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Cryovolcanism on Charon and other Kuiper Belt Objects
Steve Desch
Jason Cook, Wendy Hawley, Thomas Doggett
School of Earth and Space Exploration
Arizona State University
Outline
•Crystalline water ice as a
signature of cryovolcanism
•Correlation of crystalline water
ice with KBO Size
•Thermal evolution models
Some KBOs have Crystalline Water Ice on their Surfaces; Some have Amorphous Ice
Mastrapa & Brown (2005)
0.03
0.12
Band Ratio
1.65 micron feature is diagnostic
Crystalline Water Ice = Sign of CryovolcanismCrystalline water ice is rapidly amorphized
•in ~ 1 Myr by cosmic rays (Cooper et al. 2003)
•in < 0.1 Myr by solar UV (Cook et al. 2007)
•Heating and annealing of ice by micrometeorites?
•Takes > 3 Myr (Cook et al. 2007)
•Would work equally on KBOs of all sizes
•Cryovolcanism most likely source of crystalline H2O ice
•Corroborated by ammonia hydrates (Charon,Quaoar)
•Appears limited to KBOs with radii > 400-500 km
Only Large KBOs clearly have Crystalline Water Ice
2003 EL61
Quaoar
Charon
Orcus
2002 TX300
~ 725 km
630 +/- 95 km
603.6 km
600 +55/-90 km
< 555 km (3)
0.06
0.12
0.13
~ 0.12
~ 0.1 ?
Object Radius Band Ratio
Small KBOs have Amorphous Water Ice
1996 TO66
S/2005 (2003 EL61) 1
1997 CU26
Hale-Bopp
C/2002 T7
~ 325 km
~ 160 km
118 km
~ 30 km
~ 10 km
0.04
0.03
0.03
0.03
0.03
Object Radius Band Ratio
1996 TO66 (Brown et al. 1999)
S/2005 (2003 EL61) 1
Barkume et al. (2006)
1997 CU26
(Brown et al. 1998)
Cryovolcanism on KBOs
•If less dense than overlying layers, subsurface liquid easily rises to surface via self-propagating cracks (Crawford & Stevenson 1988).
•Subsurface liquid requires T > 273 K (pure water ice) or T > 176 K (with ammonia)
•Internal temperatures of KBOs modeled using a thermal evolution code we wrote.
Thermal Evolution Models
•1-D spherical geometry (~ 100 zones)
•Radiogenic heating from 40K, 235U, 238U, 232Th
•Conductive fluxes in and out of each zone
•Conductivities k(T), T(E) depend on material
Thermal Evolution Models
•Five phases: rock; H2O(s); ADH; H2O(l); NH3(l)
•Given heat capacities, latent heats, rock / H2O / NH3 fractions, and total internal energy E, we find ice phases, temperature T(E)
(176 < T < Tliq)E.g.,
Thermal Evolution Models
•Rdiff =maximum radius to ever reach T > 174 K (ADH melts; ice creeps).
•Inside Rdiff, rock sinks to core, water ice floats, liquid/ADH slush in between.
•Thermal conductivities of ordinary chondrites (Yomogida & Matsui 1983), ADH (Lorenz & Shandera 2001) used; combined using Sirono &Yamamoto (2001)
•Charon (63% rock, R = 604 km, Tsurf = 60 K) differentiates in < 70 Myr,
• Rdiff = 480 km, Rcore = 330 km (has half of Charon’s rock)
•All ADH inside Rdiff melts, yielding 4 x 1022 g (if X = 0.05) of NH3-rich (32%) liquid.
•Core temperature rises until t = 2.0 Gyr, to 1300 K, steadily declines thereafter
Thermal Evolution Models: Results
•Release of heat from core over next 2.5 Gyr increases average flux from 1.0 to 1.5 erg cm-2 s-1
•Temperature just outside core maintained above 176 K until about 4.8 Gyr: has liquid today
•NH3-rich liquid much less dense ( < 0.9 g cm-3) than overlying rocky layers ( ~ 1.7 g cm-3), and is positively buoyant.
•Temperatures outside core always < 273 K: liquid only possible with ammonia.
Thermal Evolution Models: Results
Thermal Evolution Models: Results
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Thermal Evolution Models: Results
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are needed to see this picture.
•Calculation repeated for smaller bodies:
•R = 600 km (Charon): liquid until 4.8 Gyr
•R = 500 km maintains liquid until 4.4 Gyr
•R = 400 km maintains liquid until 3.2 Gyr
•Cryovolcanism possible, today, on Charon, Quaoar & Orcus
•Minimum radius needed close to 500 km, consistent with observations of crystalline ice.
Thermal Evolution Models: Results
ArielLinear troughs = extensional stresses
Some terrains on Ariel < 100 million years old (Plescia 1989)