contrasting geodynamics of small cold and giant hot orogens c. beaumont r. jamieson p. fullsack...
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![Page 1: Contrasting Geodynamics of Small Cold and Giant Hot Orogens C. Beaumont R. Jamieson P. Fullsack Dalhousie University, Canada B.Lee M. Nguyen Susan Ellis](https://reader036.vdocuments.mx/reader036/viewer/2022070307/551b75be550346d6338b50ab/html5/thumbnails/1.jpg)
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Contrasting Geodynamics of Small
Cold and Giant Hot OrogensC. Beaumont
R. Jamieson P. Fullsack Dalhousie University, Canada B.Lee
M. Nguyen
Susan Ellis New Zealand
Adrian Pfiffner University of Bern, Switzerland
Institute of
GEOLOGICAL
& NUCLEAR
SCIENCES
limited
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GLOBE project (NOAA)1. Indentation (3D)
2. Pre-existing weakness
3. Lower lithosphere dynamics
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0
500
1000
1500
2000
2500
3000
0 500 1000 1500 2000 2500
convergence (km)
wav
elen
gth
(km
)Orogen wavelength vs. convergence
HT
VA
NZ, EA
Modified from Ellis (1995)
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Eastern Swiss Alps
NARROW -- < 250 km
•moderate crustal temperatures (< 700 C)
•little crustal melting
•most intense crustal deformation intense mantle lithosphere deformation
•three-dimensionality generally not a first-order control on wavelength
“Small Cold (SC) Orogens”
New Zealand Southern Alps
Wellman, 1979
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•high crustal temperatures and extreme crustal thickening
•crustal melting
•most intense crustal deformation most intense mantle lithosphere deformation
•three-dimensionality may be a first-order control on wavelength
“Giant Hot (GH) Orogens”
WIDE-- > 1000 km
X
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Small vs. giant orogens: (1) strength of ductile lower crust?
x=100 km
Viscosity
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Ellis et al, 2000
Small vs. giant orogens: (2) localisation by strain weakening?
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Ellis et al, 2000
Small vs. giant orogens: (3) localisation by erosion?
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Tectonic processes affecting the Himalayan-Tibetan System“Giant Hot” (GH) orogens:
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= B * ex p (Q * /n R T )
H T R L -2 5 : R eferen ce M o d el, In itia l C o n d itio n s
02 03 5
km
T = 1 3 5 0 o Ca
q s = 7 0 m W /m 2
R h eo lo g ica l P ro p erties:
U p p er c ru s t: = 1 5 o (W et Q u a rtz ite x 5 ) L o w er c ru s t: = 1 5 o (D ry M ld D iab ase )
T h erm a l P ro p ertie s:
K = 2 .0 W /m o K = 1 .0 x 1 0 m /s-6 2A = 2 .0 W /m1
3 A = 0 .7 5 W /m23
Tem p era tu re a n d Ve lo c ity
C p( T / t + v T ) = K T + AA d v e c tio n D iffu s io n H ea t
P ro d u c tio n
E ffectiv e V isco sity : H ea t B a la n ce:11
n
2 cm /y
D en u d ation ra te = S lop e f(t) g (x )
M o h o = 7 0 4 C0
A 1
A 2
0
6 0 0 k m
3 52 5
1 4 0 0 k m
km
M a rker G rid
2 cm /y
...... ........ 2 0 o
q m = 2 0 m W /m 2
K inem a tic Subduc tion
C o nd uc tive Stea dy-Sta te
E ro s io n fu n c tio n g (x )
1.0 0.0
Beaumont et al, 2001
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Beaumont et al, 2001
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Beaumont et al, 2001
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Channel flow only occurs for cases where partial melt ( 1019 Pa.s) is present
Extrusion only occurs for cases with high erosion
Beaumont et al, 2001
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Beaumont et al, submitted
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“Small Cold (SC) Orogens”
New Zealand Southern Alps
Walcott, 1998
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• Extrusion of mid-lower crust (Grapes, 1995; Walcott, 1998)
Batt and Braun, 1999
Felsic crustTotal erosionConvergence 10mm/a
6 Ma
Retro shear zone
Secondary pro-shear
Primary pro-shear
0 C
600 C
30
km
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shortening = 40 km
-104090
140
12 62 112 162distance (km)
Vertical velocity
20C/km geotherm
1 cm/yr
Gerbault and Ellis, submitted
1021 1024
x
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Structural Geology Transect
Little et al. in press
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Arthur’s Pass: Campaign data sets
Beavan and Ellis, in prep.
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Post-seismic signal
VISCOELASTIC MODEL: Lower crustal channel =1018 Pa s
OBSERVATIONS
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“Small Cold (SC) Orogens” “Giant Hot (GH) Orogens”
High non-linear viscosities make extrusion less likely
Inherited material heterogeneities can influence dynamics
Low linear viscosities (partial melt)+erosion can cause extrusion
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Hertzsprung-Russell diagrams for stars
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Excess volume
H-R diagram for orogens
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