ice physics i: comets · 2005-01-20 · comets, asteroids bring water & organics to earth the...
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Ice Physics I:Ice Physics I:CometsComets
Karen Karen MeechMeechSession # 24 Session # 24 –– Mon 1/17/05 Mon 1/17/05
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Temperature ScalesTemperature Scales
Kelvin Kelvin –– absolute scale absolute scale –– atomic motion atomic motion C = 5/9 (F C = 5/9 (F –– 32) 32) K = C + 273K = C + 273
100100373373273273KelvinKelvin
10010010010000CentigradeCentigrade1801802122123232FahrenheitFahrenheit
ΔΔTTHH22O BoilO BoilHH22O FreezeO FreezeScaleScale
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Water Water –– Features Relevant to Ice Features Relevant to Ice
Bent molecule (104.52Bent molecule (104.52oo) ) –– H Bond H Bond Dipole momentDipole moment Tetrahedral Crystal structureTetrahedral Crystal structure Expands upon freezing (less dense)Expands upon freezing (less dense)
Negative slope on melting curveNegative slope on melting curve Le Le ChatlierChatlier Principle Principle
Triple Point [S.M.O.W.]Triple Point [S.M.O.W.] P = 611.657 Pa (0.006 bar)P = 611.657 Pa (0.006 bar) T = 273.16 K (0.16T = 273.16 K (0.16oo C) C) DD22O: 661 Pa, 276.82KO: 661 Pa, 276.82K
-0.02 0 0.02-0.02 0 0.02 Temperature [C] Temperature [C]
612612
611611
610610
613613
Pre
ssur
e [P
a]P
ress
ure
[Pa]
1 bar = 101 bar = 1055 Pa = 10 Pa = 1055 Nt/m Nt/m22
1 1 atmatm = 101325 Pa = 101325 Pa
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Water Ice PhysicsWater Ice Physics Exists in 13 crystallineExists in 13 crystallinephases (diff T & P)phases (diff T & P) Phase I: P < 2700 Phase I: P < 2700 atmatm
IhIh –– hexagonal hexagonal IcIc –– cubic (low T, low P) cubic (low T, low P)
metastablemetastable
High P forms: II to XIHigh P forms: II to XI
Amorphous IceAmorphous Ice ClathratesClathrates
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Amorphous IceAmorphous Ice Forms at low T Forms at low T insufficient E insufficient E
for crystal structurefor crystal structure Physical PropertiesPhysical Properties
Large voids: trapped gasesLarge voids: trapped gases Gases released between 35-120KGases released between 35-120K
AnnealingAnnealing 38-68K 38-68K –– transition from transition from IIaahh IIaall Beginning at 90K Beginning at 90K IcIc (exothermic) (exothermic)
Two formsTwo forms High Density, High Density, IIaahh Low Density, Low Density, IIaall
Ice Ice IIaall and and IIaahh formation formation
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ClathrateClathrate Hydrates Hydrates Crystalline framework of H-bonded HCrystalline framework of H-bonded H22O O molecmolec..
trapping guest moleculestrapping guest molecules Guests donGuests don’’t affect the chemistryt affect the chemistry
Released upon sublimation of waterReleased upon sublimation of water Cages unstable without guestsCages unstable without guests Some physical properties are alteredSome physical properties are altered Some Some clathrateclathrate formation not possible at low T and P formation not possible at low T and P Stability: low T (< 273K), moderate to high P (100 Stability: low T (< 273K), moderate to high P (100 atmatm))
ImportanceImportance May store most of SS inventory: CO, COMay store most of SS inventory: CO, CO22, CH, CH44 Catastrophic destabilization due to T , PCatastrophic destabilization due to T , P
Collapse & flow featuresCollapse & flow features OutgassingOutgassing Greenhouse gas budgetsGreenhouse gas budgets
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ClathrateClathrate Hydrates Hydrates–– Contd. Contd.
Type IType I 46 H46 H22O moleculesO molecules 2 small cages, 6 large2 small cages, 6 large 12- and 14- sided polygons12- and 14- sided polygons Traps in ratio 1/7Traps in ratio 1/7
Type IIType II 126 H126 H22O moleculesO molecules 16 small cages, 8 large16 small cages, 8 large 14- and 16- sided polygons14- and 16- sided polygons Traps in ratio 1/17Traps in ratio 1/17
ClathratesClathrates in the Solar System in the Solar System CHCH44 –– marine sediments marine sediments –– by 2x by 2x
exceeds other fossil fuelexceeds other fossil fuelsourcessources
COCO22 –– sequester CO sequester CO22 in ocean in oceanseafloor from seafloor from atmatm (climate) (climate)
Destabilization on Mars &Destabilization on Mars &EuropaEuropa –– chaotic terrain? chaotic terrain?
CHCH44 / N / N22 on Triton on Triton –– geysers geysers Air Air –– polar ice sheets polar ice sheets –– info on info on
atmosphere up to 10atmosphere up to 1066 yr ago yr ago
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Ice Regimes Ice Regimes –– Interior Pressures Interior Pressures PPcc = 2 = 2ππGGρρ22 (R (R22 –– r r22)/3)/3
ppmppm
<100 <100 ppmppm
2:1?2:1?
2:1?2:1?
Dust:IceDust:Ice
IhIh, , clathratesclathrates300300331-1.61-1.6Mars IceMars Ice
High den. High den. amorphamorph––1010-10-100.10.1ISgrainsISgrains
IhIh, , clathratesclathrates300300330.920.92GlacierGlacier
IhIh, II, , II, clathratesclathrates1x101x1044135013502.072.07TritonTriton
IhIh, II, VII, VIII, , II, VII, VIII, clathclath3x103x1044156915692.972.97EuropaEuropa
IhIh, II, , II, clathclath, , amorphamorph3.5-14003.5-1400101022-10-10330.5-1?0.5-1?KBOKBO
IhIh, , IcIc, amorphous, amorphous0.0003-0.10.0003-0.11-101-100.5-1?0.5-1?CometComet
IcesIcesP [bar]P [bar]Size [km]Size [km]ρρ [g/cm [g/cm33]]RegimeRegime
Phase changes: volume changes Phase changes: volume changes fractures fractures Amorphous Amorphous IcIc, exothermic , exothermic volatile release volatile release ClathrateClathrate destabilization destabilization outgassingoutgassing
G = 6.67 x 10G = 6.67 x 10-11-11 Ntm Ntm22/kg/kg22
ρρ = density, kg/m = density, kg/m33
R = radius, mR = radius, m
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Comet ExpectationsComet Expectations Amorphous iceAmorphous ice
Formation T: 30-100KFormation T: 30-100K Crystalline icesCrystalline ices
Solar heating: Solar heating: amorphousamorphouscrystallinecrystalline transition peaking at 137K transition peaking at 137K
Balance with cosmic ray processingBalance with cosmic ray processing Lack of Lack of ClathratesClathrates
Small size, low central pressuresSmall size, low central pressures Release of volatiles in excess ofRelease of volatiles in excess of
clathrateclathrate capacity capacity Not necessary to explain activity!Not necessary to explain activity!
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Cosmic Solar System HistoryCosmic Solar System History
>4.6 >4.6 GyGyISM dark cloudISM dark cloud
PlanetesimalsPlanetesimals condense condensePlanets accretePlanets accreteForm few x100 million yearsForm few x100 million years
Earth in the HadeanEarth in the HadeanOceans & rocks formOceans & rocks form~4.4 ~4.4 GyGy ago ago
Late planetary bombardmentLate planetary bombardmentComets, asteroids bring water &Comets, asteroids bring water &Organics to EarthOrganics to Earth
The The ArcheanArchean Epoch EpochOldest life on EarthOldest life on Earth3.5-3.8 3.5-3.8 GyGy ago ago
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Comet FormationComet Formation
100K100K
64K64K
31K31K
00 1010 100 AU100 AU
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Low Temperature CondensationLow Temperature Condensation Ices in comets condensedIces in comets condensed
T< 100KT< 100K Amorphous formAmorphous form Trapped other gasesTrapped other gases Amounts depend on Amounts depend on rr
Release of gasesRelease of gases 90-137K amorphous 90-137K amorphous
crystalline phase changecrystalline phase change Annealing (30-120K)Annealing (30-120K) IIaahh IIaall IcIc IhIh ~ 150 K ~ 150 K Sublimation start 160-180KSublimation start 160-180K
CHCH44
NN22
ArArCOCO
Gas release at large distances:Gas release at large distances:controlled by Watercontrolled by Water
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Sublimation of Volatiles?Sublimation of Volatiles?
DelsemmeDelsemme’’ss original work: original work: albedoalbedo too high too high Water-activity out beyond JupiterWater-activity out beyond Jupiter
Log
Z [
Log
Z [ m
olec
mol
ec m m
-2-2 s s
-1-1]]
DelsemmeDelsemme (1971) (1971)
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Complications:Complications:Heat Transport in Real NucleiHeat Transport in Real Nuclei
Solve the heat conduction equationSolve the heat conduction equation ρρ(z(z) ) c(z,Tc(z,T) ) dT/dtdT/dt = = d/dzd/dz [ [κκ(z,T(z,T) ) dT/dzdT/dz]] Boundary condition: Energy Balance EquationBoundary condition: Energy Balance Equation Heat sources:Heat sources:
Solar radiation Solar radiation –– cyclic cyclic Radioactivity Radioactivity –– declining declining Crystallization Crystallization –– transient, front induced transient, front induced
ApproximationsApproximations Ice Thermal properties very differentIce Thermal properties very different
κκaa << << κκcc (4 orders of (4 orders of magmag)) κκaa αα T and T and κκcc αα 1/T 1/T
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Heat Conduction in Porous MediaHeat Conduction in Porous Media
Pores reduce thermal conductivityPores reduce thermal conductivity Conduction by radiationConduction by radiation Conduction by vapor sublimation Conduction by vapor sublimation
recondensationrecondensation Releases heat, warming colder areasReleases heat, warming colder areas Reduces the thermal gradientReduces the thermal gradient Sintering Sintering decreases porosity decreases porosity
Porosity: 7.5% 13% 15% 22%Porosity: 7.5% 13% 15% 22%
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Activity at Large r?Activity at Large r?The Evidence for FadingThe Evidence for Fading
Morehouse 1908 IIIGreat Comet 1577 Halley 1910 Delavan 1914
Different types of evidenceDifferent types of evidence Really bright comets are all long-periodReally bright comets are all long-period Distant comets Distant comets narrow tails (large dust) narrow tails (large dust) volatile gases volatile gases New comets tend to split more frequently (more volatiles)New comets tend to split more frequently (more volatiles) Non-gravitational motion (jets)Non-gravitational motion (jets)
ProblemsProblems Non uniform data setsNon uniform data sets Non-linear detectorsNon-linear detectors
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SP Comets 3.4-14.5 AUSP Comets 3.4-14.5 AU
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Comet Activity Levels Comet Activity Levels Trends Trends
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Evidence for DifferencesEvidence for Differences
Dots = All SP Dots = All SP obsobs Squares = HalleySquares = Halley Triangles = DN cometTriangles = DN comet
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The Halley OutburstThe Halley Outburst
Gas Laden amorphous ice modelGas Laden amorphous ice model Heat from perihelion penetrates to ice layerHeat from perihelion penetrates to ice layer Exothermic transformation (137K)Exothermic transformation (137K) Released gases build up pressure Released gases build up pressure outburst outburst
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ChironChiron’’s Behaviors Behavior
Amorphous ice modelAmorphous ice model 60% dust60% dust 40% amorphous ice40% amorphous ice 0.1% trapped CO0.1% trapped CO
Matches observationsMatches observations Density < 0.4 g/cmDensity < 0.4 g/cm33
Mass loss rates & dustMass loss rates & dust CO fluxes match CO fluxes match obsobs TTsurfacesurface matches matches obsobs Activity sporadic Activity sporadic
not refreshing surfacenot refreshing surface
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C/1995 O1 (Hale C/1995 O1 (Hale BoppBopp))
Active at large rActive at large r Discovered in 1995 atDiscovered in 1995 at
7.2 AU (active, inbound)7.2 AU (active, inbound) Pre-discovery imagePre-discovery image
13.0 AU (1993)13.0 AU (1993)
Dynamically youngDynamically young Large CO fluxes seenLarge CO fluxes seen Molecules of differentMolecules of different
volatilities appear atvolatilities appear atsimilar timessimilar times
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Thermal models: Comet Hale Thermal models: Comet Hale BoppBopp
Amorphous ice crystallization modelAmorphous ice crystallization model Porosity 0.65Porosity 0.65 4% by mass trapped CO4% by mass trapped CO
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Activity at Larger r?Activity at Larger r?
Distance for T ~ 137KDistance for T ~ 137K Beginning near 10 AUBeginning near 10 AU
Mechanisms at r > 10 AUMechanisms at r > 10 AU Solid volatiles (e.g. CO,Solid volatiles (e.g. CO,
COCO22) sublimation) sublimation Amorphous Amorphous Crystalline Crystalline
transitiontransition AnnealingAnnealing
C/2003 A2 GleasonC/2003 A2 Gleasonq = 11.43 AUq = 11.43 AU1/a = 42 x 101/a = 42 x 10-6-6 AU AU-1-1
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KBO1996 TOKBO1996 TO6666 –– Activity? Activity? OrbitOrbit
Q = 48.6, q = 38.5Q = 48.6, q = 38.5 q: 5/3/1910 Q: 2/1/2054q: 5/3/1910 Q: 2/1/2054
LightcurveLightcurve period period 1997: 2 peak 6.25 +/- 0.031997: 2 peak 6.25 +/- 0.03
hr, hr, ΔΔm = 0.12 m = 0.12 magmag 1998: single peak, 1998: single peak, ΔΔm =m =
0.330.33 Consistent with activityConsistent with activity Blue colorsBlue colors
Vary with rotation in 1999Vary with rotation in 1999
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Direct Evidence for Ice PhasesDirect Evidence for Ice Phases
C/1995 O1 Hale C/1995 O1 Hale BoppBopp 1.4-2.5 1.4-2.5 µµm: no 1.65 m: no 1.65 µµmm
feature feature amorphous amorphous
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MirandaMiranda
1.65 1.65 µµm crystalline water ice feature presentm crystalline water ice feature present Spectral models: NHSpectral models: NH33 .. H H22O for 2.2 O for 2.2 µµm featurem feature Dark spectrally neutral componentDark spectrally neutral component
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SummarySummary HH22O ice in cometsO ice in comets IaIa, , IcIc, , IhIh, no , no clathratesclathrates ClathratesClathrates imptimpt else else
where in the SSwhere in the SS((KBOsKBOs?)?)
Gas release at largeGas release at larger: controlled by Hr: controlled by H22OO AnnealingAnnealing IaIa IcIc IhIh sublimationsublimation
Comets are cosmicComets are cosmic““thermometersthermometers”” for forSS formationSS formation
Low heat transportLow heat transport Solar Solar insolationinsolation Radioactive decayRadioactive decay crystallizationcrystallization
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Inactivity to ActivityInactivity to Activity
Sublimation termSublimation term Cools nucleus surfaceCools nucleus surface dmdmss/dt/dt = = PPvaporvapor/v/vthth
P: from lab, or thermo.P: from lab, or thermo.
ConductionConduction Often assumed small..Often assumed small..
Incident E depends onIncident E depends on Heliocentric distanceHeliocentric distance Surface Surface albedoalbedo / /
scatteringscattering
Re-radiated ERe-radiated E Surface T (rotationSurface T (rotation
dependent; material prop)dependent; material prop)
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Radioactive Heat ProductionRadioactive Heat Production MechanismMechanism
Elements spontaneously lose mass and EElements spontaneously lose mass and E Decay rate depends on # atomsDecay rate depends on # atoms Rate Rate characterizedcharacterized by by ““half-lifehalf-life””
ImplicationsImplications Small comets Small comets IaIa IhIh quenched by dust quenched by dust Medium to large Medium to large KBOsKBOs IhIh & liquid & liquid
interiorsinteriors
1.261.264040ArAr4040KK
0.72 My0.72 My2626MgMg2626AlAl16 My16 My129129XeXe129129II
48.848.88787SrSr8787RbRb4.474.47206206PbPb238238UUHalf-Life [Half-Life [GyGy]]DaughterDaughterParentParent