surfaces processes ii chemical routes - radboud universiteit · surfaces processes ii chemical...
TRANSCRIPT
Surfaces processes IIChemical routes
François Dulieu
LERMA
Paris Observatory and Cergy Pontoise University
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
Molecules detected in 2002 in astrophysical environments
Surface processes I
Order of magnitudesStickingDesorptionComparison of methods (TPD, RAIRS, STM)
Surface processes IIChemical routes
Surface processes IIIDiffusion on surfaceDiffusion in bulkEnergetic aspects
Studied in lab.
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
“Thermal cold surface Chemistry”, today
And H2O
2 ,
NH
2OH (?), CH
3NH
2 ...
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
H CO O2
O O3
NO C2/3
H4/6
HCN H2
H H2
H2CO
CH3OH
H2O
2
H2O
+
OH+
H2O
2
H2O
+
NH2OH
NO2
CH2NH
CH3NH
2
O OH+
CO2
(?) (O2/O
3 ) C
2/3H
4/6O
OH HCOOHH
2CO
3
CO2
HNO3
+++
H2O
“Thermal cold surface (fast) chemistry”
No bulk chemistryNo irradiation (UV, electrons, Ions...)
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
H CO O2
O NO C2/3
H4/6
HCN H2
H H2
H2CO
CH3OH
H2O
2
H2O
OH NH2OH
NO2
CH2NH
CH3NH
2
O OH CO2
(?) (O2/O
3 ) C
2/3H
4/6O
OH HCOOHH
2CO
3
CO2
HNO3
+++
H2O
“Thermal cold surface (fast) chemistry”
Num
ber
of m
olec
ule
s
Year
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
H2 formation, a world in itself ! (Experiments only...)
On silicatesEfficiencies & process, see numerous Vidali and coworkers, (Cazaux et al)Energetic aspects, Lemaire et al 2010
On carbonaceous materialsEfficiencies & process : Vidali et al, Menella,
Zecho et al, Hornekaer et al …Energetic aspects, S. Price and coworkers
On water Ice :Efficiencies & process : Vidali et al, Amiaud et al 2007, Hornekaer et al 2003, Watanabe et al 2010.Energetic aspects : Hornekaer et al 2003, Congiu et al 2009,
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
CO + H
CO + H HCO
tunnelling
Pirim et al, 2010, J. Phys. Chem. A
H2CO
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
CO H2 H
3 K
10 K
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
CO + H
CO + H HCOtunnelling
Pirim et al, 2010, J. Phys. Chem. A
H2CO H
2COH CH
3OH
Fuchs et al, 2009, A&A
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen II/III
CO + HCO + H HCO
tunnellingH
2CO H
2COH CH
3OH
tunnelling
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Oxygen and Hydrogen experimentsO beam H beam
Ozone
About 20 reactions... + different experimental conditions and methods
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Oxygen and Hydrogen experimentsO beam H beam
Water is easy to form experimentally !
O + H
O2 + H
O3 + H
Water is one of the compound easily formedon cold surfaces (10 - 50K)
Dulieu et al 2010, Vidali et al 2011
Miyauchi et al 2008, Ioppolo et al 2008Matar et al 2008, Oba et al 2009, Ioppolo et al 2010, Cuppen et al 2010
Mokrane et al 2009, Romanzin et al2011
Water formation rate >> CO + H ; CO+OH … > H + H
Water is amorphous and compact (Oba et al 2009, Accolla thesis)
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Experimental agreement ?
3 itemsNo doubt
2 itemsstrong evidences
1 itemweak evidence
No item?
See Dulieu 2011IAU 280
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Water formation (sub monolayer)
O2 + D → OD
O2D + D → D
2O
2
D2O
2+D → D
2O+OD
OD+ D → D2O
No barrier model. The probability of reaction is proportional to the surface concentration of reactants.
O2
HO2
H2O
2 OH
H2O
(D+D is small as longAs other product is present )
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
O2 + D
O3+ D @ 10K
O3 + D @ 45 K
O3 +H → O2 + OHO2 desorb below 45 K
Signal O2
TPD, sub-monolayer regime
Water formation (sub monolayer)
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
O2 + D → O2DO2D + D → D2O2D2O2+D → D2O+ODOD+ D → OD
Signal H2O2
Signal H2O
Signal H2O2
OH + H ?
H2O
2 is almost always < H
2O
O3+ H @ 10K
O3 + H @ 45 K
O2 + H
Water formation (sub monolayer)
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Water formation “Multilayer”
Ioppolo et al PCCP 2010, IR spectroscopy, growing a O
2+ H layers (35 ML)
Much more H2O
2 than H
2O
Low H2O
2 comsuption
Probably H+H → H2
is the most active reaction !
H needs to penetrate through thesample
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Water formation
Can explainMost of the signal,But chemical desorptionIs missing
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Water formation O2
HO2
H2O
2 OH
H2O
Can explainMost of the signal,But chemical desorptionIs missing
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Water formation
- Chemical desorption
- Substrate dependancy
Still to do :
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO + OH reaction on cold surfaces
Photochemistry : CO + OH → CO2 + H
CO + OH on surfaces but “bulk or matrix” conditionsOba et al 2010, Ioppollo et al 2011, Zins et al 2011
© Noble et al 2011
No pure OH beam → in situ control of OH formation
Comparison of surfaces, coverage, temperature andChemical networks
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO + OH reaction on cold surfacesH addition to CO/O2 mixtureOr CO/O3 mixture © Noble et al 2011
CO/O2 + H
Slow
HCO +HH
2CO
CO/HO2 + H
Slow
CO/H2O
2 + H
CO/OH / H2O
+ H
CO/ H2O / H
2O
CO2
+H
CO/O3 + H CO/OH + H
@ 50K
CO / H
2O
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO + OH reaction on cold surfacesO2 and O3 pathways
© Noble et al 2011
CO2 is always a tiny compounds (max 4 %)No important substrate effectKinetics is different starting from O3 and O2
CO/O3 + H
CO/O2 + H
CO2
CO
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO + OH reaction on cold surfacesH addition to CO/O2 mixture
© Noble et al 2011
CO2 is always a tiny compounds (max 4 %)No important substrate effectKinetics is different starting from O3 and O2
CO/O3 + H
CO/O2 + H
CO2
CO
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO + OH reaction on cold surfacesH addition to CO/O2 mixture
© Noble et al 2011
CO2 is always a tiny compounds (max 4 %)No important substrate effectKinetics is different starting from O3 and O2
CO/O3 + H
CO/O2 + H
CO2
CO
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
CO/O2 mixture + H (Ioppolo et al 2011) CO + OH mixture(Oba et al 2010)
From Goumans et al 2008
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
© Congiu et al 2012, ApJ L et soumis a JCP
CO/O2 + H
- IR spectroscopy vs Mass spectroscopy
- Bulk chemistry vs surface chemistry
NH2OH synthesis via NO +H
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
NH2OH synthesis via NO +H
© Congiu et al 2012, ApJ
NO (et éventuellement (NO)2) exposé à H ou D à 10 K disparait
CO/O2 + H
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Synthèse de NH2OH via NO +H
© Congiu et al 2012, ApJ L et soumis a JCP
CO/O2 + H
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
© Congiu et al 2012, ApJ
CO/O2 + H
NH2OH synthesis via NO +H
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
© Congiu et al 2012, ApJ L and submitted to JCP© Fedoroseev et al 2012, submitted to JCP
- IR spectroscopy vs Mass spectroscopy
- Bulk chemistry vs surface chemistry
- "Fast” chemistry vs “slow” chemistry
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
HCN + H
© Theulé et al 2011, A&A
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
C2H4 + O → C2H4O
© Ward & Price 2011, ApJ
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
C2H4 + O → C2H4O
© Ward & Price 2011, ApJ
==
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
“Fast and slow chemistry”Surface and bulk chemistry
© Mispealer, 2012, A&A
Review ofreactions
H+H
CO + H
Water formation
CO2 formation
HCOOH, H2CO3
C2H4O
NH2 -X
conclusion
F- Dulieu – LERMA – Chemistry and Infrared Spectroscopy of Interstellar Dust – June 2012, Nijmegen
Surface, dynamic matrix and bulk chemistry
More and more molecules …
Be carrefull when you compare results.
Surface: competition of fast process - stable products and fast reactions
Matrix dynamically grown : - radicals may survive- “secondary” reactions can happen- can be surface reactions if the reaction are faster than the growth
(T dependant)
Bulk chemistry- driven by slow reorganisation of the ice- in competition with desorption