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I.Nb.9H 35187A2Ve IS lineNa DIS linex .8CS lines—200 0 200 400 600Heliocentric Velocity (km/s)J>,.Na2.52COCOb 1.5x1HD 144432A9/FOVeCa KCS line5—400 —300 —200 —100 0 100 200 300Heliocentric Velocity (km/s)1.1 Na DHD 144432 A9/FOVelrbx9r ÎS linesIS linesCS lines.8 f--200 0 200 400Heliocentric Velocity (km/s)Figure 1. Circumstellar lines detected in HD 35187 and HD 144432. The Ca II spectrum of HD 144432is the result of the observed spectrum having been divided through by a model for the photosphericspectrum.26
TRANSIENT ACCRETION EVENTS IN HERBIGAE/BE STAR SPECTRA: THE EVIDENCE FORINFALLING PLANETESIMALS IN HD 100546 (B9E)C.A. GRADY Eureka Scientific, Oakland, CA 96402,M.R. PEREZ Applied Research Corporation, Landover MD 20785K.S. BJORKMAN SAL, University of Wisconsin, Madison WI 53706-1390ABSTRACT. Enhanced gaseous absorption resembling the high velocity circumstellargas features in the spectrum of 0 Pic have been detected in IUE high dispersionspectra of the 2 Myr-old Herbig Be star, HD 100546, on 1995 March 9. The presenceof atomic gas features in transitions of C I and 0 I implies that the materialis produced by the pyrolysis of an unseen, solid body in a star-grazing orbit. Thepresence of weak Fe II absorption in the same spectrum with heavily saturated magnesium,aluminum, and silicon features is consistent with an origin in the sublimationof the olivenes detected in IRAS LRS and ISO SWS spectra of this star. The C Iand 0 I detections suggest that, compared to 0 Pic, the planetesimals in this systemcontain substantial amounts of carbonaceous material. The presence of mildlyrefractory species such as Zn II and S II suggests that the planetesimal had not beensubstantially heated above 700 K during its previous lifetime.1. INTRODUCTIONRecent moderate resolution (25 km s -1 ) UV and optical spectral studies of HerbigAe/Be (HAeBe) stars have revealed the presence of systematically redshifted absorptionfeatures in approximately 33% of the stars studied (Grady et al. 1996). Thesefeatures are preferentially observed in the spectra of stars with comparatively highv sin i, double-peaked Ha emission, and histories of large amplitude photometric andpolarimetric variability (Grinin & Rostopchina 1996).Where multiple spectra are available, striking line profile changes are observed inthe accreting gas, reminiscent of those routinely observed in spectra of 0 Pic. Theidentification of these stars, together with their high luminosity from the far UVthrough mm wavelengths provides us with a laboratory for probing the nature ofcircumstellar material in close proximity to the star in objects as young as 2-3 Myr.We present IUE spectra of a transient accretion event observed on 9 March 1995toward the B9 Ve star, HD 100546. HD 100546 is an isolated Herbig Be (HBe) star(Hu et al. 1989) with a mm flux consistent with a dust and gas disk extending some665 AU from the star (Henning et al. 1994). Accreting circumstellar gas is routinelydetectable in all of the available IUE spectra (Grady et al. 1996). When observed inhigh dispersion with IUE on 1995 March 7, enhanced redshifted absorption centeredat approximately 100-150 km s -1 was detected, compared to observations made in27
Page 1 and 2: NASA Conference Publication 3343Fro
Page 3 and 4: PREFACEOn June 24 through 26, 1996,
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: accretion hypothesis, King (1994) i
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^ ô.,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
Page 60 and 61: lo`lo'00axto-,00a10 -20lo-''10' to
Page 63 and 64: EXTERNALLY INDUCED EVAPORATION OF Y
Page 65 and 66: 0-6—7—8—9v -10OD0Dispersal Ra
Page 67: CIRCUMSTELLAR DUST59
Page 70 and 71: Table 1 SiC features and the Temper
Page 72 and 73: have very similar absorption featur
Page 74 and 75: mSE1 .-SE3 -SE4U NA iLtSE5 --SE6 SE
Page 76 and 77: 3. CARBON STARSSloan, Little-Mareni
Page 78 and 79: eferences therein). The arc dischar
Page 80 and 81: the time scale of their evolution:
Page 82 and 83: easily amended for any chemical spe
Page 84 and 85:
25002000aâ^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
Page 92 and 93:
Examining a number of grain types,
Page 95 and 96:
REVISED DEPLETIONS AND NEW CONSTRAI
Page 97 and 98:
- 1 -Table 1.__Revised stellar and
Page 99:
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
Page 106 and 107:
2.1. ExtinctionInfrared photometry
Page 109 and 110:
THE EXTINCTION PROPERTIES OFHEAVILY
Page 111 and 112:
3. ANALYSISUsing a Quantimet Q520 i
Page 113 and 114:
HAC: BAND GAP, PHOTOLUMINESCENCE, A
Page 115 and 116:
3.2. The 3.4 micron Absorption Band
Page 117 and 118:
THE ROLE OF HYDROGEN IN SMALL AMORP
Page 119 and 120:
R 100an'c30w 0 Wa.AE-50A 1C.q-t0.5x
Page 121 and 122:
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.
Page 127 and 128:
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:
Page 133 and 134:
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
Page 139 and 140:
PROCESSING OF ICY MANTLES IN PROTOS
Page 141 and 142:
tions of mixtures each provide exce
Page 143 and 144:
THE ICE AND SILICATE SPECTRAL FEATU
Page 145 and 146:
2.5Model C (a= 1µm)—f=0.2-'1 - -
Page 147 and 148:
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
Page 159 and 160:
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
Page 165 and 166:
3. AN EXAMPLE CALCULATIONWe have in
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EFFECT OF DUST COAGULATION DYNAMICS
Page 169 and 170:
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 . . .
Page 183 and 184:
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
Page 191 and 192:
THE ROLE OF VORTICES IN THE FORMATI
Page 193 and 194:
(a)(b)(c)606060Y40 ,^ Y40 OOY402020
Page 195 and 196:
THE GLOBAL PERSPECTIVE ON THE EVOLU
Page 197 and 198:
103102 ..........................10
Page 199 and 200:
TOWARD AN ASTROPHYSICAL THEORY OFCH
Page 201 and 202:
and the subsolar temperatureTsub..I
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PLANETESIMAL FORMATION IN THE OUTER
Page 205 and 206:
3. SUBLIMATION, CONDENSATION, AND G
Page 207 and 208:
PLANETESIMALS AND COMETS199
Page 209 and 210:
THE MASS OF LARGE IMPACTORSM. G. PA
Page 211 and 212:
99 3JupiterNeptuneA0 20 — 0.00 0.
Page 213 and 214:
TIDAL BREAKUP OF ASTEROIDS BY THE E
Page 215 and 216:
Figure 2. Time sequence showing the
Page 217 and 218:
ON THE DYNAMICS OF THE ZODIACAL DUS
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de Log U®ro 1 — E2dt aysw Ecos z
Page 221 and 222:
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
Page 243 and 244:
plasma 216,218polarization 38, 39,
Page 245 and 246:
OBJECT INDEXAB Aur 20R Cas 15O Ceti
Page 247 and 248:
ADDRESSES OF PARTICIPANTS239
Page 249 and 250:
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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