Diverse Igneous Geology in and around the Columbia Hills
Diverse Igneous Geology
in and
around the Columbia Hills for
Diverse Science Investigations
Hanna Nekvasil
1
; Steve Ruff
2
, Donald Lindsley
1
, Vicky
Hamilton
3
, Nicholas DiFrancesco
1
, and Francis McCubbin
4
1
Stony Brook University
2
Arizona State University
3
Southwest Research Institute
4
Johnson Space Center
NOTE ADDED BY JPL WEBMASTER: This content has not been approved or adopted by, NASA, JPL, or the California Institute of Technology. This document is being made available for information
purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology.
Mantle characteristics
processing
Planetary differentiation
P-T HISTORY
Geothermometry
Geobarometry
Oxygen fugacity
Phase equilibria
Crustal structure
Crustal dynamics
Cooling history
Diffusion profiles
(trace elements
and volatiles in
minerals)
Geospeedometers
AGE
176
Lu/
176
Hf;
238
U/
206
Pb;
235
U/
207
Pb,
87
Rb/
87
Sr;
40
K/
40
Ar,
147
Sm/
143
Nd
Martian atmosphere
Sulfates and chlorides on
the surface
SOURCE CHARACTERISTICS
Bulk composition
Mineral composition
Trace element variability
Isotope initial ratios
87
Rb/
87
Sr;
147
Sm/
143
Nd, etc
VOLATILE BUDGET
Bulk volatiles (e.g.,
OH, Cl, F, S, B)
Melt inclusion volatile
content
Volatile loss [e.g., D,
37
Cl;
34
S;
66
Zn]
Timing of loss (mineral
zoning)
Coatings
fluids
Using
Backstay
as an evolved hawaiite…
•
linked the experimental phase equilibria
of a magma with Backstay composition
with
melt inclusions in the Chassigny
dunite
.
•
showed that this meteorite may have
been a cognate xenolith brought to the
surface during an eruption of residual
melt
•
constrained the magmatic water content
of the Chassigny parent.
Nekvasil et al.
(2009)
Unaltered igneous rock has already proven invaluable…
Coupling to meteorites to show fractionation processes
Using
Humphrey (Adirondack Class)
as a
relatively primitive basalt from the martian
mantle …
•
how the martian mantle water budget
would produce diverse magmas reaching
the surface if fractionating at the base of
the martian crust
McCubbin et al. (2008)
•
how these lavas would change in
composition as the crust thickened
McCubbin et al. (2008)
•
how crystallization of these lavas on
the surface could produce feldspathic
rocks of the type seen at Nili Patera
and Noachis Terra.
Rogers and
Nekvasil 2015
Coupling to surface spectroscopy
Lending insight into alteration processes from high to low temperature…
http://marsnext.jpl.nasa.gov/scieng_geo.cfm
Gusev Crater/Columbia Hills
3
3
.
.
6
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Greeley et al. (2005)
Columbia
Hills
Adirondack Class basalt
CTX
2.5 km
Columbia Hills are
embayed by plains basalt
(Adirondack Class;
Hamilton and Ruff, 2012),
thus are likely at least
Late Noachian in age
(McCoy et al., 2008)
CTX
2.5 km
Adirondack Class: An ideal sample for tying crater
retention age to absolute age
http://marsnext.jpl.nasa.gov/scieng_geo.cfm
Gusev Crater/Columbia Hills
McCoy et al., 2008
Backstay
Irvine
Ming et al 2008
4. Access to unaltered
igneous rock as float
Rimming the Tennessee Valley:
•
unaltered to modestly altered,
massive, aphanitic, alkaline
basalts of the Irvine (tholeiitic
basalt) and Backstay classes
(trachybasalt) are found as
exotics [McSween et al., 2006a;
Ruff et al., 2006],
•
Adirondack class basalts
(picritic basalt) also present,
that are prevalent on the plains
[McSween et al., 2004, 2006b].
Irvine class basalts also dominate
the Inner Basin of the Columbia
Hills to the south of Husband Hill
[Crumpler et al., 2007].
Humphrey
Adirondack
Mazatzal
•
Irvine
class basalts also dominate the Inner Basin of the Columbia Hills to
the south of Husband Hill, where they are often vesicular to scoriaceous
[Crumpler et al., 2007].
•
Descartes
class rocks are breccias with angular clasts that can reach a
centimeter in size. The origin of these rocks is uncertain, but aqueous
alteration of either a pyroclastic volcanic, impact breccia (McCoy et al. 2008)
or impact melt breccia (Arvidson et al. 2008).
•
Algonquin
series mafic-ultramafic series, olivine rich, relatively
unaltered.(Ming et al. 2008)
•
…
•
Assemblee
: pyroxene+chromite (mantle xenoliths?)
•
Algonquin/Comanche subclass
: olivine+pyroxene (ultramafic?
•
….
A
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Husband Hill
Husband Hill
Home Plate
Home Plate
Algonquin
Class
mafic-ultramafic series, olivine rich,
relatively unaltered (Ming et al. 2008)
250 m
Algonquin - Miami
Comanche
Morphologic And
Morphologic And
Thermal Expression
Thermal Expression
HiRISE
Comanche/Algonquin outcrops
Comanche/Algonquin outcrops
display distinctive knob and ridge
display distinctive knob and ridge
morphology and higher thermal
morphology and higher thermal
inertia than surrounding terrain
inertia than surrounding terrain
THEMIS colorized night IR over CTX
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3 km
THEMIS colorized night IR over CTX
Morphologic And
Morphologic And
Thermal Expression
Thermal Expression
HiRISE: All scenes 250 m across
•
Additional examples of
Additional examples of
Comanche/Algonquin-
Comanche/Algonquin-
like terrain in kipukas
like terrain in kipukas
•
Interpreted by Ruff et al.
Interpreted by Ruff et al.
(2014) as remnants of
(2014) as remnants of
formerly more extensive
formerly more extensive
Algonquin-like tephra
Algonquin-like tephra
deposits that mantled
deposits that mantled
the region and were
the region and were
eroded prior to flood
eroded prior to flood
basalts at 3.65 Ga
basalts at 3.65 Ga
(Greeley et al., 2005)
(Greeley et al., 2005)
“Promised Land”
“Italy” feature
Mantle characteristics
processing
Planetary differentiation
Igneous P-T HISTORY
Geothermometry
Geobarometry
Oxygen fugacity
Phase equilibria
Crustal structure
Crustal dynamics
Martian atmosphere
Sulfates and chlorides on the surface
Mars Exploration Rover Mission
,
JPL
,
NASA
VOLATILE BUDGET
Distribution of volatiles
(Cl, Br, Zn, S) in Coatings/dust
SOURCE CHARACTERISTICS
Mineral composition
Trace element load
FRACTIONATION PROCESSES
Mineral composition
Residual glass
Trace element variability
With PIXL, SuperCam, SHERLOC
Irvine
Backstay
Assemblee
Fluid
characteristics
Many diverse samples from
mainly igneous signature
Vapor deposits?
Brines?
Magmatic or meteoric water?
Igneous P-T HISTORY
Geothermometry
Geobarometry
Oxygen fugacity
Phase equilibria
Crustal structure
Crustal dynamics
Martian atmosphere
Sulfates and chlorides on the surface
Mars Exploration Rover Mission
,
JPL
,
NASA
INTERACTION WITH/LOSS
OF VOLATILES
Distribution of volatiles
(Cl, Br, Zn, S) in matrix and or
surface
Changes in mineral
composition
Changes in trace element
load
FRACTIONATION PROCESSES
Mineral composition
Residual glass
Trace element variability
With PIXL, SuperCam, SHERLOC
Wishstone
Everett
Peace
To increasing alteration signatures
Diverse Igneous Geology in and
around the Columbia Hills for
Diverse Science Investigations
Studying the diverse igneous geology in and around the Columbia Hills provides insights into Martian atmosphere, volatile budget, age, source characteristics, cooling history, and more. Researchers have uncovered valuable information by coupling unaltered igneous rocks with meteorites and surface spectroscopy, shedding light on fractionation processes and magma evolution. Key findings offer a deeper understanding of Mars' mantle water budget, magma diversity, and rock crystallization processes.
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Diverse Igneous Geology in and around the Columbia Hills for Diverse Science Investigations Hanna Nekvasil1; Steve Ruff2, Donald Lindsley1, Vicky Hamilton3, Nicholas DiFrancesco1, and Francis McCubbin4 1 Stony Brook University 2Arizona State University 3Southwest Research Institute 4Johnson Space Center NOTE ADDED BY JPL WEBMASTER: This content has not been approved or adopted by, NASA, JPL, or the California Institute of Technology. This document is being made available for information purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology.
Martian atmosphere Sulfates and chlorides on the surface VOLATILE BUDGET Bulk volatiles (e.g., OH, Cl, F, S, B) Melt inclusion volatile content Volatile loss [e.g., D, 37Cl; 34S; 66Zn] Timing of loss (mineral zoning) Coatings AGE 176Lu/176Hf; 238U/206Pb; 235U/207Pb, 87Rb/87Sr; 40K/40Ar, 147Sm/143Nd fluids P-T HISTORY Geothermometry Geobarometry Oxygen fugacity Phase equilibria SOURCE CHARACTERISTICS Bulk composition Mineral composition Trace element variability Isotope initial ratios 87Rb/87Sr; 147Sm/143Nd, etc Cooling history Diffusion profiles (trace elements and volatiles in minerals) Geospeedometers Mantle characteristics processing Planetary differentiation Crustal structure Crustal dynamics Mars Exploration Rover Mission, JPL, NASA
Unaltered igneous rock has already proven invaluable Coupling to meteorites to show fractionation processes Using Backstay as an evolved hawaiite linked the experimental phase equilibria of a magma with Backstay composition with melt inclusions in the Chassigny dunite. showed that this meteorite may have been a cognate xenolith brought to the surface during an eruption of residual melt constrained the magmatic water content of the Chassigny parent. Nekvasil et al. (2009)
Coupling to surface spectroscopy Using Humphrey (Adirondack Class) as a relatively primitive basalt from the martian mantle how the martian mantle water budget would produce diverse magmas reaching the surface if fractionating at the base of the martian crust McCubbin et al. (2008) how these lavas would change in composition as the crust thickened McCubbin et al. (2008) how crystallization of these lavas on the surface could produce feldspathic rocks of the type seen at Nili Patera and Noachis Terra. Rogers and Nekvasil 2015
Lending insight into alteration processes from high to low temperature
Gusev Crater/Columbia Hills http://marsnext.jpl.nasa.gov/scieng_geo.cfm
3.65 3.65 Ga Ga Wrinkle Wrinkle- -ridged Plains of Gusev ridged Plains of Gusev ( (Early Hesperian) Early Hesperian) Columbia Hills Greeley et al. (2005)
Columbia Hills are embayed by plains basalt (Adirondack Class; Hamilton and Ruff, 2012), thus are likely at least Late Noachian in age (McCoy et al., 2008) Adirondack Class basalt CTX 2.5 km
Adirondack Class: An ideal sample for tying crater retention age to absolute age CTX 2.5 km
Gusev Crater/Columbia Hills http://marsnext.jpl.nasa.gov/scieng_geo.cfm
Humphrey Adirondack Mazatzal 4. Access to unaltered igneous rock as float Rimming the Tennessee Valley: unaltered to modestly altered, massive, aphanitic, alkaline basalts of the Irvine (tholeiitic basalt) and Backstay classes (trachybasalt) are found as exotics [McSween et al., 2006a; Ruff et al., 2006], Adirondack class basalts (picritic basalt) also present, that are prevalent on the plains [McSween et al., 2004, 2006b]. Backstay Irvine Irvine class basalts also dominate the Inner Basin of the Columbia Hills to the south of Husband Hill [Crumpler et al., 2007]. McCoy et al., 2008 Ming et al 2008
Irvine class basalts also dominate the Inner Basin of the Columbia Hills to the south of Husband Hill, where they are often vesicular to scoriaceous [Crumpler et al., 2007]. Descartes class rocks are breccias with angular clasts that can reach a centimeter in size. The origin of these rocks is uncertain, but aqueous alteration of either a pyroclastic volcanic, impact breccia (McCoy et al. 2008) or impact melt breccia (Arvidson et al. 2008). Algonquin series mafic-ultramafic series, olivine rich, relatively unaltered.(Ming et al. 2008) Assemblee: pyroxene+chromite (mantle xenoliths?) Algonquin/Comanche subclass: olivine+pyroxene (ultramafic? .
AlgonquinClass mafic-ultramafic series, olivine rich, relatively unaltered (Ming et al. 2008) Husband Hill Algonquin Class outcrops, including Comanche, appear to be tephra deposits (Ruff et al., 2014) Home Plate
Algonquin - Miami Morphologic And Thermal Expression Comanche/Algonquin outcrops display distinctive knob and ridge morphology and higher thermal inertia than surrounding terrain HiRISE 250 m Comanche THEMIS colorized night IR over CTX
Morphologic And Thermal Expression Additional examples of Comanche/Algonquin- like terrain in kipukas HiRISE: All scenes 250 m across Columbia Hills Promised Land Interpreted by Ruff et al. (2014) as remnants of formerly more extensive Algonquin-like tephra deposits that mantled the region and were eroded prior to flood basalts at 3.65 Ga (Greeley et al., 2005) Italy feature 3 km THEMIS colorized night IR over CTX
With PIXL, SuperCam, SHERLOC Many diverse samples from mainly igneous signature Martian atmosphere Sulfates and chlorides on the surface VOLATILE BUDGET Distribution of volatiles (Cl, Br, Zn, S) in Coatings/dust Igneous P-T HISTORY Geothermometry Geobarometry Oxygen fugacity Phase equilibria Fluid characteristics FRACTIONATION PROCESSES Mineral composition Residual glass Trace element variability SOURCE CHARACTERISTICS Mineral composition Trace element load Irvine Backstay Assemblee Mantle characteristics processing Planetary differentiation Crustal structure Crustal dynamics Mars Exploration Rover Mission, JPL, NASA
Martian atmosphere Sulfates and chlorides on the surface To increasing alteration signatures With PIXL, SuperCam, SHERLOC Igneous P-T HISTORY Geothermometry Geobarometry Oxygen fugacity Phase equilibria INTERACTION WITH/LOSS OF VOLATILES Distribution of volatiles (Cl, Br, Zn, S) in matrix and or surface Changes in mineral composition Changes in trace element load FRACTIONATION PROCESSES Mineral composition Residual glass Trace element variability Wishstone Everett Peace Vapor deposits? Brines? Magmatic or meteoric water? Crustal structure Crustal dynamics Mars Exploration Rover Mission, JPL, NASA
Diverse Igneous Geology in and around the Columbia Hills for Diverse Science Investigations
