EART193 Planetary Capstone

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Presentation transcript:

EART193 Planetary Capstone Francis Nimmo

Topics I want to cover a couple of topics which have both terrestrial and planetary applications: Lava lakes are well-studied on Earth and also appear to exist on Io Surface inflation by subsurface intrusions is also well-studied on Earth and has been applied to Venus

Terrestrial lava lakes Patrick et al. 2016

Observations Surface temperatures are roughly 300-500 K (much less than magma temperature) Typical surface velocities ~ 20 cm/s Typical thickness of surface crust ~ 6 cm We need some theory to explain these . . .

Constant viscosity convection Vigour of convection is given by the Rayleigh number Ra: A convecting fluid will consist of an interior in motion and a thermal boundary layer which is moving horizontally but not vertically. Heat is conducted across this layer of thickness d: More vigorous convection will give thinner boundary layers (and higher heat fluxes). Note that d is independent of d. The characteristic fluid velocity is given by

Conceptual lava lake model Frad d We can solve for the surface temperature Ts How do our results compare with the observations?

What about Io? Loki Patera as seen by Voyager 1 in March 1979. Numerous volcanic calderas and lava flows are visible. Loki Patera is the large shield‐shaped black feature in the lower center and is about 200 km in diameter. The bright whitish patches are probably freshly deposited SO2 frost. The feature Loki was the source of two volcanic plumes during the Voyager epoch. Photo credit: NASA. IF THIS IMAGE HAS BEEN PROVIDED BY OR IS OWNED BY A THIRD PARTY, AS INDICATED IN THE CAPTION LINE, THEN FURTHER PERMISSION MAY BE NEEDED BEFORE ANY FURTHER USE. PLEASE CONTACT WILEY'S PERMISSIONS DEPARTMENT ON PERMISSIONS@WILEY.COM OR USE THE RIGHTSLINK SERVICE BY CLICKING ON THE 'REQUEST PERMISSIONS' LINK ACCOMPANYING THIS ARTICLE. WILEY OR AUTHOR OWNED IMAGES MAY BE USED FOR NON-COMMERCIAL PURPOSES, SUBJECT TO PROPER CITATION OF THE ARTICLE, AUTHOR, AND PUBLISHER. Journal of Geophysical Research: Planets Volume 111, Issue E9, E09002, 2 SEP 2006 DOI: 10.1029/2006JE002703 http://onlinelibrary.wiley.com/doi/10.1029/2006JE002703/full#jgre2189-fig-0001

Loki Patera is probably a lava “lake” Image of Loki Patera showing the Davies [2003] temperature map with the location and inferred direction of motion of the resurfacing front noted. Also shown is the age of the surface and the crustal thickness. The active front, where crust is foundering and being replaced by new, hot lava, is probably to the NE of the area covered by the Galileo NIMS observation 32INTHLOKI01 obtained in October 2001 from which the Davies [2003] age‐temperature map was derived. IF THIS IMAGE HAS BEEN PROVIDED BY OR IS OWNED BY A THIRD PARTY, AS INDICATED IN THE CAPTION LINE, THEN FURTHER PERMISSION MAY BE NEEDED BEFORE ANY FURTHER USE. PLEASE CONTACT WILEY'S PERMISSIONS DEPARTMENT ON PERMISSIONS@WILEY.COM OR USE THE RIGHTSLINK SERVICE BY CLICKING ON THE 'REQUEST PERMISSIONS' LINK ACCOMPANYING THIS ARTICLE. WILEY OR AUTHOR OWNED IMAGES MAY BE USED FOR NON-COMMERCIAL PURPOSES, SUBJECT TO PROPER CITATION OF THE ARTICLE, AUTHOR, AND PUBLISHER. Journal of Geophysical Research: Planets Volume 111, Issue E9, E09002, 2 SEP 2006 DOI: 10.1029/2006JE002703 http://onlinelibrary.wiley.com/doi/10.1029/2006JE002703/full#jgre2189-fig-0007

Evidence for foundering? Model 3 is the “foundering” model [after Rathbun et al., 2002]. IF THIS IMAGE HAS BEEN PROVIDED BY OR IS OWNED BY A THIRD PARTY, AS INDICATED IN THE CAPTION LINE, THEN FURTHER PERMISSION MAY BE NEEDED BEFORE ANY FURTHER USE. PLEASE CONTACT WILEY'S PERMISSIONS DEPARTMENT ON PERMISSIONS@WILEY.COM OR USE THE RIGHTSLINK SERVICE BY CLICKING ON THE 'REQUEST PERMISSIONS' LINK ACCOMPANYING THIS ARTICLE. WILEY OR AUTHOR OWNED IMAGES MAY BE USED FOR NON-COMMERCIAL PURPOSES, SUBJECT TO PROPER CITATION OF THE ARTICLE, AUTHOR, AND PUBLISHER. Journal of Geophysical Research: Planets Volume 111, Issue E9, E09002, 2 SEP 2006 DOI: 10.1029/2006JE002703 http://onlinelibrary.wiley.com/doi/10.1029/2006JE002703/full#jgre2189-fig-0005

Surface temperatures Two-temperature fits “Cold” part is probably cooled crust “Hot” part is probably fissures Hot component Cold component Orbit Temp (K) Area (km2) Output (GW) G2 1394+/-25 0.46 99 769+/-25 5.8 116 G8 1362+/-78 0.20 39 549+/-19 31 161 C10 1077+/-13 1.6 122 544+/-7 24.4 121 E15 1369+/-141 0.42 94 625+/-43 15.4 133 E16 1353+/-46 0.63 120 649+/-16 15.9 160 C20 1300+/-71 0.41 66 588+/-8 25.4 172 Davies, Volcanism on Io, CUP, 2007

Periodic Behaviour? Rathbun et al. 2002

“Mogi model” What happens if a magma body is intruded at depth? r d 2a u = horizontal displacement v = vertical displacement

1d 2d 3d 4d v u er et What would a plot of the strains look like? What would you predict for their surface expression?

S. America (Pritchard & Simons 1994) Long Valley, CA (Tizzani et al. 2009))

What about Venus? Grindrod et al. (2005) Scale bar 100 km

Homework – Week 7 Write a ~1000 word chunk of your report Due next Tues No class on Thurs – use the time to write