Unification of Sciences: Astronomy, Physics, and …Unification of Sciences: Astronomy, Physics, and...

Unification of Sciences:Astronomy, Physics, and Chemistry

II

Takeshi Oka

Department of Astronomy and Astrophysicsand Department of Chemistry,

the Enrico Fermi Institute, the University of Chicago

Tokyo Institute of Technology, October 23, 2007

1642

1791

1879

Memorable years

Isaac Newton

Michael Faraday

Albert Einstein

Galileo Galilei

Wolfgang Amadeus Mozart

James Clerk Maxwell

annus mirabilis

1666

1905

Fdt

xdm =2

2

tA

cE

∂∂

−=1

Universal constants

e electric charge

c velocity of light

h Planck’s constant

G gravitational constant

me, mp,…….

electromagnetism

relativity

quantum mechanics

gravity

Chandrasekhar Limit

23

2 ⎟⎟⎠

⎞⎜⎜⎝

⎛=

pp

Chandra

GmcC

mM h

Quantum mechanics

Special relativity

Gravitation

Hydrogenic Species

H+ H2+ H3

+

H H2

H-RadioFUV

FUVIRFIR

IR

re 0.7414 Å

ν 4161.18 cm-1

H2

H3+

re 0.8731 Å

ν1 3178.3 cm-1

ν2 2521.3 cm-1

D0 = 4.478 eV

Proton affinity 4.39 eV

⎟⎠⎞

⎜⎝⎛

aλ

2

∼ 109

1911 Discovery J. J. Thomson

1916 n(H3+) » n(H2

+) Arthur Dempster

1925 H2+ + H2 → H + H3

+ Thorfin Hogness

1961 Interstellar H3+ + , prediction, prediction Earl McDaniel

1973 H3+ + X → H2 + HX+ Herbst, Klemperer, Watson

1975

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

Ubiquity Dense and Diffuse Clouds

Historical Sketch of H3+

T.G.

B.M.

M.G.

+

1970

1996

1980 Oka, PRL. 45, 531Laboratory Spectrum

1996Geballe, Oka, Nature 384, 334

Interstellar H3+, Discovery

H3+

1951 H

H2

H3+ in the (3, 3) metastable level

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

Interstellar chemistry

T ~ 30 Kn ~ 104 cm-3

+-

+

Langevin forcer-5

Tree of Interstellar ChemistryTree of Interstellar Chemistry

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

Herbst & Klemperer, ApJ 185, 505 (1973)

W. D. Watson, ApJ 183, L17 (1973)

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

Differece frequency spectrometer

LiNbO3ν1

ν2

ν1-ν2

N(H3+) ~ 1014 cm-2

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

laboratory

Interstellar space1018 cm 10-4 cm-3

Column density

Vibration-rotation spectrum of H3+

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

0

Ortho

ParaPara

0

2000

4000

6000

8000

10000

12000

14000En

ergy

(cm

-1)

3ν23

4ν22

5ν23

ν2

2ν20

2ν22

3ν21

4ν20

4ν24

5ν21

5ν25

3ν1

3ν1+ν2

3ν1+2ν2

ν1

2ν1

2ν1+ν2

2ν1+2ν2

2ν1+3ν26ν20 6ν2

26ν2

4 6ν26

ν1+ ν2

ν1+2ν20

ν1+2ν22

ν1+ 3ν2

ν1+ 4ν2

The most rigorous test of ab-initio theory

Gottfried, McCall, Oka, JCP 2003

Cencek, Rychlewski, Jaquet, Kutzelnigg(1998) ΔE < 10-6 H ~ 0.2 cm-1

Schiffel, Alija, Hinze (2003)Hyperspherical coordinate

Spectroscopy of fundamental ions

H3+search is on!!

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

Telescope and spectrometer

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

Nature 384, 334 (1996)

4 × 1014 cm-2

6 × 1014 cm-2

First signal!!

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

Surprise!! More H3+ in diffuse clouds

N(H3+) ~ 3.6 ×1012 cm-2 AV

N(H3+) ~ 4.4 ×1013 cm-2 AV

Central Molecular Zone, treasure house of H3+

M ~ 5 ×107 M⊙

Dominantly molecularDense clouds, n(H2) > 104 cm-4

Volume filling factor 0.1Hot gas T ~ 300 KHigh velocity dispersionLow dust temperature T ~ 20-30 K

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

Morris, Serabyn, ARA&A (1996)

CMZ

７:30 pm

Sagittarius

Scorpius

Centaurus

Metastable H3+ !!

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

(3, 3) metastable

Subaru telescope

(1, 1) ground levelCMZ and spiral arms

(3, 3) metastable levelAll CMZ

(2, 2) unstable levelNeither

CO Mostly spiral arms

High temperature

Low density

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

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

Oka, Geballe, Goto, Usuda, McCall, ApJ Oct. 1 (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

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

Treasure hunting

Give an example of unification of concepts or fields.

Do not use cases used in the class.

Include what are unified, who did it and when.

You may use your own research.

Limit 1 page, in English

Send your answer to t-oka@uchicago.edu byNovember 5, electronically as an attachment.