS soft EOS

distance [km] neutrino energy density [log erg/cc]

NS merger à Origin of elements

mass number mass number abundance 50 100 150 200 250 10-8 10-7 10-6 10-5 10-4 10-3 10-2 mass-averaged solar r-abundance

Wanajo （ithes fellow) et al., Ap.J. Lett. 789 (2014) L39

First nuleosynthesis study based on Full 3D general relativistic simulations With neutrino transport.

Gravitational force Strong force Weak force Electromagnetic force TOE ? Grand Unified Theory Electro

• Weak

Theory NOW (2015) Newton Yukawa Fermi Maxwell Weinberg Nambu Einstein

Unification of forces

Fundamental questions in 21th physics

4．Extra dimensions

• 5. Quantum gravity

…

• 1. Matter under Extreme Conditions
• 2. Origin of Dark Matter
• 3. Origin of Dark Energy

Thank you !