Lahrauli Comparison Table

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rock > igneous rock > differentiated meteorite > differentiated achondrite > asteroidal achondrite > ureilite > medium shock ureilite > Lahrauli

Next medium shock ureilite: LEW 88774 Up: medium shock ureilite, meteorite fall, monomict ureilite Previous medium shock ureilite: Kenna

Lahrauli 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 fragmentation probability has olivine grain characteristic has fall date 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 fall description 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 number of find has origin has ablative mass loss has shock pressure has solidification timescale has plagioclase has pigeonite composition has intergranular boundary has definition has gain size 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 recorded by eyewitness or inferred from dating methods 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cooling in deep underground chambers diamonds and/or lonsdaleite sub-grain boundaries may be prominent AURE 9 kg (out of date) carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume often minerals not found on Earth S6 shock stage meteorite 6 (out of date) asteroid directly proportional to initial velocity from 20 GPa to 100 GPa very slow coarse-grained granular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 fall which depends on its composition during meteor phase which depends on composition recorded by eyewitness or instruments negligible due to quick recovery of meteorite before corrosion begins what witnesses saw or what was recorded by instruments higher because the fall was witnessed 485755 kg often minerals not found on Earth meteorite 1691 meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal directly proportional to initial velocity a meteorite whose fall was witnessed by human or electronic means

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 recorded by eyewitness or inferred from dating methods 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

Lahrauli which depends on its composition greater extent of fracturing, undulatory extinction, and kink banding Malhotra (1962), Bhandari et al. (1981) olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) medium S4-S6 meteorite fall 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 recorded by eyewitness or instruments may be cloudy due to glassy inclusions shock metamorphism partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite Fo% 79 sub-grain boundaries may be prominent negligible due to quick recovery of meteorite before corrosion begins what witnesses saw or what was recorded by instruments AURE large, anhedral olivine and pyroxene grains higher because the fall was 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 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 % Wo% 7.7 En% 74 curved meeting in triple junctions 1 mm coarse-grained granular

Next medium shock ureilite: LEW 88774 Up: medium shock ureilite, meteorite fall, monomict ureilite Previous medium shock ureilite: Kenna

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 fragmentation probability	has olivine grain characteristic	has fall date	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 fall description	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 number of find	has origin	has ablative mass loss	has shock pressure	has solidification timescale	has plagioclase	has pigeonite composition	has intergranular boundary	has definition	has gain size	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	recorded by eyewitness or inferred from dating methods	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 fall	which depends on its composition								during meteor phase which depends on composition		recorded by eyewitness or instruments								negligible due to quick recovery of meteorite before corrosion begins	what witnesses saw or what was recorded by instruments				higher because the fall was witnessed	485755 kg			often minerals not found on Earth	meteorite	1691	meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal	directly proportional to initial velocity						a meteorite whose fall was witnessed by human or electronic means
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	recorded by eyewitness or inferred from dating methods			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
Lahrauli	which depends on its composition	greater extent of fracturing, undulatory extinction, and kink banding	Malhotra (1962), Bhandari et al. (1981)	olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	medium	S4-S6	meteorite fall	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	recorded by eyewitness or instruments	may be cloudy due to glassy inclusions	shock metamorphism	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite	Fo% 79	sub-grain boundaries may be prominent	negligible due to quick recovery of meteorite before corrosion begins	what witnesses saw or what was recorded by instruments	AURE		large, anhedral olivine and pyroxene grains	higher because the fall was 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		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 %	Wo% 7.7 En% 74	curved meeting in triple junctions		1 mm	coarse-grained granular