Hughes 009 Comparison Table

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rock > igneous rock > differentiated meteorite > differentiated achondrite > asteroidal achondrite > ureilite > medium shock ureilite > Hughes 009

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Hughes 009 comparison table

Subject has weather resistance has shock texture has reference has minerology has degree of shock metamorphism has shock stage is an instance of has distinguishing feature has orthopyroxene composition has fragmentation probability has olivine grain characteristic has pyroxene shock metamorphism has metamorphism mechanism has likely origin has solidification mechanism has shock diagnostic mineral has olivine composition has olivine shock metamorphism has weather has letter designation has relative abundance has texture has value has total mass of find has matrix composition has characteristic mineral has composition is a kind of has find date has augite composition has number of find has origin has ablative mass loss has shock pressure has solidification timescale has plagioclase has intergranular boundary has definition has gain size has pyroxene content has petrology

medium shock ureilite which depends on its composition greater extent of fracturing, undulatory extinction, and kink banding olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) medium S4-S6 no chondrules during meteor phase which depends on composition reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal may be cloudy due to glassy inclusions shock metamorphism partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite sub-grain boundaries may be prominent AURE 9 kg (out of date) carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume often minerals not found on Earth S6 shock stage meteorite 6 (out of date) asteroid directly proportional to initial velocity from 20 GPa to 100 GPa very slow coarse-grained granular

meteorite find which depends on its composition during meteor phase which depends on composition can be severe due to long exposure time to environmental corrosion agents lower because the fall was not witnessed 485755 kg often minerals not found on Earth meteorite when the meteorite was found 1691 meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal directly proportional to initial velocity a meteorite whose fall was not witnessed

monomict ureilite low olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) no chondrules high because it is more friable than iron meteorite reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal partial melting residue cooling in deep underground chambers AURE 7.1 % of meteorite falls large, anhedral olivine and pyroxene grains 9 kg (out of date) carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume silicates (with very few exceptions) ureilite 6 (out of date) asteroid high because it is more friable than iron meteorite very slow 0 % curved meeting in triple junctions 1 mm coarse-grained granular

Hughes 009 which depends on its composition greater extent of fracturing, undulatory extinction, and kink banding Wlotzka (1994), Goodrich (1998) olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) medium S4-S6 meteorite find no chondrules Wo% 4.9 En% 84 during meteor phase which depends on composition reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal may be cloudy due to glassy inclusions shock metamorphism partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite Fo% 87 sub-grain boundaries may be prominent can be severe due to long exposure time to environmental corrosion agents AURE large, anhedral olivine and pyroxene grains lower because the fall was not witnessed 485755 kg carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume often minerals not found on Earth when the meteorite was found Wo% 37 En% 56 1691 meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal directly proportional to initial velocity from 20 GPa to 100 GPa very slow 0 % curved meeting in triple junctions 1 mm 0.7 in modal pyroxene/(pryroxene+olivine) coarse-grained granular

Next medium shock ureilite: Jalanash Up: medium shock ureilite, meteorite find, monomict ureilite Previous medium shock ureilite: Hajma

Subject	has weather resistance	has shock texture	has reference	has minerology	has degree of shock metamorphism	has shock stage	is an instance of	has distinguishing feature	has orthopyroxene composition	has fragmentation probability	has olivine grain characteristic	has pyroxene shock metamorphism	has metamorphism mechanism	has likely origin	has solidification mechanism	has shock diagnostic mineral	has olivine composition	has olivine shock metamorphism	has weather	has letter designation	has relative abundance	has texture	has value	has total mass of find	has matrix composition	has characteristic mineral	has composition	is a kind of	has find date	has augite composition	has number of find	has origin	has ablative mass loss	has shock pressure	has solidification timescale	has plagioclase	has intergranular boundary	has definition	has gain size	has pyroxene content	has petrology
medium shock ureilite	which depends on its composition	greater extent of fracturing, undulatory extinction, and kink banding		olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	medium	S4-S6		no chondrules		during meteor phase which depends on composition	reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal	may be cloudy due to glassy inclusions	shock metamorphism	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite		sub-grain boundaries may be prominent		AURE				9 kg (out of date)	carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume	olivine-pigeonite about 90% by volume	often minerals not found on Earth	S6 shock stage meteorite			6 (out of date)	asteroid	directly proportional to initial velocity	from 20 GPa to 100 GPa	very slow						coarse-grained granular
meteorite find	which depends on its composition									during meteor phase which depends on composition									can be severe due to long exposure time to environmental corrosion agents				lower because the fall was not witnessed	485755 kg			often minerals not found on Earth	meteorite	when the meteorite was found		1691	meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal	directly proportional to initial velocity					a meteorite whose fall was not witnessed
monomict ureilite	low			olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)				no chondrules		high because it is more friable than iron meteorite	reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal			partial melting residue	cooling in deep underground chambers					AURE	7.1 % of meteorite falls	large, anhedral olivine and pyroxene grains		9 kg (out of date)	carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume	olivine-pigeonite about 90% by volume	silicates (with very few exceptions)	ureilite			6 (out of date)	asteroid	high because it is more friable than iron meteorite		very slow	0 %	curved meeting in triple junctions		1 mm		coarse-grained granular
Hughes 009	which depends on its composition	greater extent of fracturing, undulatory extinction, and kink banding	Wlotzka (1994), Goodrich (1998)	olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	medium	S4-S6	meteorite find	no chondrules	Wo% 4.9 En% 84	during meteor phase which depends on composition	reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal	may be cloudy due to glassy inclusions	shock metamorphism	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite	Fo% 87	sub-grain boundaries may be prominent	can be severe due to long exposure time to environmental corrosion agents	AURE		large, anhedral olivine and pyroxene grains	lower because the fall was not witnessed	485755 kg	carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume	olivine-pigeonite about 90% by volume	often minerals not found on Earth		when the meteorite was found	Wo% 37 En% 56	1691	meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal	directly proportional to initial velocity	from 20 GPa to 100 GPa	very slow	0 %	curved meeting in triple junctions		1 mm	0.7 in modal pyroxene/(pryroxene+olivine)	coarse-grained granular