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• W2588760160 abstract "ANATOMY OF A CLUSTER IDP (II): NOBLE GAS ABUNDANCES, TRACEELEMENT GEOCHEMISTRY, ISOTOPIC ABUNDANCES, AND TRACE ORGANICCHE3MISTRY OF SEVERAL FRAGMENTS FROM L200805; K.L. Thomas 1, S. J. Clemett 2 , G. J.Hynn , L. P. KeUer 4, D. S. McKay 5, S Messenger 6, A O Nier 7, D J Schlutter 7 S R Sutton 8 R. MWalker6, andR. N. Zare 2; 1Lockheed2400NasaRd. 1Honston, TX,'77058, 2Depl. of Chemi_y[ SMVAtanfordUniversity, Stanford, CA 94305, 3Dept. of Physics, SUNY-Plattsburgh, Plattsburgh, NY 12901,Inc., 5500/State 200 Oakbrook Pkwy., Norcross, GA 30093, 5NASA/JSC, SN, Houston, TX/777058, 6McDonnel Center for the Space Sciences, Physics Dept., Washington University, St. Louis, MO63130, 7School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, 8Dept. ofGeophysical Sciences, The University of Chicago, Chicago, IL 60637In Part I, we described the bulk chemistry and mineralogy of large fragments and fines (<5 tun)from a cluster IDP originally ~ 40-50 tun in diameter [1]. Here we report results from several types ofanalyses: noble gas measurements (Nier), Synchrotron X-Ray Fluorescence (SXRF) for trace elementabundances (Flynn and Sutton), ion probe studies (Messenger and Walker), and trace organic chemistry(Clemett and Zare). The same fragments were analyzed for isotopic abundances and organic compounds.Noble Gas Content _d R¢!¢_¢ Temeeratures He content and the He release temperatures for foursamples were determined by step-heating experiments [2]. The average 4He abundance is --4.1 (ccx 1011)and extraction temperatures for removal of 50% of the He range from 750-1040 °C, with an average at 928°C (Table 1). The low He content and high release temperatures indicate that all fragments from L2008#5have experienced heating during atmospheric entry. He measurements have been used to distinguishasteroidal from cometary IDPs in individual, small-sized particles (< 10 pm in diameter) [3]; however thesemeasurements cannot be used to determine sources of cluster particles because higher deceleration heatingoccurs in large-size particles.Trace Element Abundances SXRF was used to determinetrace element abundances in four fi'agmentsfrom L2008#5 [technique described in 4]. Two fragments show marked depletions in Zn (Zn/Fe < 0.1)indicating they have experienced heating during atmospheric entry (Table 2). Zn/Fe ratios range from 0.2-0.5 for the _ fragments. All four fragments show deviations by more than a factor of 2 from CIfor 3 or more elements (Table 2). The only consistent trends are enrichments in Cu, Se, and Br, and adepletion in Zn relative to CI.Heating Summary of Cluster Fraements He content and release temperatures of fines suggest theyexperienced atmospheric entry heating. The large range in 50% He release temperatures suggests thatfragments have not been heated equally. Low Zn/Fe ratios show that 2 of 4 fiagments were heated duringatmospheric entry. Previous TEM studies have shown that the presence of magnetite rims on IDP surfacesis an indication of atmospheric entry heating [e.g., 5]. Magnetite rims were observed in 13 of 20 fragmentsand fines from this cluster[l]. The He measurements indicate that cluster L2008#5 has not been uniformlyheated;trace element abundances and magnetite rims are evidence that heating is seen-inselectedfrasments, probably those located on the exterior surfaces of the cluster.Isotopic Measurem¢nt_ D/H ratios of eight fragments were measured using an ion microprobe [techniquedescribed in 6]. Deuterium enrichments (SD) were observed in all four of the C-rich fragments and rangefrom +322- +822 per rail. Four fragments from C1u37, which had a chondritic C abundance, showed no Denri_ (Table 3). The D enrichments in the C-rich fragments are far in excess of values for terrestrialsamples and are another indication that the fragments are extraterrestrial [6]. There is an apparent positivecorrelation of D enrichment with the abundance of carbonaceous material in our fragments. A larger groupof IDPs should be examined to confirm this result.Trace Organic Chcmi_t_ The signatures ofpolycyclic aromatic hydrocarbons (PAHs) in lDPs have beenobserved with a microprobe two-step laser mass spectrometer (tdo2MS) [7]. All cluster fiagnmts whichhad been analyzed previously for isotopic abundances were examined for the presence of PAHs (Table 3)." @default.
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• W2588760160 title "ANATOMY OF A CLUSTER IDP (II): NOBLE GAS ABUNDANCES, TRACE ELEMENT GEOCHEMISTRY, ISOTOPIC ABUNDANCES, AND TRACE ORGANIC" @default.
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