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

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SCIENTIFIC ORGANIZING COMMITTEEP. Bodenheimer (University of California, Santa Cruz)Alan Boss (Carnegie Institute, Washington)Don Brownlee (University of Washington, Seattle)John Kezridge (University of California, San Diego)Michael Mumma (Goddard Space Flight Center)Jane Luu (Harvard University, Boston)Tobias Owen (University of Hawaii, Honolulu)Yvonne Pendleton (NASA Ames Research Center, Chair)T.P. Snow (Univeriity of Colorado, Boulder)A.G.G.M. Tielens (NASA Ames Research Center)LOCAL ORGANIZING COMMITTEEMax BernsteinSteven CharnleyMichael KaufmanMonika KressBill Latter.Brent RogervilleScott SandfordMaureen SavageJeff ScargleGreg SloanDave ScimecaBob WalkerJuliet WiesemaSue Zaboriv
TABLE OF CONTENTSPreface.................................................................................. mScientific and Local Organizing Committees ....................................... ivpage5 PIC AND SIMILAR DISK-LIKE OBJECTSPlanetesimals around V536 AQL ................................................... 3N. Ageorges & W.J. DuschlModelling the dust around Vega-like stars ......................................... 9R.J. Sylvester, C.J. Skinner & M.J. BarlowExamples of comet-like spectra among P Pic-like stars .......................... 13H.M. Butner, H.J. Walker, D.H. Wooden & F.C. WittebornPartially crystalline silicate dust in protostellar disks ............................. 19M.L. Sitko, D.K. Lynch, R.W. Russell, M.S. Hanner & C.A.GradyHigh-resolution spectroscopy of Vega-like stars: abundances andcircumstellar gas ....................................................................... 23S.K. Dunkin, M.J. Barlow & S.G. RyanTransient accretion events in Herbig Ae/Be star spectra: the evidence forinfalling planetesimals in HD 100546 (B9e) ....................................... 27C.A. Grady, M.R. Perez & K.S. BjorkmanSTAR FORMATIONThe remarkable Herbig Ae star V351 Ori .......................................... 33M.E. van den Ancker, P.S. The & D. de WinterDust around Herbig Ae stars: additional constraints from their photometricand polarimetric variability ........................................................... 37N.A. Krivova, V.B. Il'in & O. FischerAn infrared study of the juggler nebula .............................................. 41J. C. Holbrook, P. Temi, D. Rank & J. BregmanImaging polarized dust emission in star formation regions with the OVRO mmarray..................................................................................... 45R. Akeson & J. CarlstromV
Page 1 and 2: NASA Conference Publication 3343Fro
Page 3: PREFACEOn June 24 through 26, 1996,
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
Page 52 and 53: 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
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Max BernsteinJurgen BlumNASA Ames R
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Connie ChangSimon ClemettHarvard Un
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Jamie ElsilaMarina FomenkovaKalamaz
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Mayo GreenbergUniv. of LeidenHuygen
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Dan JudnickJohn F. Kerridge5702 Cal
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John KulanderOliver LayP.O. Box 704
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Vito MennellaDaffel MoonObservatori
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Pendleton YvonneSun Hong RhieNASA A
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Anneila SargentRussell ShipmanCalif
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Prof. Stanislav SvirschevskyHead of
Page 271 and 272:
Christoffel WaelkensFrancis P. Wilk
Page 273:
REPORT DOCUMENTION PAGEForm Approve
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