HaH 126 Comparison Table

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rock > igneous rock > differentiated meteorite > differentiated achondrite > asteroidal achondrite > ureilite > medium shock ureilite > HaH 126

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HaH 126 comparison table

Subject has shock texture has weather resistance has reference has minerology has degree of shock metamorphism has shock stage is an instance of has distinguishing feature has fragmentation probability has fall location has olivine grain characteristic has metamorphism mechanism has pyroxene shock metamorphism has likely origin has solidification mechanism has shock diagnostic mineral has olivine composition has olivine shock metamorphism has weather has letter designation has acronym 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 number of find has origin has ablative mass loss has shock pressure has solidification timescale has plagioclase has pigeonite composition has intergranular boundary has gain size has pyroxene content has petrology

Hammadah al Hamra meteorite which depends on its composition during meteor phase which depends on composition Hammadah al Hamra can be severe due to long exposure time to environmental corrosion agents HaH lower because the fall was not witnessed 485755 kg often minerals not found on Earth Sahara 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

medium shock ureilite greater extent of fracturing, undulatory extinction, and kink banding which depends on its composition olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) medium S4-S6 no chondrules during meteor phase which depends on composition strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal shock metamorphism may be cloudy due to glassy inclusions 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cooling in deep underground chambers diamonds and/or lonsdaleite sub-grain boundaries may be prominent AURE 9 kg (out of date) carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume often minerals not found on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

monomict ureilite low olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) no chondrules high because it is more friable than iron meteorite strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity 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

HaH 126 greater extent of fracturing, undulatory extinction, and kink banding which depends on its composition Weber and Bischoff (1996), Sexton et al. (1996), Chikami et al. (1997b) olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) medium S4-S6 Hammadah al Hamra meteorite no chondrules during meteor phase which depends on composition Hammadah al Hamra reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal shock metamorphism may be cloudy due to glassy inclusions partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite Fo% 79 sub-grain boundaries may be prominent can be severe due to long exposure time to environmental corrosion agents AURE HaH large, anhedral olivine and pyroxene grains lower because the fall was not witnessed 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 when the meteorite was found 6 (out of date) 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% 8.4 En% 74 curved meeting in triple junctions 1 mm 0.3 in modal pyroxene/(pryroxene+olivine) coarse-grained granular

Next Hammadah al Hamra meteorite: HaH 180 Up: Hammadah al Hamra meteorite, medium shock ureilite, monomict ureilite Previous Hammadah al Hamra meteorite: HaH 119

Subject	has shock texture	has weather resistance	has reference	has minerology	has degree of shock metamorphism	has shock stage	is an instance of	has distinguishing feature	has fragmentation probability	has fall location	has olivine grain characteristic	has metamorphism mechanism	has pyroxene shock metamorphism	has likely origin	has solidification mechanism	has shock diagnostic mineral	has olivine composition	has olivine shock metamorphism	has weather	has letter designation	has acronym	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 number of find	has origin	has ablative mass loss	has shock pressure	has solidification timescale	has plagioclase	has pigeonite composition	has intergranular boundary	has gain size	has pyroxene content	has petrology
Hammadah al Hamra meteorite		which depends on its composition							during meteor phase which depends on composition	Hammadah al Hamra									can be severe due to long exposure time to environmental corrosion agents		HaH			lower because the fall was not witnessed	485755 kg			often minerals not found on Earth	Sahara 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
medium shock ureilite	greater extent of fracturing, undulatory extinction, and kink banding	which depends on its composition		olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	medium	S4-S6		no chondrules	during meteor phase which depends on composition	strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity	reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal	shock metamorphism	may be cloudy due to glassy inclusions	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
monomict ureilite		low		olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)				no chondrules	high because it is more friable than iron meteorite	strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity	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
HaH 126	greater extent of fracturing, undulatory extinction, and kink banding	which depends on its composition	Weber and Bischoff (1996), Sexton et al. (1996), Chikami et al. (1997b)	olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	medium	S4-S6	Hammadah al Hamra meteorite	no chondrules	during meteor phase which depends on composition	Hammadah al Hamra	reduced rims contacting carbonaceous matrix material 0.1 mm FeO-free olivine and/or enstatite rims riddled with tiny inclusions of low-Ni metal	shock metamorphism	may be cloudy due to glassy inclusions	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite	Fo% 79	sub-grain boundaries may be prominent	can be severe due to long exposure time to environmental corrosion agents	AURE	HaH		large, anhedral olivine and pyroxene grains	lower because the fall was not witnessed	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		when the meteorite was found	6 (out of date)	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% 8.4 En% 74	curved meeting in triple junctions	1 mm	0.3 in modal pyroxene/(pryroxene+olivine)	coarse-grained granular