THE PHYSICS AND CHEMISTRY...1 THE PHYSICS AND CHEMISTRY ON THE SURFACE OF COSMIC DUST GRAINS Alexey...
Transcript of THE PHYSICS AND CHEMISTRY...1 THE PHYSICS AND CHEMISTRY ON THE SURFACE OF COSMIC DUST GRAINS Alexey...
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THE PHYSICS AND CHEMISTRY
ON THE SURFACE OF COSMIC DUST GRAINS
Alexey Potapov Laboratory Astrophysics Group of the Max Planck Institute for Astronomy
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2Credit: Lund observatory
The whole sky (by eyes)
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3Credit: Lund observatory
The whole sky (by eyes)
“a lot of stars and black holes” (Jules Verne)
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4Credit: Lund observatory
Molecular clouds
Credit: Nielbock et al. 2012
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Origin of life
Earth
Prebiotic molecules
Interstellar medium
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Credit: Burke & Brown 2010
Structure of dust/ice grains
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Credit: Burke & Brown 2010
HRTEM image of silicate grains (real surface area is unknown) Inset: carbon grains on a KBr substrate (nominal surface area is 1 cm2)
High porosity Large surface
Structure of dust/ice grains
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Credit: Burke & Brown 2010
Cold condensation of dust in dense clouds
Structure of dust/ice grains
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Credit: Burke & Brown 2010
Comet 67P (credit: ESA)
Structure of dust/ice grains
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Structure of dust/ice grains
Dust is physically mixed with ice!
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Thermal desorption of H2O ice
A – integrated band intensity T – temperature v0 – pre-exponential factor = 1012 b – heating rate = 1 K/min N – number of molecules i – desorption order E – desorption energy
dA/dT = v0.1/b.Ni.e-E/RT
H2O
H2O+carbon grains
H2O H2O + carbon grains
Potapov A. et al., ApJ, 2018, 865, 58
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Thermal desorption of H2O ice
Correction factor of 400!
Ice coverage of dust grains in the ISM:1018 molecule cm-2 – 1000 ML / 400 = 2.5 ML
HRTEM image of silicate grains (real surface area is unknown) Inset: carbon grains on a KBr substrate (nominal surface area is 1 cm2)
H2O (130 nm, 400 ML):desorption order = 0 – multilayer desorption
H2O (130 nm, 400 ML) + carbon grains:desorption order = 1 – monolayer desorption
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Cosmic dust grains
Huge number of studies
from simple molecules to amino acids
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- Direct participation of functional groups and atoms in surface reactions
Threefold catalytic effect- A place where molecules can rapidly diffuse and react
- A third body to dissipate the energy released in exothermic bond formations
- Lowering the activation barriers of reactions
Role of dust grains in the chemistry on their surfaces
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Direct participation of dust
A handful of studies
CO2 in H2O ice covering hydrogenated carbon grains by ion irradiation (Mennella et al., 2004)
CO and CO2 in H2O ice covering hydrogenated carbon grains by UV irradiation (Mennella et al., 2006)
CO2 in O2 ice covering atomic carbon foils by UV irradiation (Fulvio et al., 2012)
CO2 in H2O ice covering atomic carbon foils by proton irradiation (Raut et al., 2012)
CO and CO2 in H2O ice covering hydrogenated carbon grains by proton irradiation (Sabri et al., 2015)
CO and CO2 in H2O ice covering graphite films by UV irradiation (Shi et al., 2015)
Formation of CO and CO2
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Direct participation of dust
LabAstro, Jena MONARIS, Paris
+
Amorphous hydrogenated fullerene-like carbon grains
Sample - fixed on a copper mirror at 10 K
High vacuum chamber (10−9 mbar)
Bombardment – 30 minutes, 1.8×1020 atoms cm-2
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Direct participation of dust
Difference IR spectrum before and after O/H bombardment of carbon grains
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Direct participation of dust
A new route of molecules formation in the ISM: grain surface processes
Potapov A., …, Krim L., ApJ, 2017, 846, 131
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Catalytic effect of dust
Some studies
H2 on crystalline silicate films (Pirronello et al., 1997)
H2O on amorphous silicate films (Jing et al., 2011)
H2O on amorphous silicate films (He and Vidali, 2014)
H2 on amorphous silicate grains (Gavilan et al., 2014)
…
Formation of H2 and H2O
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Catalytic effect of dust
FTIR spectrometer
Closed-cycle helium cryostat
Turbopump
FTIR detector
Quadrupole MassSpectrometer
Turbopump
Sample lock
Pressure gauge
Pressure gauge
Gate valve
UV source
Annealing chamber
Rotatable flange
Ion + Non-Evaporable-Getter pump
QMS
FTIR spectrometer
Gas inlet
Gas inlet
UV source
FTIR detector
Cryostat
Sample holder
Ion pump
INterStelar Ice Dust Experiment (INSIDE)
CO2 + 2NH3 → NH4+NH2COO-
Potapov A. et al., ApJ, 2019, 880, 12
UHV chamber (10-11 mbar)
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Catalytic effect of dust
IR spectra taken after the deposition of a NH3:CO2 4:1 mixture on carbon grains at 15 K and after 4 hours of the reaction at 80 K
Time dependences of the NH4+NH2COO- column density
evolved from isothermal kinetic experiments at 80 K
* NH4+NH2COO-
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Catalytic effect of dust
Dependence of the reaction rate coefficients of the CO2 + 2NH3 → NH4+NH2COO-
reaction on the ice thickness for various surfaces
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Catalytic effect of dust
Potapov A., Theule P., et al., ApJL, 2019, 878, L20
Monolayer
Multilayer
Dependence of the reaction rate coefficients of the CO2 + 2NH3 → NH4+NH2COO-
reaction on the ice thickness for various surfaces
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Catalytic effect of dust
- An increased diffusion rate of species
- A formation of an intermediate weakly bound CO2‒NH3 complex that helps to overcome the reaction barrier
- Lowering of the activation barrier of the reaction
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Catalytic effect of dust
- An increased diffusion rate of species?
- A formation of an intermediate weakly bound CO2‒NH3 complex that helps to overcome the reaction barrier
- Lowering of the activation barrier of the reaction
Potapov A. et al., to be submitted
60 65 70 75 80
1,0x10-4
2,0x10-4
3,0x10-4
4,0x10-4
5,0x10-4
6,0x10-4
7,0x10-4
carbon KBr
k (s
-1)
Temperature (K)
0,012 0,013 0,014 0,015 0,016 0,017
-8,8
-8,6
-8,4
-8,2
-8,0
-7,8
-7,6
-7,4
ln(k
)1/T
carbon (activation energy 115 K)
KBr (activation energy 340 K)
CO2
NH3
Hea t
Dust gr ains
CO2
CO2
NH3
NH3
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Role of dust grains in the chemistry on their surfaces
C
Atom bombardment (H + O)
C
C
C
C
CC
C
C
CHydrogenation reactions (as a good example)
H + N CH3NH2
CO2
H + O CH3OH
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4000 3500 3000 2500 2000 1500 1000
0,92
0,96
1,00
O-H stretchingO-H bending
Tra
nsm
issi
on
Wavenumber, cm-1
H2O 200 K
MgSiO3/H
2O
200 K
Si-O stretching
Trapping of water in silicates
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Potapov A. et al., ApJ, 2018, 861, 84 and to be submitted
4000 3500 3000 2500 2000 1500 1000
0,92
0,96
1,00
O-H stretchingO-H bending
Tra
nsm
issi
on
Wavenumber, cm-1
H2O 200 K
MgSiO3/H
2O
200 K
Si-O stretching
Trapping of water in silicates
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Trapping of water in silicates
Trapped water can survive the transition from cold star-forming regions to protoplanetary disks and stay in silicates in the terrestrial planet zone
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Cheers, Xander!