laboratory chemistry of the outer solar system marla moore nasa/goddard space flight center january...
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Laboratory Chemistry of the
Outer Solar System
Marla MooreNASA/Goddard Space Flight Center
January 28, 2008
Cosmic Ice Lab Cosmic Ice Lab
Polar Gateways Arctic Circle Sunrise 2008, Barrow Alaska
What we do ?Laboratory radiation chemistry of relevant outer solar system ices.
What we need!A good understanding of outer solar system environments, e.g.:
TemperatureRadiation environment
Ice composition of surfaces
Laboratory Chemistry GoalHelp explain observations and predict likely new products yet to
be discovered
50 years ago
Explorer I. January 31, 1958
Temperature – calculated – assuming black bodies T ≈ 300 r -1/2
Radiation environment
Cosmic ray energy spectrum of primary cosmic rays was known
Launch of Explorer I— discovery of Van Allen radiation belts
e.g. Pluto 55 K
50 years agoIce Composition Near-Infrared water-ice feature detected on:
Mars polar capRings of SaturnEuropa and GanymedeSuspected water ice on inner satellites of Saturn
based on reflectivity
Laboratory radiation chemistry
1953 (origin of life study) gas phase mixtures
1957-1960 (rocket fuel?)Frozen free radicalexperiments
1963 ( comets)77 K mixture H2O+CH4+NH3
5 MeV electrons
John Oro
Gerald Kuiper
Some Ice
Environments
KBOs
water
carbon dioxide ammonia
methanenitrogencarbon monoxide
Earth H2O Mars H2O Jupiter Io Europa H2O
Ganymede H2O
Callisto
Saturn Mimas H2O Hyperion
Enceladus H2O Iapetus Tethys H2O Phoebe Dione Titan Rhea Rings H2O Uranus Miranda Ariel
Titania
Umbriel Oberon Neptune Triton Pluto
Earth H2O Mars H2O, CO2 Asteroids H2O, also ice containing a CH IR signature Jupiter Io SO2, SO3, H2S?, H2O? Europa H2O, SO2, SH, CO2, CH,
XCN, H2O2, H2SO4, carbonate salt, hydrous sulfate
Ganymede H2O, SO2, SH, CO2, CH, XCN, O2, O3, hydrated and hydroxylated minerals
Callisto H2O, SO2, SH, CO2, CH, XCN, hydrated and hydroxylated minerals
Saturn Mimas H2O Hyperion H2O Enceladus H2O Iapetus H2O, C, HC, H2S? Tethys H2O Phoebe H2O, CO2, CH,
XCN Dione H2O, C, HC, O3 Titan H2O, C2(CH)2 Rhea H2O, HC?, O3 Rings H2O Uranus Miranda H2O, NH3 hydrate, hydroxylated silicates Ariel H2O, CO2,
OH? Titania H2O, C, HC, OH?
Umbriel H2O Oberon H2O, C, HC, OH? Neptune Triton N2, CH4, CO, CO2, H2O Pluto N2, CH4, CO, H2O, C2H6 Charon H2O, NH3, (NH3 hydrate?) Kuiper Belt Objects H2O seen on some KBOs; NH3 is seen on
Quaoar
*
**
Based onTable 4 from T. Roush, JGR, 2001
*
WaterMethaneAmmonia
Carbon Monoxide Carbon Dioxide
Methane Methyl Alcohol Formaldehyde
Ammonia Formic Acid
Hydrogen Sulfide Hydrogen Cyanide
Acetylene Ethane
Thioformaldehyde Cyanoacetylene
Formamide Methyl Formate Methyl Cyanide
Carbon Disulfide Sulfur Dioxide
Sulfur Monoxide Isocyanic Acid Ethylene Glycol
Radiolysis
Photolysis
/Magnetospheric
How do we study ices in the laboratory ?
Ice at 10 K
Vacuum
Infrared Spectrum
Infrared Light
Laboratory Set-Up
MeV p+10−7 mm Hg
H2O
CO2NH
3
Gas
p+
IR
Spectrometer
UV
Examples
1. H2O2 and sulfur--Europa
2. Fate of methane--Pluto
3. If methanol then sugar ? --Comets
•
EUROPA
10-2
10-2 10-1 100 101 102
Energy MeV
H2O, SO2, SH, CO2, CH,XCN, H2O2, H2SO4, carbonate salt, hydrous sulfate
Laboratory ice studies used to: IDENTIFY
Hydrogen Peroxide on Europa
400800120016002000
-1
0
1
2
3
4
5
65 10 15 20
Wavenumber (cm-1)
Re
lativ
e A
bso
rba
nce
(a) 86 K
(c) 180 K
(e) 210 K
(d) 200 K H2SO4
monohydrate (ref.)
(f) 260 K
Wavelength (m)
(b) 175 K
x 2
x 2.5
x 2
600800100012001400160018002000-1.0
-0.5
0.0
0.5
1.0
1.5
2.0
2.5
3.05 10 15 20
SO2
SO2
SO2-4
HSO-3
HSO-4
Rel
ativ
e A
bsor
banc
e
Wavenumber (cm-1)
H2O + SO2
86 K
SO2
H3O+
(a)
(b)
(c)
(d)
Wavelength (m)
H2O + SO2 Sulfuric acidp+
Laboratory ice studies shows that on Europa
The dashed curve shows the spectrum of a mixture of C2H2:C2H6:CH4 (Sasaki et al., 2005)
PLUTO
N2
CH4-methaneCO
Irradiated methaneforms ethaneand propane
Pluto spectrum
COMETHALE-BOPP
Carbon Monoxide Carbon Dioxide
Methane Methyl Alcohol Formaldehyde
Ammonia Formic Acid
Hydrogen Sulfide Hydrogen Cyanide
Acetylene Ethane
Thioformaldehyde Cyanoacetylene
Formamide Methyl Formate Methyl Cyanide
Carbon Disulfide Sulfur Dioxide
Sulfur Monoxide Isocyanic Acid Ethylene Glycol
H2O + CO, T= 15 K
(~108 yr)
Methanol
~ 10 K
H2Op+
OHOH
C O HCO H2COCH3O
CH2OHCH3OHH H H
HOCH2CH2OHCO2
H2CO3
HCOOH
HCOO
40%
7% 12%
20%
Ethylene Glycol
Discovered in 2002 in the ISM & in Comet Hale-Bopp
in 2004!(Hollis et al., 2000)
(Crovisier et al., 2004)
Methanol
Discovered in the ISM(Hollis et al., 2002)
C C H
OHH
OH
H
H
C C
H
OH
H
H
O
Ethylene Glycol Glycolaldehyde
p+
Looking to the future--------
Room temperature residues
New Tools for Chemical Analyses
HPLC & Detectors MS
Liquid ChromatographyMass Spectrometry
LC-MS
Gas ChromatographyMass Spectrometry
GC-MS
MSGC
New Horizons will reachthe Pluto system in July 2015
The ESA Rosetta spacecraft will reachcomet 67P/Churyumov-Gerasimenko in 2014
•Radiation processing complex molecules, and ions
•Reactions generally understood
•Laboratory work predicts new molecules and ions awaiting detection
SUMMARY
Reggie Hudson
Collaborators
Reggie Hudson
Robert Ferrante
Paul Cooper
Reggie Hudson
Reggie Hudson
Robert Ferrante
Paul Cooper
www-691.gsfc.nasa.gov/cosmic.ice.lab
2 3 4 5 6 7 8 9 10 11 12 13 H H2O NH3 CH4 CH3OH HC(O)CH3 CH3COOH (CH3)2O (CH3)2CO HC9N C6H6 HC11N
CO H2S H2CO SiH4 CH3SH c - C2H4O HC(O)OCH3 CH3CH2OH HOCH2CH2OH CO(CH2OH)2? CSi HCN H2CS CH2NH C2H4 CH2CH(OH) HOCH2C(O)H CH3CH2CN C2H5C(O)H CP HNC C2H2 NH2CN H(CC)2H CH3CCH CH3CCCN CH3C4H CH3(CC)2CN CS CO2 HNCO CH2CO CH3CN CH3NH2 H2C6 HC7N NO SO2 HNCS HCOOH CH3NC CH2CH(CN) H(CC)3H C8H NS MgCN H3O+ HCCCN HC(O)NH2 H(CC)2CN C2H3C(O)H SO MgNC SiC3 HCCNC HCCC(O)H C6H C7H HCl NaCN C3S c - C3H2 HC3NH+ NaCl N2O H2CN l - C3H2 HC4N KCl NH2 c - C3H CH2CN C5N AlCl OCS l - C3H H2COH+ C5H AlF CH2 HCCN C4Si H2CCCC PN HCO CH3 C5 C4H SiN C3 C2CN HNCCC SiO C2H C3O SiS C2O HCNH+ NH C2S HOCO+ OH AlNC C2 HNO CN SiCN HF N2H+ FeO SiNC LiH
c - SiC2
CH HCO+ CH+ HOC+ CO+ HCS+ SO+ H3
+ SH OCN− N2
O2 ?