Havero Comparison Table

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rock > igneous rock > differentiated meteorite > differentiated achondrite > asteroidal achondrite > ureilite > monomict ureilite > Havero

Next meteorite fall: Holbrook Up: meteorite fall, monomict ureilite, mosaicized ureilite Previous meteorite fall: Grosnaja

Havero comparison table

Subject 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 olivine grain characteristic has fall date 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 fall description 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 original texture has number of find has origin has ablative mass loss has shock pressure has solidification timescale has plagioclase has pigeonite composition has definition has intergranular boundary has gain size has pyroxene content has petrology

meteorite fall which depends on its composition during meteor phase which depends on composition recorded by eyewitness or instruments what witnesses saw or what was recorded by instruments negligible due to quick recovery of meteorite before corrosion begins 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cooling in deep underground chambers AURE 7.1 % of meteorite falls large, anhedral olivine and pyroxene grains 9 kg (out of date) carbon, metal, sulfides small silicate grains along grain boundaries less than 10% by volume olivine-pigeonite about 90% by volume silicates (with very few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

mosaicized ureilite which depends on its composition olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) shock melted shock melted 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 shock metamorphism mottled by melt glass partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite completely shattered or mosaicized AURE mosaicized 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 shock melted meteorite visible via dark matrix outlining relict grain boundaries of large, elongate grains, and a common preferred orientation of grains within relict domains -has source: Berkley JL, Taylor GJ, Keil K. Harlow GE, Prinz M 1980, Geochim Cosmochim Acta 44, 1579 -has URL: http://adsabs.harvard.edu/cgi-bin/bib_query?1980GeCoA..44.1579B 6 (out of date) asteroid directly proportional to initial velocity 100 GPa or greater very slow much less than 1 mm coarse-grained granular

Havero which depends on its composition Berkley et. al (1980) olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite) shock melted shock melted 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 shock metamorphism mottled by melt glass partial melting residue cooling in deep underground chambers diamonds and/or lonsdaleite Fo% 79 completely shattered or mosaicized what witnesses saw or what was recorded by instruments negligible due to quick recovery of meteorite before corrosion begins AURE mosaicized 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 visible via dark matrix outlining relict grain boundaries of large, elongate grains, and a common preferred orientation of grains within relict domains -has source: Berkley JL, Taylor GJ, Keil K. Harlow GE, Prinz M 1980, Geochim Cosmochim Acta 44, 1579 -has URL: http://adsabs.harvard.edu/cgi-bin/bib_query?1980GeCoA..44.1579B 1691 meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal directly proportional to initial velocity 100 GPa or greater very slow 0 % Wo% 2.5 En% 81 clinobronzite curved meeting in triple junctions much less than 1 mm 0.17 in modal pyroxene/(pryroxene+olivine) coarse-grained granular

Next meteorite fall: Holbrook Up: meteorite fall, monomict ureilite, mosaicized ureilite Previous meteorite fall: Grosnaja

Subject	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 olivine grain characteristic	has fall date	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 fall description	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 original texture	has number of find	has origin	has ablative mass loss	has shock pressure	has solidification timescale	has plagioclase	has pigeonite composition	has definition	has intergranular boundary	has gain size	has pyroxene content	has petrology
meteorite fall	which depends on its composition							during meteor phase which depends on composition		recorded by eyewitness or instruments								what witnesses saw or what was recorded by instruments	negligible due to quick recovery of meteorite before corrosion begins				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
mosaicized ureilite	which depends on its composition		olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	shock melted	shock melted		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	shock metamorphism	mottled by melt glass	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite		completely shattered or mosaicized			AURE		mosaicized		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	shock melted meteorite	visible via dark matrix outlining relict grain boundaries of large, elongate grains, and a common preferred orientation of grains within relict domains -has source: Berkley JL, Taylor GJ, Keil K. Harlow GE, Prinz M 1980, Geochim Cosmochim Acta 44, 1579 -has URL: http://adsabs.harvard.edu/cgi-bin/bib_query?1980GeCoA..44.1579B	6 (out of date)	asteroid	directly proportional to initial velocity	100 GPa or greater	very slow					much less than 1 mm		coarse-grained granular
Havero	which depends on its composition	Berkley et. al (1980)	olivine, pyroxene (some combination of pigeonite, orthopyroxene, augite)	shock melted	shock melted	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	shock metamorphism	mottled by melt glass	partial melting residue	cooling in deep underground chambers	diamonds and/or lonsdaleite	Fo% 79	completely shattered or mosaicized	what witnesses saw or what was recorded by instruments	negligible due to quick recovery of meteorite before corrosion begins	AURE		mosaicized	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		visible via dark matrix outlining relict grain boundaries of large, elongate grains, and a common preferred orientation of grains within relict domains -has source: Berkley JL, Taylor GJ, Keil K. Harlow GE, Prinz M 1980, Geochim Cosmochim Acta 44, 1579 -has URL: http://adsabs.harvard.edu/cgi-bin/bib_query?1980GeCoA..44.1579B	1691	meteoroid from interplanetary space or fragment dislodged from another planet, moon or planetesimal	directly proportional to initial velocity	100 GPa or greater	very slow	0 %	Wo% 2.5 En% 81 clinobronzite		curved meeting in triple junctions	much less than 1 mm	0.17 in modal pyroxene/(pryroxene+olivine)	coarse-grained granular