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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