Subject |
has part mean Ni content of sulfide |
has weather resistance |
has part carbon |
has alteration temperature range |
has synonym |
has olivine shock metamorphism |
has part matrix |
has prototype |
is independent of |
has shock pressure |
has acronym |
has matrix abundance |
has sediment mechanism |
has image |
has weather |
has degree of secondary process |
has part feldspar |
has metal abundance |
has refractory inclusion abundance |
has relative abundance |
has fragmentation probability |
has chondrule mean diameter |
has metamorphism mechanism |
has weathering stage |
is a kind of |
has age |
has part sulfide Ni content |
has part maximum bulk Ni in metal |
has oxidation state |
has definition |
has number of find |
has petrologic type |
has find date |
has comment |
has part water |
has degree of thermal metamorphism |
has orthopyroxene shock metamorphism |
has plagioclase shock metamorphism |
has degree of shock metamorphism |
has mass |
has peak temperature |
has shock diagnostic mineral |
has name |
be shock |
has fall location |
is an instance of |
has shock stage |
has part metal maximum bulk |
has homogeneity of olivine and low Ca pyroxene |
has composition |
has structural state of low Ca pyroxene |
has value |
has fall coordinate |
has olivine and low Ca pyroxene homogeneity |
has ablative mass loss |
has total mass of find |
has chondrule abundance |
has parent body |
has part chondrule |
has petrologic type range |
Hammadah al Hamra meteorite | | which depends on its composition | | | | | | | | | HaH | | | | can be severe due to long exposure time to environmental corrosion agents | | | | | | during meteor phase which depends on composition | | | | Sahara meteorite | | | | | | 1691 | | when the meteorite was found | | | | | | | | | | based on the locale, region, or nearby town in which the fall occurred | | Hammadah al Hamra | | | | | often minerals not found on Earth | | lower because the fall was not witnessed | in degrees, minutes and seconds of lattitude and longitude | | directly proportional to initial velocity | 485755 kg | | | | |
meteorite find | | which depends on its composition | | | | | | | | | | | | | can be severe due to long exposure time to environmental corrosion agents | | | | | | during meteor phase which depends on composition | | | | meteorite | | | | | a meteorite whose fall was not witnessed | 1691 | | when the meteorite was found | | | | | | | | | | based on the locale, region, or nearby town in which the fall occurred | | strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity | | | | | often minerals not found on Earth | | lower because the fall was not witnessed | in degrees, minutes and seconds of lattitude and longitude | | directly proportional to initial velocity | 485755 kg | | | | |
R chondrite | in weight % | low | in weight % | | rumurutiite | | fine grained disequilibrium mixture of silicates, oxides, metal, sulfides and organic constituents | Rumuruti meteorite | | | | 36 % by volume | agglomeration of particles, many of which record individual, diverse histories | | | | usually plagioclase tectosilicate | 0.1 % by volume | 0 % by volume | 85.7 % of meteorite falls | high because it is more friable than iron meteorite | 0.4 millimeters | | | anhydrous chondrite | oldest and most primitive rock in solar system | | | highly oxidized | | 1030 | 3 to 6 | | | 0 % by weight (approximately) | | | | | | less than 950 degree Celsius during its entire history since solidification | | based on the locale, region, or nearby town in which the fall occurred | | strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity | | | in weight % | definition goes here | enriched in 17O isotope | definition goes here | | in degrees, minutes and seconds of lattitude and longitude | | high because it is more friable than iron meteorite | 20461 kg | greater than 40 % by volume | asteroid smaller than 100 km in diameter | small sphere of about 1 mm diameter of formerly melted minerals | which depends on degree of aqueous alteration and thermal metamorphism |
S3 shock stage chondrite | in weight % | which depends on its composition | in weight % | | | planar fractures, undulatory extinction, irregular fractures | fine grained disequilibrium mixture of silicates, oxides, metal, sulfides and organic constituents | | the nature and degree of thermal metamorphism or aqueous alteration | 15 to 20 GPa | | in volume % | agglomeration of particles, many of which record individual, diverse histories | | | providing insight into geological evolution of parent asteroid | usually plagioclase tectosilicate | in volume % | in volume % | | during meteor phase which depends on composition | millimeters | shock metamorphism | | S3 shock stage meteorite | oldest and most primitive rock in solar system | | | | | 1691 | | | | in weight % | | clinoenstatite lamellae on (100), undulatory extinction, planar fractures, irregular fractures | undulatory extinction | weakly shocked | | less than 950 degree Celsius during its entire history since solidification | orthopyroxene for enstatite chondrite | based on the locale, region, or nearby town in which the fall occurred | before, during or after other types of metamorphism | strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity | | S3 | in weight % | definition goes here | often minerals not found on Earth | definition goes here | | in degrees, minutes and seconds of lattitude and longitude | | directly proportional to initial velocity | 485755 kg | in volume % | asteroid smaller than 100 km in diameter | small sphere of about 1 mm diameter of formerly melted minerals | which depends on degree of aqueous alteration and thermal metamorphism |
type 4 chondrite | in weight % | low | less than 0.2 % by weight | the range over at which the alteration took place | | | transparent, recrystallized, small crystals | | | | | in volume % | agglomeration of particles, many of which record individual, diverse histories | | | providing insight into geological evolution of parent asteroid | secondary, grains than 2 microns | in volume % | in volume % | 85.7 % of meteorite falls | high because it is more friable than iron meteorite | millimeters | thermal metamorphism | | anhydrous chondrite | oldest and most primitive rock in solar system | less than 0.5 % by weight | greater than 20 % by weight, kamacite and taenite in exsolution relationship | | | 1030 | 4 | | | less than 1.5 % by weight | weak | | | | | less than 950 degree Celsius during its entire history since solidification | | based on the locale, region, or nearby town in which the fall occurred | | strewn fields, elongated footprints which depends on impact angle, airbursts, and impact velocity | | | in weight % | definition goes here | often minerals not found on Earth | greater than 20 % monoclinic | | in degrees, minutes and seconds of lattitude and longitude | less than 5 % mean deviations | high because it is more friable than iron meteorite | 20461 kg | in volume % | asteroid smaller than 100 km in diameter | chondrules well defined | which depends on degree of aqueous alteration and thermal metamorphism |
HaH 119 | in weight % | which depends on its composition | less than 0.2 % by weight | the range over at which the alteration took place | rumurutiite | planar fractures, undulatory extinction, irregular fractures | transparent, recrystallized, small crystals | Rumuruti meteorite | the nature and degree of thermal metamorphism or aqueous alteration | 15 to 20 GPa | HaH | 36 % by volume | agglomeration of particles, many of which record individual, diverse histories |
 | can be severe due to long exposure time to environmental corrosion agents | providing insight into geological evolution of parent asteroid | secondary, grains than 2 microns | 0.1 % by volume | 0 % by volume | | during meteor phase which depends on composition | 0.4 millimeters | thermal metamorphism | W4 | | oldest and most primitive rock in solar system | less than 0.5 % by weight | greater than 20 % by weight, kamacite and taenite in exsolution relationship | highly oxidized | | 1691 | 4 | April 1995 | unbecciated | less than 1.5 % by weight | weak | clinoenstatite lamellae on (100), undulatory extinction, planar fractures, irregular fractures | undulatory extinction | weakly shocked | 0.352 kg | less than 950 degree Celsius during its entire history since solidification | orthopyroxene for enstatite chondrite | HaH 119 | before, during or after other types of metamorphism | Hammadah al Hamra | S3 shock stage chondrite | S3 | in weight % | definition goes here | enriched in 17O isotope | greater than 20 % monoclinic | lower because the fall was not witnessed | 28° 30.87' N., 12° 53.81' E. | less than 5 % mean deviations | directly proportional to initial velocity | 485755 kg | greater than 40 % by volume | asteroid smaller than 100 km in diameter | chondrules well defined | which depends on degree of aqueous alteration and thermal metamorphism |