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NASA Conference Publication 3343From Stardust toPlanetesimals:Contributed PapersEdited byM. E. Kress, A. G. G. M. Tielens, and Y. J. PendletonAmes Research Center, Moffett Field, CaliforniaProceedings of a symposiumheld in Santa Clara, CaliforniaJune 24 26, 1996^ a ^National Aeronautics andSpace AdministrationAmes Research CenterMoffett Field, California 94035-10001996
PREFACEOn June 24 through 26, 1996, a scientific conference entitled From Stardust to Planetesimalswas held at the Westin Hotel, Santa Clara, California, as part of the 108th annual meeting ofthe Astronomical Society of the Pacific. This conference was made possible by generous grantsfrom the Astrophysics and Exobiology programs of the National Aeronautics and SpaceAdministration, and support services rendered by the dedicated staffs of NASA Ames ResearchCenter and the Astronomical Society of the Pacific.Over the last decade, our understanding of the formation and early evolution of the solarSystem has advanced considerably due to progress that has been made simultaneously on manyfronts. Stardust has been isolated in meteorites and interplanetary dust particles (IDPs),providing us with sample materials which predate the solar system and which offer clues to theprocessing that has occurred. At the same time, infrared studies have led to a bettercharacterization of the composition of interstellar dust, which is now readily accepted as animportant component of the interstellar medium. Infrared observations have also provided amuch better view of the star-formation process and the role of dust therein. Recently, thepresence of Kuiper Belt planetesimals has been confirmed and spectroscopy of these ratherpristine objects may soon become available. Analysis of spacecraft data from the Comet Halleyflybys has yielded a wealth of information on the composition of this comet. Theseobservational advances have changed our understanding of planetesimal processing. Thelaunch of the Infrared Space Observatory, the opening of 10-meter class telescopes, and, in thelonger term, the Rosetta mission, promise to continue to broaden and deepen ourunderstanding of the evolution from stardust to planetesimals.For these reasons we considered it timely to organize a meeting focused on the processes thatconnect stardust and planetesimals. The goal of this meeting was, therefore, to bring togetherastronomers interested in star- and planet-formation, planetary scientists studying early solarsystem relics, laboratory scientists studying the processing of analogs, and scientists analyzingmeteorites and interplanetary dust particles, grain by grain. As a result of this endeavor, over200 participants, including 153 scientists from 14 different countries, gathered to discuss theorigin and evolution of stardust. We hope that this encounter in Santa Clara will foster anongoing interchange of information and ideas within this diverse group of scientists.A major aim of this meeting was to produce conference proceedings which reflect the currentsituation regarding the evolution from stardust to planetesimals. This volume contains thecontributed papers presented at the meeting. The invited review papers will be publishedseparately in the Astronomical Society of the Pacific conference series. We extend specialthanks to Greg Sloan, who produced the poster paper abstract book which was a tremendousasset during the meeting.The conference was dedicated to three outstanding scientists whose untimely deaths left manyhearts saddened. James Pollack, Akira Sakata, and Jason Cardelli each contributedsignificantly to the body of knowledge presented at this conference. Their scientific insight willbe missed as we continue to explore the pathway From Stardust to Planetesimals. Tributes totheir scientific achievements can be found in the proceedings book of the invited review papers.We thank the Local and Scientific Organizing Committees, NASA Ames Research Center, andthe Astronomical Society of the Pacific for making this conference a rewarding endeavor.M. E. Kress A. G. G. M. Tielens Y. J. PendletonMoffett Field, CANovember, 1996
Page 1: NASA Conference Publication 3343Fro
Page 5 and 6: TABLE OF CONTENTSPreface...........
Page 7 and 8: The role of hydrogen in small amorp
Page 9: P PIC AND SIMILAR DISK-LIKE OBJECTS
Page 12 and 13: y linear deconvolution of the SSA i
Page 14 and 15: `planetesimals'. Those ones are spa
Page 16 and 17: o Variations of the size of the blo
Page 18 and 19: Table 1 Best-fitting model paramete
Page 20 and 21: 10-10SAO 179815 (HD 98800)10-1110-1
Page 22 and 23: 2. 0 Pic-like SYSTEMSOne of the gre
Page 24 and 25: Backman, D. E., and Paresce, F. 199
Page 27 and 28: PARTIALLY CRYSTALLINE SILICATE DUST
Page 29 and 30: 12D 100546 vs Forsterite (dashed) a
Page 31 and 32: HIGH RESOLUTION SPECTROSCOPY OF VEG
Page 33 and 34: accretion hypothesis, King (1994) i
Page 35 and 36: TRANSIENT ACCRETION EVENTS IN HERBI
Page 37 and 38: e ionized by the stellar radiation
Page 39: STAR FORMATION31
Page 42 and 43: 1980 1985 1990 19959.09.5®rIL10.01
Page 44 and 45: 4. DISCUSSION AND CONCLUSIONSWe hav
Page 46 and 47: 2. SHELL MODELThe dusty envelope is
Page 48 and 49: — "Fluffiness" of dust particles.
Page 50 and 51: 2. OBSERVATIONSThe observations wer
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1050.015^ ^o.,a •,o a0s0au0—5
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IMAGING POLARIZED DUST EMISSION IN
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Figure 3. The total intensity (left
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0fvac = 0.3(dot), 0.5(dash), 0.7(li
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lo`lo'00axto-,00a10 -20lo-''10' to
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EXTERNALLY INDUCED EVAPORATION OF Y
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0-6—7—8—9v -10OD0Dispersal Ra
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CIRCUMSTELLAR DUST59
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Table 1 SiC features and the Temper
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have very similar absorption featur
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mSE1 .-SE3 -SE4U NA iLtSE5 --SE6 SE
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3. CARBON STARSSloan, Little-Mareni
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eferences therein). The arc dischar
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the time scale of their evolution:
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easily amended for any chemical spe
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25002000a^a^H150010001 2 3 4r/Rstar
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2. METHODThe stellar wind model is
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0 0.04(a)3007EU200(b)0.03Ec 0.02^s0
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0 CETIX = 8-9 µm ,(off dust featur
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Examining a number of grain types,
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REVISED DEPLETIONS AND NEW CONSTRAI
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- 1 -Table 1.__Revised stellar and
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ReferencesAannestad, P. 1995, ApJ,
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3.02.52.0CL1.51.00.50.03 4 5 61 /X
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ReferencesAnderson, C.M. et al. 199
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2.1. ExtinctionInfrared photometry
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THE EXTINCTION PROPERTIES OFHEAVILY
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3. ANALYSISUsing a Quantimet Q520 i
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HAC: BAND GAP, PHOTOLUMINESCENCE, A
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3.2. The 3.4 micron Absorption Band
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THE ROLE OF HYDROGEN IN SMALL AMORP
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R 100an'c30w 0 Wa.AE-50A 1C.q-t0.5x
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OBSERVATIONS OF TWO NON-STANDARD GR
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where VSGs break off larger grains
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IRAS COLORS OF THE PLEIADESSEAN J.
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4. IDENTIFICATION OF DENSE (MOLECUL
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PAH EMISSION IN THE ORION BARJESSE
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0.80.60.40.20.8N 0.60.4DN 0.2^ E b:
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LABORATORY EXPERIMENTS ON THE REACT
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500Cto 8+ + 0 ®> CgH8+ + CO400AvrA
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433v02110 30 60 90 120 150 180 210F
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PROCESSING OF ICY MANTLES IN PROTOS
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tions of mixtures each provide exce
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THE ICE AND SILICATE SPECTRAL FEATU
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2.5Model C (a= 1µm)—f=0.2-'1 - -
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EVIDENCE FOR THE EVOLUTION OF GRAIN
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(a) Ih2FIRS,_I(h}p 56^LOo . o FIR4'
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THE ABUNDANCES OF CHARGED PARTICLES
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2.3. Grain Charge TransferIn order
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THE PROTOSOLAR NEBULA147
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CATALYSIS BY DUST GRAINS IN THE SOL
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Figure 1 shows the steps involved i
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(e.g., surface-catalyzed) ones. Thi
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RESTRUCTURING OF DUST AGGREGATES IN
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3. AN EXAMPLE CALCULATIONWe have in
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EFFECT OF DUST COAGULATION DYNAMICS
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NUMERICAL SIMULATIONS FOR SUM KERNE
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SELF-CONSISTENT SIMULATION OF THE B
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and a diffusivity Di = Tfi kT/mi. D
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DUST COAGULATION IN PROTOPLANETARYA
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Coogulction tit?- )e• zn /5139,5
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SIZE SEGREGATION AND NUMBER DENSITY
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10`1100.01 cm . . . . .0.1 cm . . .
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FROM CHONDRULES TO PLANETESIMALS:SO
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Figure 2. Regions of high particle
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VORTICES AND PLANETESIMALSP. BARGE
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c0UdWU)0 10 -1ULUiCROSSING * ` yAjr
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THE ROLE OF VORTICES IN THE FORMATI
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(a)(b)(c)606060Y40 ,^ Y40 OOY402020
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THE GLOBAL PERSPECTIVE ON THE EVOLU
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103102 ..........................10
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TOWARD AN ASTROPHYSICAL THEORY OFCH
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and the subsolar temperatureTsub..I
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PLANETESIMAL FORMATION IN THE OUTER
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3. SUBLIMATION, CONDENSATION, AND G
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PLANETESIMALS AND COMETS199
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THE MASS OF LARGE IMPACTORSM. G. PA
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99 3JupiterNeptuneA0 20 — 0.00 0.
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TIDAL BREAKUP OF ASTEROIDS BY THE E
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Figure 2. Time sequence showing the
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ON THE DYNAMICS OF THE ZODIACAL DUS
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de Log U®ro 1 — E2dt aysw Ecos z
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DUST AND SPUTTERED PARTICLE STREAMS
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A"P -0.1s^nntU 8 -- -3.2- - 3.6-- 3
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PRELIMINARY RESULTS OF OBSERVATIONS
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4. ULYSSES COMET WATCH NETWORKIn 19
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POROSITY AND PERMEABILITY OF CHONDR
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from the dessi cation of such a "we
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5. POROSITY MEASUREMENTS OF BULK CH
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RAMAN SPECTRUM OF QUENCHEDCARBONACE
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Raman shift (Acm -1)1000 1300 1600
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AUTHOR INDEXAdamson, A.J. 101,131 G
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SUBJECT INDEXabundances, cosmic 89a
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plasma 216,218polarization 38, 39,
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OBJECT INDEXAB Aur 20R Cas 15O Ceti
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ADDRESSES OF PARTICIPANTS239
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Nancy AgeorgesEmma BakesESONASA Ame
Page 251 and 252:
Max BernsteinJurgen BlumNASA Ames R
Page 253 and 254:
Connie ChangSimon ClemettHarvard Un
Page 255 and 256:
Jamie ElsilaMarina FomenkovaKalamaz
Page 257 and 258:
Mayo GreenbergUniv. of LeidenHuygen
Page 259 and 260:
Dan JudnickJohn F. Kerridge5702 Cal
Page 261 and 262:
John KulanderOliver LayP.O. Box 704
Page 263 and 264:
Vito MennellaDaffel MoonObservatori
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Pendleton YvonneSun Hong RhieNASA A
Page 267 and 268:
Anneila SargentRussell ShipmanCalif
Page 269 and 270:
Prof. Stanislav SvirschevskyHead of
Page 271 and 272:
Christoffel WaelkensFrancis P. Wilk
Page 273:
REPORT DOCUMENTION PAGEForm Approve
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