meteorites

meteorites - Cup-right music-:1 Hefracmw inclusiuns...

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Unformatted text preview: Cup-right music-:1 Hefracmw inclusiuns "Fluffy" Type A CAI'E Lug Afmudumrfi, Sflhrr Phurusphsra I2 H1 ha 1f 4 {i .5 m Lag Abmm‘mmn {T I Chflfldrfftfi IE 9.6.7.3 0.72 30.71 Tieschitz 4.52 i 0.03 Billion Years 0.1 0.2 0.3 87Hb/87Sr 0.4 0.5 EMS SM F‘v’ Angfilcs —I—I—I—l—l— l PhIPh ages Chan-drulub; j. Al-Mgagm I Mn-Fragcs: {A15 5M F‘IJ 1.5:; - - .~_- —l—l—h—l—i-— 1' L db“ C hmldnlles SM F‘u' Angritcs ——I———I——-I-——I——-CI-— {Thflndmlm anchnr 5M Acapulcn anclmr 455131 4555 45m 4555 4555 4555 Age: {millifln yams hafnr: pregnant) ILEEinnEIrJI Condensation Sequence 1 400 Refractory Inclusions 1100 .................................... -- ' 6‘ 9., g Plagioclase E Olivineleroxene g with higher iron content gm Id _ 150 __ m- 1 .— ._ .._ __ M. “c Manhunh 41'an o rnnlinrr nphnlnr (rm: nf 6170 (per min Terrestrial Samples TABLE I Observational Constraints for Chondrule and CAI Formation Models Constraint Supporting observations Essential constraints for which a model must account: High efficiency High chondrule abundances Nebular timescales only Isotopic dating Low ambient temperature Presence of volatiles Short heating time (minutes) Retention of volatiles; preservation of relict grains; experimental reproduction of textures Peak temperatures ~2000 K Experimental reproduction of textures Short cooling time (hours) Experimental reproduction of textures; zoning in minerals; presence of glass Localized process Limited size range in each chondrite group; differences in O isotopic composition Multiple episodes; recycling Relict grains; compound chondmles; igneous rims Magnetic field Remanent magnetization Constraints not firmly accepted by meteoriticists: Chondrule formation ~2 Myr Short-lived radioisotope data after CAI formation Elevated gas pressure Stability of molten chondrule Variable nebular oxidation states Variable oxidation states of chondrules Well-defined observations for which a heating model does not necessarily need to account: Size sorting Restricted size range in each chondrite group Presence of dust that escapes Fine-grained rims heating Copy-nng NEMS. 20m Chondrite Parent Bodies 93 Asteroid and Meteorite Spectra Mineral Spectra 0.5 0.4 0.3 a: o E 0.2 L4 Ordinary Chondrire ‘g o g . 8 u: Serpentine Q < 01 ' E4 Enstatile Chondrite Ahab-— 0.06 Asphaltite 0M2 arbonaceous Chondrite 004 Magnetite 0.4 0.8 1.2 1.6 2.0 0.3 0.6 0.9 1.2 1.5 1.8 2.1 2.4 Wavelength (urn) Wavelength ( um) Eccentricity 0.15 0.10 Orbits of Vestoids 4 Vesta '. c 3I1 Resonance 2.4 Semimajor Axis (AU) 2.5 Ordinary Chan dritss Carbonacwm Cfmndrfm Achflndnres Imm Storylfllmns Figure 10.11. Relative abundance of maier typea of meteorites Falls. Chundrites Elfh-flfilflfl-Lt‘l: chandfltal Errdlnarjr Bhnndritaa H Humumli L fihundfita: LL El'llllfltl ChandfltaI—l: EH EL Metachund rites EV GR H Stung-Iran Meteurites Pilillit-H- mulldarllu Achand rites Eustalita- Fril'nathrn Ana put-unite: Antilan Wlnnnaita: Angri‘lu Lnd'ranitu Brlchlntt-u Ll'railltai. HEIIIII Hawardtlns E Eutrlt-M Diuqanita-n Lunir Muflhl Emcciu E Basalt: Ga hhlfll Eharguttit-as Halthlhlu thunlg my ICE MCI'HEITIE'I‘It EII‘Id MEIEDI‘HE Cancentratiun MEIEEIFIIE Ia IIEI. ...
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This note was uploaded on 01/03/2012 for the course GEL 133 taught by Professor List during the Fall '10 term at Caltech.

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meteorites - Cup-right music-:1 Hefracmw inclusiuns...

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