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Applications of Abundance Data and Requirements for Cosmochemical Application Abundancf so e Dat Requirementd aan r sfo Cosmochemical Modeling H. Busemann Binns. R . 1 ,W . Chiappini 2,C Gloeckler. 3,G . Hoppe4,P . 5,D Kirilova Leske. A Manuel. K 6 ,R . Mewaldt. 7,O A . 8,R . Mobius7,E Wider. 9,R 10, Wiens. RC . Wimmer-SchweingruberF . 11,R . YanasakE . N d 1an 7 ^hysikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland 2McDonnell Center for the Space Sciences, Washington University, St. Louis, MO, USA 3Observatory of Trieste, Trieste, Italy 4Department of Physics, University of Maryland, College Park, USA 5Cosmochemistry Department, Max-Planck-Institute Chemistry,for Mainz, Germany 6Institute of Astronomy, Bulgarian Academy of Sciences, Sofia, Bulgaria 7Space Radiation Laboratory, California Institute of Technology, Pasadena, CA,USA 8Department of Chemistry, University of Missouri,USA MO, 9Department of Physics, University of New Hampshire, Durham, NH, USA 10u Institutej for Isotope Geology and Mineral Resources, ETH Zurich, Zurich, Switzerland 1 Space and Atmospheric Sciences, MS D466, Los Alamos National Laboratory, Los Alamos, NM 87545, USA Abstract. Understanding the evolution of the universe from Big Bang to its present state requires an understanding of the evolution of the abundances of the elements and isotopes in galaxies, stars, the interstellar medium, the Sun and the heliosphere, planets and meteorites. Processes that change the state of the universe include Big Bang nucleosynthesis, star formatio stellad nan r nucleosynthesis, galactic chemical evolution, propagatio cosmif no c rays, spallation, ionization and particle transport of interstellar material, formation of the solar system, solar wind emission and its fractionation (FIP/FIT effect), mixing processes in stellar interiors, condensation of material and subsequent geochemical fractionation. Here attempe w , compilo t t e some major issue cosmochemistrn si addressee yb than ca t d wit hbettea r knowledge of the respective element or isotope abundances. Present and future missions such as Genesis, Stardust, Interstellar Pathfinder, and Interstellar Probe, improvements of remote sensing instrumentation and experiments on extraterrestrial material suc meteoritess ha , presolar grains lunad an ,r returne o r d planetar r cometaryo y samples will result in an improved database of elemental and isotopic abundances. This includes the primordial abundances of D, 3He, 4 7Hed Li,an , abundance heaviee th f so r element star n galaxiessi d san compositioe th , interstellae th f no r medium, solar wind and comets as well as the (highly) volatile elements in the solar system such as helium, nitrogen, oxygen or xenon. INTRODUCTION identify elements, whic servy hgoos ma e a d references or indicators for the key physical processes involved. This manuscript is the resume of a working group Certainly, we cannot provide a complete overview of at the joint SOHO-ACE workshop held in Bern, all questions in the various disciplines relevant to this Switzerland Marcn i , h 2001 goae thif Th .o l s working goal. Therefore, we will follow the expertise of the group was "to determine the importance of various working group members and discuss some of the most elements from the point of view of discerning different crucial questions in cosmochemistry that can and models that address questions such as solar-system shoul e answere b de nea th rn i dfutur e through formation, stellar and Big Bang nucleosynthesis, and improvement n i instrumentations , observational chemical evolutio Galaxy"e th f nwero e W .e askeo dt techniques, theory, and with new dedicated missions. CP598, Solar Galacticd an Composition, . Wimmer-SchweingrubeF edite. R y db r © 2001 American Institut Physicf eo s 0-7354-0042-3/017$ 18.00 357 Downloaded 02 Oct 2007 to 131.215.225.176. Redistribution subject to AIP license or copyright, see http://proceedings.aip.org/proceedings/cpcr.jsp wile W l start with issues concernin formatioe gth n gravitationally capture s fro d e nebulga dmth an 6 ( a and composition of the solar system, and then address references therein, see also for alternative trapping the composition of the (local) interstellar medium mechanisms). The Sun and the gaseous giant planets (L)ISM and of galactic cosmic rays (OCR). While the Jupiter and Saturn, which formed only relatively small solar system represent a sampls f galactio e c matter core hencd san e remain largely undifferentiated, might fro billio5 m4. n years ago LISe th curren,a Ms i d an t represent isotopically undisturbed solar system local r samplGalaxyou f o e . Both samples provide compositio r nearlno , althougyso h Jupiter appearo st benchmark modelr sfo f galactiso c chemical evolution have a more evolved atmosphere, possibly of cometary (GCE Bang ) Bi fro ge muntith l today. OCRs represent origin (7). another sample currenth f o et Galaxy fro ma wid e range of distances that shows some additional The protosolar He abundance as well as its value in characteristics of high-energy interactions. With this the present-day convectiv e preciseleb zonn ca e y paper, we aim to contribute to the interdisciplinary determined by solar modeling and helioseismology discussions between planetary scientists, solar (e.g., 8). However, for the solar Ne, Ar, Kr, and Xe physicists, cosmochemists astrophysicistsd an , . abundances, we must rely on extrasolar sources, analyses of implanted solar wind (SW) in lunar soils, and the systematics of s-process nucleosynthesis, which leads to rather large uncertainties of 15-25% (1, SOLAR SYSTEM ABUNDANCES 2). The abundance of these elements is important to assess the fractionation in the upper solar atmosphere accordin firso gt t ionization potentia firsr lo t ionization time (the so-called FIP/FIT effect, the relative Highly Volatile Elements enrichmen f elemento t s witbeloP e hFI th w n i ~1 V 0e low speed solar wind relativ o t photospherie c Absorption-line spectra of the solar photosphere abundance high-FId an s P element abundances, e.g.9 , and laboratory-based analyses of the most primitive and references therein), compositional differences meteorites, the CI (Ivuna-type) carbonaceous between the solar wind and solar energetic particles chondrites, yield solar-system abundances of the (SEP), temporal variability of the solar wind, or elements (1, 2). For most elements, the agreement of possible fractionation upon trapping in lunar soil (e. g., these data set ~10s si bette%r o r (Figure 1). However, , 11)10 . Most solar wind nobl isotopis ega c ratios a s meteorite t represenno o d s t solar abundancee th f o s derived from measurements of implanted solar wind in ligh d mosr o tan , t O volatil, N , C e, elementBe , Li , sH lunar material have stated precisions of 1% or better the noble gases e reasonTh .e nucleosynthesiar s s (12 and references therein) but better values are processe e Sun'th n s i s e incomplet interioth d an r e needed especially for the less abundant light Kr and condensation during formatio firse th tf nsolio d matter Xe isotopes (see below) e ApollTh . o Solar Wind in the solar system, respectively (2). Among the light Composition experiment (13spacd an ) e missions such elements, only the meteoritic abundance of boron as Ulysses (14d SOHan ) O ) (15als16 o, provided agrees wite valuth h e recently determinee th n i d isotopic ratios for He-Ar in the solar wind. Higher photosphere (3). Therefore, even relatively imprecise precision data from future missions, e.g., Genesis, are measurements (compared to the precision usually required, however, to test whether the values derived obtained from e mentionemeteoritesth l al f do ) from lunar e affectesampleb y y isotopib ma ds c elements in the Sun and the solar wind provide fractionation upon or after trapping. cosmochemically important information e solaTh .r system isotopic composition of these elements is Solar elementae ar O d l an abundance , N , C f o s relatively poorly known. The light elements in believed to be known to within 8-12%, comparable meteorite e particularlar s y subjec o t isotopit c with the estimated accuracy for most elements in CI fractionation from originally solar system composition chondrite . Thei2) , r (1 sisotopi c ratios, howevere ar , duo t theie r volatility e largth , e relative mass t sufficientlno y well known e wilW .l discuss below differences of their isotopes and their chemical how a more precise solar oxygen isotopic composition reactivity (4). It might well be that the isotopic f higio s h importance with respec o studiee t t th f o s compositio noble th f eno gase meteoriten i s t no e ar s homogeneit e solath f r o n ya nebul r fo s wela as a l representative of the solar system at all (5), because improved understandin e GCEth f .o g Even more the meteorite parent bodie precursor so r planetesimals controversial is the solar 15N/14N ratio, as we will might never have incorporated these gases, in contrast discuss below. e mucth ho t heavier planets which could have 358 Downloaded 02 Oct 2007 to 131.215.225.176. Redistribution subject to AIP license or copyright, see http://proceedings.aip.org/proceedings/cpcr.jsp 1 1.4 - iii • Au &&& ' ESS • Pt 1.3 - o z o • Cd • F • TI 1.2 • Os • Ti ~ 1.1 0.9 ._ •U!n • Dy - P• Cu« - 0.8 *•• & i • Sn - 'I <»Mn T 0.7 -2. • Tm - "T • Ge , Pb 0.6 "~ * ( Ga ~" • Ho ( Be _ 0.5 T.B................. ,,,,,,,,,,,,,,^,,,,,,,,,,,,,,,,,< 10 20 30 40 50 60 70 80 90 FIGUR . ECompariso1 solaf no r photospheric (N meteoritid ph)an c "Q" (Nm) abundances heav e (2)mosr th Fo .f yo t elements, the abundances agree within 10%. Error bars are shown if they do not overlap with the range Nph/Nm = 0.9-1.1.
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