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 [email protected] byNovember 5, electronically as an attachment.
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