Ion chemistry and N-containing molecules in Titan’s upper ...
Formation of complex molecules after cosmic ion ......Formation of complex molecules after cosmic...
Transcript of Formation of complex molecules after cosmic ion ......Formation of complex molecules after cosmic...
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Formation of complex molecules after cosmic ion bombardment and
UV photolysis of interstellar ice analogues
Maria Elisabetta Palumbo
INAF – Osservatorio Astrofisico di Catania
http://www.oact.inaf.it/weboac/labsp/index.html
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Energetic processing in dense molecular clouds
Interaction of cosmic rays with molecular clouds
low-energy cosmic rays UV photons
High density and high extinction stellar radiation does not penetrate molecular clouds
E = keV - MeV E = 6.9-13.6 eV
electrons
E = keV
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Energetic processing in the Solar System
Energy Fluxes (cm-2 s-1)
Solar Photons 2 eV Visible 2.0·1017
4 eV NUV 1.5·1016
6 eV FUV 3.0·1013
Solar Wind (1 AU)
1keV H+ 3.0·108
4keV He2+
Solar Flares (1 AU)
>1 MeV H+ 1010 (cm-2 yr-1)
>1 MeV He2+
Galactic cosmic rays
>1 MeV H+ 1-10
>1 MeV He2+
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Interaction of ions with matter
1 MeV protons on H2O
J.F. Ziegler: SRIM (Stopping and Range of Ions in Matter); TRIM (TRansport of Ions in Matter)
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Interaction of ions with matter
J.F. Ziegler: SRIM (Stopping and Range of Ions in Matter); TRIM (TRansport of Ions in Matter)
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IR and Raman spectroscopy
Palumbo M.E., Ferini G., Baratta G.A., 2004, Adv. Sp. Res. 33, 49
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Effects of energetic processing
keV-MeV ions
UV photons frozen gases
Sputtering Structural Chemistry Implantation Residue
changes
Laboratory experiments
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H2O:CO
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H2O:CO
Mixture after processing
H2O:CO:CO2:H2CO:CH3OH = 100:15:15:1.5:1.5
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CH3OH
Modica and Palumbo 2010, A&A 519, A22
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Formation rates
R(0) = 6.2 × 10-18 s-1
Occhiogrosso, A., Viti, S.,
Modica, P., Palumbo, M.E.
2011, MNRAS 418, 1923
0 = 3 × 10-17 s-1
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CH3OH at 10 K
New bands observed during the
photolysis of CH3OH at 10 K
Gerakines et al. 1996, A&A 312, 289
Munoz Caro and Schutte 2003, A&A 412, 121
Oberg et al. 2009, A&A 504, 891
Islam et al. 2014, A&A 561, A73
UV photolysis
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CH4 + 60 keV Ar++ at 12 K
Baratta et al. 2003, NIMB 209, 283
The intensity of CH4 bands decreases.
Other bands appear assigned to
ethane, propane, ethylene, acetylene
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Formation of linear carbon chains
Compagnini et al. 2009, Carbon 47, 1605
Puglisi et al. 2014, NIMB 326, 2
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Formation of linear carbon chains
Compagnini et al. 2009, Carbon 47, 1605
Puglisi et al. 2014, NIMB 326, 2
From the peak position, the
chains involved should
contain 8-12 carbon atoms
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Formation of formamide (NH2CHO) and isocyanic acid (HNCO)
Studied mixtures
H2O:CH4:NH3 = 1:1:1 + 200 keV H+
CH3OH:N2 = 1:1 + 200 keV H+
H2O:CH4:N2 = 1:1:1 + 30 keV He+
H2O:CH4:N2 = 1:2:1 + 30 keV He+
H2O:CH4:N2 = 1:2:10 + 30 keV He+
H2O:CH4:N2 = 1:2:100 + 30 keV He+
Kanuchova Z., Urso, R.G., Baratta, G.A, Brucato J.R., Palumbo M.E., Strazzulla G. 2016, A&A 585, A155
See poster presented
by Riccardo Urso
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Formamide (NH2CHO)
Brucato, Baratta, Strazzulla, 2006, A&A 455, 395
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HNCO
Kanuchova Z., Urso, R.G., Baratta, G.A, Brucato J.R., Palumbo M.E., Strazzulla G. 2016, A&A 585, A155
Formation of formamide (NH2CHO) and isocyanic acid (HNCO)
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Formation of formamide (NH2CHO) and isocyanic acid (HNCO)
Experimental results
after dose = 10 eV/16u
NH2CHO/nitrogen ~ 10-2
HNCO/nitrogen ~ 10-3
Nitrogen cosmic abundance ~ 2x10-5
Assuming high N-depletion
NH2CHO fractional abundance ~ 10-7
comparable to observed values
HNCO fractional abundance ~ 10-8
lower than observed values
Kanuchova Z., Urso, R.G., Baratta, G.A, Brucato J.R., Palumbo M.E., Strazzulla G. 2016, A&A 585, A155
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Formation of formamide (NH2CHO) and isocyanic acid (HNCO)
While the observed amount of
formamide can be accounted for by
cosmic-ray bombardment of icy
grain mantles, other processes
(such as gas-phase and grain-
surface reactions) have to be
invoked to explain the observed gas-
phase abundance of HNCO.
Kanuchova Z., Urso, R.G., Baratta, G.A, Brucato J.R., Palumbo M.E., Strazzulla G. 2016, A&A 585, A155
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Formation of formamide (NH2CHO) Result
The hydrogenation of HNCO does not produce
detectable amounts of formamide
The major conclusion of this Letter is that there is no need
to invoke grain-surface chemistry to explain the presence of
formamide provided that its precursors, NH2 and H2CO, are
available in the gas phase
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Infrared and Raman spectroscopy of residues
T=300 K
Strazzulla, Baratta, Palumbo 2001, Spectrochim. Acta A 57, 825
Palumbo, Ferini, Baratta, 2004, Ad Sp Res 33, 49
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Infrared and Raman spectroscopy of residues
T=300 K
500 1000 1500 2000 2500 3000 3500
200
800
1000
1200
C
C
Si
Si
T=300 K
+1.91015
30 keV He+/cm
2
residue from H2O:CH
4:N
2
Inte
nsity (
c.p
.s.)
Raman shift (cm-1)
1000 1500 2000
0
100
200
300
G
D
H2O:CH
4:N
2 +30 keV He
+ at 12 K
T=300 K
G=1539 cm
-1
FWHMG=197 cm
-1
D=1328 cm
-1
FWHMD=351 cm
-1
ID/I
G=0.74
Inte
nsity (
c.p
.s.)
Raman shift (cm-1)
Ferini G., Baratta G.A., Palumbo M.E., 2004, A&A 414, 757
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Ultra Carbonaceous Antarctic micrometeorites probing the Solar System beyond the nitrogen snow-line
Dartois et al. 2013, Icarus 224, 243
Baratta et al. 2015, Planet. Space Science, 118, 211
CN
C-H
N-H
C=C
C=N
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Comet Wild2 grains collected by Stardust
Rotundi A., Baratta G.A., … Brucato J.R., … Colangeli L., … Ferrini G., … Mennella V., … Palumbo
M.E., et al. Meteoritics & Planetary Science 2008, 43, 367
The most disordered amorphous carbon detected by Raman spectroscopy in some Stardust grains could be indicative of ion irradiation of carbon containing ices or of pre-existing more ordered carbons.
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Summary
Molecules formed in the solid phase are
released to the gas phase after desorption of
ice mantles or are incorporated in planets,
satellites and comets
cosmic
ions
UV photons
Energetic processing
modifies the chemical
composition of icy grain
mantles;
gives a significant contribution
to the formation of complex
molecules in the solid phase.
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Acknowledgments
Mario Accolla Giuseppe Baratta Giuseppe Compagnini Saro Di Benedetto Vincenzo Greco Zuzana Kanuchova Carlotta Scirè Giovanni Strazzulla Riccardo Urso