Unification of Sciences: Astronomy, Physics, and Chemistry I · PDF fileUnification of...

Unification of Sciences:Astronomy, Physics, and Chemistry

ITakeshi Oka

Department of Astronomy and Astrophysicsand Department of Chemistry,

the Enrico Fermi Institute, the University of Chicago

Tokyo Institute of Technology, 10:40 – 12:10, October 16, 2007

http://Fermi.uchicago.edu/http://Fermi.uchicago.edu/~oka/FTP

Experiments, Observations

Empirical rule

Fundamental theory

PV = nRTPV T= nR1662 Boyle1778 Charles

1811 Avogadro

Thermo Dynamics

The Ideal Gas Law

1802 Gay-Lussac

1860 Cannizzaro

273 K

Boltzmann

Battery 1800

Alessandro Volta1745 - 1827

Luigi Galvani

Unification of Concepts

Electricity

Michael Faraday

Electromagnetism Light

Electricity Chemistry

Electrochemistry

Electricity Gravity×

Ion, cation, anion, cathode, anode,electrode, electrolysis,…

Magnetism

James Clerk Maxwell1791 - 1867

1831 - 1879

• I have long held an opinion, almost amounting to conviction, in common I believe with many other lovers of natural knowledge, that the various forms under which the forces of matter are made manifest have one common origin; or, in other words, are so directly related and mutually dependent, that they are convertible, as it were, one into another, and possess equivalents of power in their action.

• Action of magnets on light Michael FaradayPhilosophical Transactions, 1846, p. 1

Molecule, Ion, Gas. Liquid. Salt, Solution, Colloid, Crystal, Steel, Glass, Force, Motion, Electricity, Magnetism, Electrolysis, Light, Field, Discharge.

A P C B

Johannes Kepler Galileo Galilei

Friedrich Wöhler

Synthesis of urea, 1828

Unification of Fieldｓ

Isaac Newton 1666

A P C B

Statistical thermodynamics

Quantum mechanicsWillard Gibbs

Physics and Chemistry

PV = nRTPV T= nR1662 Boyle1802 Gay-Lussac1811 Avogadro

Thermo Dynamics Chemistry

A P C BSpectroscopy

X-ray Crystallography,……

Joseph von Fraunhofer1787 – 1826

Approximavit Sidera

"The most remarkable discovery in all of astronomy is that the stars are made of atomsof the same kind as those on the earth."

Feynman Lectures on Physics I, 3-6 (1963)

Astronomy, Physics, and Chemistry

1814

A P C B

P

CA B

P

C

BA

Who discovered H3+ ?

1766 Henry Cavendish

1861 Anders Ångstrom

1911 J. J. Thomson

1913 Niels Bohr

1928 堀 健夫

1935 Charles Coulson

1980 岡 武史

1967 Gerhard Herzberg

Discovery of Hydrogen

Spectrum of H

Discovery of H3+

Theory of H

Analysis of H2 spectrum

Theory of H3+

Search for H3+

Spectrum of H3+

Astronomy Chemistry

Nuclear fusion

Ion – neutral reactions H３＋

Star, Galaxy, Universe Atom, Molecule, Matter

H → He → C, N, O, Ne, Mg, Si, S,…..Fe…

Star ← Molecular cloud

Interstellar chemistry

HCO＋

William Klemperer

Star formation

Formation of molecules Star

Diffuse cloud

Dense cloud

H3+

kTE

e−

Collision Spontaneous emission

Astronomers’ Periodic Table

Ben McCall

He

C N O Ne

Si S ArMg

Fe

Molecules everywhere

CO

HC5NHC7NHC9N

●

Ungerechts & Thaddeus, ApJS 63, 645 (1987)

Plasmas everywhere

Cosmic Ray 0.6 primary particles cm-2s-1

H2 → H2+ + e- ζ[H2] ζ ~ 10-17s-1

H2 H2e

-H -H

H2+ + H2 → H + H3

+ kL[H2][H2+]

H3+ + O → OH+ + H2 kL[H3

+][O] kL~ 10-9 cm3 s-1

OH+ → H2O+ → H3O+ → H2O

O + H2 → OH + H

1975 H–C≡C–C≡C–C≡N H–C≡C–C≡C–C≡C–C≡N

H–C≡C–C≡C–C≡C–C≡C–C≡N

C60

H3+

H2

H2+

CH3+

CH5+

CH4

C H2 3+

C H2 2

C H3+

C H3 3+

C Hm n

CH+

CH2+

N H2+

HCO+OH+H O2

+H O3

+H O2

OH

C H CNH2 5+

CH CNH3+

CH NH3 2+

H CN2+

HCN

CH NH3 2

CH NH2

CH CN3

C H CN2 5

CH

CH CO3+

CH OH3 2+

CH CO2

CH OH3

H COC H OH

CH OCH

2

2 5

3 3

C H2 5+

C H2 4

H C O2 3+

C O3

C H2

H C N3 3+

HC N3

HC N5

HC N7

HC N9

HC N11

C H3

C4+

C H4+

C H4 2+

C H4 3+

C H4

C H3 2

cosmic ray

H2N2

COO

H2

H2

e

e

e

ee

e

e

N

NH3

HCN

CH CN3

e

COH O2

CH OH, e3

C

H2

H2

H2

e

eCH3

+e

e eHCN

C+

e

C+

H2

e eC

+

H2H2

e

CO

C

H

+

e

e

Ar+ laser Dye laser

Ar+ laser

Difference frequency spectrometer A. Pine

LiNbO3ν1

ν2

ν1-ν2

N(H3+) ~ 1014 cm-2

L 103 cm n(H3+) 1011 cm-3

Lab

Interstellar space1018 cm 10-4 cm-3

Column density

H3+ Vibration – rotation infrared spectrum

T. Oka, Phys. Rev. Lett. 45, 531 (1980)

0

Ortho

ParaPara

thermometer

densitometer

基礎的なイオン分子

FHFー

CCCCCCHー

H3+ Search is on!!

Less than one year after first line was seen in laboratory!!!

Telescopes and spectrometers

UKIRT 3.8 m CGS4 8 km s-1 Mauna Kea 1982Subaru 8.2 m IRCS 15 km s-1 Mauna Kea 2000Gemini South 8 m Phoenix 5 km s-1 Cerro Pachon 2003VLT 8 m CRIRES ≤3 km s-1 Cerro Paranal 2006

H3+ emission from Jupiter

Maillard, Drossart, Watson, Kim, CaldwellApJ 262, L37 (1990)

Connerney, Satoh Phil. Trans.R. Soc. Lond. 358, 2359 (2000)

Magnetohydrodynamic plasma of Jupiter

Io, Volcano

H3+ aurora

H3+ aurora

Nature 384, 334 (1996)

4 × 1014 cm-2

6 × 1014 cm-2

やっと見つかった

単純な星間 H3+の化学

)()()( 2

3 COnHn

kHn

L

ζ=+

生成 H2 → H2+ + e H2

+ + H2 → H3+ + H 速度 = ζn(H2)

分解 濃い雲 (104 cm-3) H3+ + CO → H2 + HCO+ kLn(H3

+)n(CO)

薄い雲 (102 cm-3) H3+ + e- → H + H + H ken(H3

+)n(e)

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

103

104

105

106

n(X

)

10-1100101102103104105106

n(H)

Dense Clouds Diffuse Clouds

H2

HCO

C+H3

+

ζ

)()()( 2

3 enHn

kHn

e

ζ=+

kL ~ 10-9 cm3/s ke ~ 10-7 cm3/s

1.01

1.00

0.99

0.98

0.973.6693.6683.667

Wavelength (µm)

3.7173.7163.715

R(1,1)uR(1,1)l

R(1,0)

N(H3+) ~ 3 × 1014cm-2

111025

214

141516617 5

31222918

27

2619237824

21

H3+ in Diffuse Clouds!!

Cygnus OB2 No 12 HD 183143

1.01

1.00

0.99

0.98

0.973.7173.7163.7153.6693.6683.667

Wavelength (µm)

R(1,1)u

R(1,1)l

R(1,0)

V = 11.48

V = 6.86

Geballe, McCall, Hinkle, Oka, ApJ 510, 251 (1999) McCall et al. ApJ 567, 391 (2002)

6

5

4

3

2

1

0

H3+ C

olum

n D

ensi

ty (1

014cm

-2)

50403020100

E(B-V) (mag)

AFGL2136

W33A

MonR2 IRS 3

AFGL961E

AFGL490

AFGL2591

8

6

4

2

0

H3+ C

olum

n D

ensi

ty (1

014cm

-2)

6543210

E(B-V) (mag)

ζ OphP Cygni

HD 183143

WR 118

Cyg OB2 12

WR 104

Cyg OB2 5

WR 121

HD 168607

HD 194279

GC IRS 3

χ2 Ori

HD 20041

Dense clouds

McCall, Geballe, HinkleOka, ApJ 522,338(1999)

Diffuse clouds

McCall, Hinkle, Geballe, Moriarty-Schieven, Evans,Kawaguchi, Takano, Smith, Oka, ApJ 567, 391 (2002)

ζ Per

H3+ は薄い雲のほうに沢山ある!!

N(H3+) ~ 3.6 ×1012 cm-2 AV

N(H3+) ~ 4.4 ×1013 cm-2 AV

薄い雲の中の宇宙線は一桁強い

)()()( 2

3 COnHn

kHn

L

ζ=+

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

103

104

105

106

n(X

)

10-1100101102103104105106

n(H)

Dense Clouds Diffuse Clouds

H2

HCO

C+H3

+

ζ

)()()( 2

3 enHn

kHn

e

ζ=+

kL ~ 10-9 cm3/s ke ~ 10-7 cm3/s

濃い雲

薄い雲

Central Molecular Zone

Morris, Serabyn, ARA&A (1996)CMZ

OH, H2CO, CO, CS, NH3, HCN

Mezger, Duschl, Zylka, A&A Rev. (1996)

H3+

R(1, 1)u R(1, 0)

Geballe Phil. Trans. RSL A358, 2503 (2000)

: H3+ の宝庫

７:30 pm

1:30 am

(1, 1) ground levelCMZ and spiral arms

(3, 3) metastable levelAll CMZ

(2, 2) unstable levelNeither

CO Mostly spiral arms

High temperature

Low density

GCS 3-2, the brightest Quintuplet star

J

K32.9 K

361 K

(J, K)

H3+の理想的な回転準位

+para I = 1/2

(3, 3) metastable level

(1, 1) ground level

ortho I = 3/2

Δk = ± 3 forbidden transitions

27.2 days (2, 2) unstable level

Pan & Oka, ApJ 305, 518 (1986)

(1, 0)

Oka & Epp, ApJ 613, 349 (2004)0 ±1 ±2 ±3 k

Ncrit ~ 200 cm-3

H3+ + H2 → (H5

+)* → H3+ + H2

準安定回転状態にある H3+の発見

Goto, McCall, Geballe, Usuda,Kobayashi, Terada, OkaPASJ, 54, 951 (2002)

(3, 3) metastable

後藤美和、臼田知史

小林直人，寺田宏

すばる望遠鏡

The Expanding Molecular RingKaifu, Kato, Iguchi, Nature (1972)Scoville, ApJ (1972)

Whiteoak, Gardner, MNRAS (1979)

Scoville ApJ 175, L127 (1972)

Nagata, Hyland, Straw, Sato, Kawara, ApJ 406, 501 (1993)

Four categories of gas

Cold

Cold 30 K ≥ 104 cm-3 0.1 CO, CS, NH3

Warm 250 K 102 cm-3 0.5 – 1 H3+

Hot 104 K 102 cm-3 0.5 Radio scattering

Ultrahot 107~8 K 0.3 cm-3 «1 X-ray

T n f

Yusef-Zadeh ApJ 637, L101 (2006)

Dust ≤ 30 K

0.01

2005 Hot and Diffuse Clouds near GC Probed by Metastable H3+

Oka, Geballe, Goto, Usuda, McCall, ApJ 632, 883 (2005)

1998 – 2002 Ubiquity, Dense and Diffuse CloudsMcCall, Geballe, Hinkle, Oka

1980 Oka, PRL. 45, 531Laboratory Spectrum

1996Geballe, Oka, Nature 384, 334

Interstellar H3+, Discovery

1989 - 95

2002 Metastable H3+, Discovery

Goto, McCall, Geballe, Usuda, Kobayashi, Terada, OkaPASJ, 54, 951

1975

2006 Interstellar H3+, Oka, Proc. Natl. Acad. Sci. 103, 12235 (2006)

道程

Interstellar Space

Dense (molecular) cloudsDiffuse clouds New class of clouds?

Galactic Center

Expanding molecular ringGalactic nucleus New class of clouds?

Extragalactic Object

Obscured AGN Magellanic cloudsCircumstellar Space

Planetary nebulae protoplanetary nebulaePlanet

Planets Proto-planet Exo-planet

宝探し, Treasure hunting

H3+

H2+

CH3+

CH5+

CH4

C H2 3+

C H2 2

C H3+

C H3 3+

CH+

CH2+

N H2+

HCO+OH+H O2

+H O3

+H O2

OH

C H CNH2 5+

CH CNH3+

CH NH3 2+

H CN2+

HCN

CH NH3 2

CH NH2

CH CN3

C H CN2 5

CH

CH CO3+

CH OH3 2+

CH CO2

CH OH3

H COC H OH

CH OCH

2

2 5

3 3

C H2 5+

C H2 4

H C O2 3+

C O3

C H2

H C N3 3+

HC N3

HC N5

HC N7

HC N9

HC N11

C H3

C4+

C H4+

4 2

C H3 2

cosmic ray

H2N2

COO

H2

H2

e

e

e

ee

e

e

N

NH3

HCN

CH CN3

e

COH O2

CH OH, e3

C

H2

H2

H2

e

eCH3

+e

e eHCN

C+

e

C+

H2

e eC

+

H2H2

CO

C

+

e

e

Protonated Acetylene C2H3+

Bond Breaking Tunneling

J. A. Pople 1972

(1, 1) ground levelCMZ and spiral arms

(3, 3) metastable levelAll CMZ

(2, 2) unstable levelNeither

CO Mostly spiral arms

High temperature

Low density

Help!!! Theory of H3+ recombination

badly needed.A spectrum is haunting the field of dissociativerecombination, the spectrum of H3

+ in the diffuse interstellar medium………………….Astronomers, physicists and chemists of the world, unite!!!

H3+ + e- → H3* → H + H + H

McCall et al. Nature, 422, 500 (2003), Phys. Rev. A70, 052716 (2004)

Kokoouline, Greene Phys. Rev. Lett. 90, 133201 (2003)Phys. Rev. A68, 012703 (2003)

田代基慶、加藤重樹