From Stardust to Planetesimals: Contributed Papers - NASA Lunar ...

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The spectral energy distribution of HH 100 IRS ................................. 49R. SiebenmorgenExternally induced evaporation of young stellar disks in Orion ................. 55D. Johnstone, D. Hollenbach & F. ShuCIRCUMSTELLAR DUSTThe 11 µm silicon carbide feature in carbon star shells ........................... 61A.K. Speck, M.J. Barlow & C.J. SkinnerOn the classification of infrared spectra from circumstellar dust shells ......... 65G.C. Sloan, I.R. Little-Marenin & S.D. PriceFormation of cosmic carbon dust analogs in partially hydrogenatedatmospheres ............................................................................ 69A. Blanco, S. Fonti, A.M. Muci & V OrofinoTime dependent models of grain formation around carbon stars ................ 73M.P. Egan & R.F. ShipmanThe size distribution of stardust injected into the ISM ........................... 77D. Kruger & E. SedlmayerConstraints on circumstellar dust grain sizes from high spatial resolutionobservations in the thermal infrared ................................................. 81E.E. Bloemhof, R.M. Danen & C.R. GwinnINTERSTELLAR DUSTRevised depletions and new constraints on interstellar dust composition ...... 87T.P. Snow & A.N. Witt0The interstellar polarization feature associated with the 2175 A extinctionbump .................................................................................... 93G.C. Clayton, M.J. Wolff, S.H. Kim, P.G. Martin & C.M.AndersonInterstellar extinction, polarization, and grain alignment in high-latitude clouds 97K.A. Larson & D.C.B. WhittetThe extinction properties of heavily-reddened lines of sight in the Galaxy .... 101M.G. Rawlings, A.J. Adamson & D.C.B. WhittetHAC: band gap, photoluminescence, and optical/near-infrared absorption .... 105A.N. Witt, D. Ryutov & D.G. Furtonvi
The role of hydrogen in small amorphous carbon grains: the IR spectrum .... 109V. Mennella, L. Colangeli, C. Cecchi Pestellini, E. Palomba,P Palumbo, A. Rotundi & E. BussolettiObservations of two nonstandard grain components ............................. 113R.F. Shipman, S.J. Carey & F.O. ClarkIRAS colors of the Pleiades .......................................................... 117S.J. Carey, R.F. Shipman & F.O. ClarkPAH emission in the Orion Bar ..................................................... 121J. Bregman & G.C. SloanLaboratory experiments on the reactions of PAH cations with molecules andatoms of interstellar interest .......................................................... 125V. LePage, H.S. Lee, V.M. Bierbaum & T.P. SnowProcessing of icy mantles in protostellar envelopes ............................... 131J.E. Chiar, D.C.B. Whittet, P.A. Gerakines, A. CA. Boogert & A.J.AdamsonThe ice and silicate spectral features for dust aggregates ......................... 135A. E. IlinEvidence for the evolution of grain properties in the NGC 2024 star formingridge................................................................................... 139C.J. Chandler, J.E. Carlstrom, J.S. Richer, A. Visser & R. PadmanThe abundances of charged particles in protostellar cores ........................ 143S.J. DeschTHE PROTOSOLAR NEBULACatalysis by dust grains in the solar nebula ........................................ 149M.E. Kress & A.G.G.M. TielensRestructuring of dust aggregates in the solar nebula .............................. 155C. Dominik & A.G. G.M. TielensEffect of dust coagulation dynamics on the geometry of aggregates ............ 159R. NakamuraSelf-consistent simulation of the Brownian stage of dust growth ............... 163S. Kempf, S. Pfalzner & Th. HenningDust coagulation in protoplanetary accretion disks ................................ 167W. Schmitt, Th. Henning & R. MuchaSize segregation and number density enhancement of particles in accretiondiskeddies ............................................................................. 171H.H. Klahr & Th. HenningVii
Page 1 and 2: NASA Conference Publication 3343Fro
Page 3 and 4: PREFACEOn June 24 through 26, 1996,
Page 5: TABLE OF CONTENTSPreface...........
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
Page 52 and 53: 1050.015^ ^o.,a •,o a0s0au0—5
Page 54 and 55: IMAGING POLARIZED DUST EMISSION IN
Page 56 and 57:
Figure 3. The total intensity (left
Page 58 and 59:
0fvac = 0.3(dot), 0.5(dash), 0.7(li
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lo`lo'00axto-,00a10 -20lo-''10' to
Page 63 and 64:
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
Page 111 and 112:
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
Page 239 and 240:
AUTHOR INDEXAdamson, A.J. 101,131 G
Page 241 and 242:
SUBJECT INDEXabundances, cosmic 89a
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plasma 216,218polarization 38, 39,
Page 245 and 246:
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
Page 265 and 266:
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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