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Astrophysical Dust Grains in Stars,
the Interstellar Medium, and the Solar System
ROBERT D. GEHRZ
University of Minnesota
ABSTRACT
Studies of astrophysical dust grains in circumstellar shells, the inter-
stellar medium (ISM), and the solar system, may provide information about
stellar evolution and about physical conditions in the primitive solar nebula.
Infrared observations give information about the mineral composition and
size distribution of the grains. Grain materials identified in sources exter-
nal to the solar system include silicates, silicon carbide, amorphous carbon,
and possibly hydrocarbon compounds. The nucleation and growth of as-
trophysical carbon grains has been documented by infrared observations of
classical novae. In the solar system, dust is Mown to be a major constituent
of comet nuclei, and infrared spectroscopy of comets during perihelion
passage has shown that the ablated material contains silicates, amorphous
carbon, and hydrocarbons. Cometary grains resemble extra-solar-system
grains in some ways, but there is evidence for additional processing of the
grain materials in comets. Comets are discussed as a possible source for
zodiacal dust.
Solar system grain materials have been sampled by the collection
of micrometeorites and by isolating microscopic inclusions in meteorites.
Meteorite inclusions exhibit several chemical abundance anomalies that are
similar to those predicted to be produced in the explosive nucleosynthesis
that accompanies novae and supernovae. The possible connections between
extra-solar-system astrophysical dust grains and the grains in the solar
system are explored. A recent suggestion that grains are rapidly destroyed
in the interstellar medium by supernova shocks is discussed. Experiments to
establish the relationships between extra-solar-system astrophysical grains
126
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AMERICAN AND SOVIET RESEARCH
127
and solar system grains, and between cometary dust and the zodiacal dust
are suggested. Among the most promising are sample return missions and
improved high-resolution infrared spectroscopic information.
THE CYCLING OF DUST IN STELLAR EVOLUTION AND
THE FORMATION OF PLANETARY SYSTEMS
Small refractory dust grains are present in circumstellar shells around
many different classes of stars, in the interstellar medium (ISM), and in
comets and the zodiacal cloud in the solar system. The mineral composition
and size distribution of the grains in all three environments have similarities,
but there are also distinct differences. Condensable elements produced in
stars during nucleosynthesis presumably condense into grains during the
final mass-loss stages of stellar evolution in aging stars like M-type giants
and supergiants (Gehrz 1989), or during nova and supernova eruptions
(Clayton 1982; Gehrz 1988~. These grains can be expelled into the ISM
where they may be processed further by supernova shocks and in molecular
clouds. The grains can eventually be incorporated into young stars and
planetary systems during star formation in the clouds (Gehrz et al. 1984~.
Dusty and rocly solids that may derive from remnants of the forma-
tive phase are present in our own solar system and around some other
main-sequence stars. Grains could therefore be a significant reservoir for
condensable elements, effecting the transportation of these elements from
their sites of production in stars into new stellar and planetary systems.
Studies of astrophysical grains can provide significant information
about stellar evolution, physical conditions in circumstellar environments,
and processes that occur during star formation. In particular, grains in
the solar system may contain evidence about conditions in the early solar
nebula. A major issue is whether grains made by stars actually survive
intact in significant quantities as constituents of mature planetary systems,
or whether most of the dust we see in the ISM and the solar system
represents a re-accretion of condensables following the destruction of cir-
cumstellar or interstellar grains. There is theoretical evidence that grains
can be destroyed in both the ISM (Scab 1987) and during the formation
of planetary systems (Boss 19883. A paucity of gas-phase condensables in
the ISM (Jenkins 1987), a low input rate to the ISM of dust from evolved
stars (Gehrz 1989), and evidence for a hydrocarbon component in ISM
grains (Allamandola et al. 1987) all suggest that grains can accrete material
in molecular clouds. If the grains can survive the interstellar and star for-
mation environments intact, then studies of the elemental abundances and
mineralogy of solar system grains may provide fundamental information
about stellar nucleosynthesis and evolution. If the grains are substantially
processed, or evaporate and recondense after leaving the circumstellar
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PL~ANETARY SCIENCES
environment, then their chemical history may be much more difficult to
evaluate, and their current composition may reflect relatively recent events.
This review discusses the observed characteristics of astrophysical grains,
compares the properties of grains in the solar and extra-solar environments,
and suggests investigations to address the question of whether stardust is
an important constituent of solar system solids.
ASTROPHYSICAL DUST GRAINS IN
CIRCUMSTELLAR ENVIRONMENTS
Infrared observations made more than two decades ago provided the
first convincing evidence that dust grains are present in the winds of late-
type giant and supergiant stars. Most of this circumstellar dust is refractory
material. Woolf and Ney (1969) were the first to recognize that silicate
grains, similar in mineral composition to materials in the Earth's crust and
mantle, were a major constituent of the dust in oxygen-rich stars.
Circumstellar stardust around carbon-rich stars is composed primarily
of amorphous carbon and silicon carbide (Gehrz 1989~. The identification
of the silicate and SiC material comes from 10 and 20pm emission features
caused by the Si-O/Si-C stretching and O-Si-O bending molecular vibra-
tional modes (see Figures 1 and 2~. Silicates, having the triatomic molecule
SiO2 in their structure, show both the features. The diatomic molecule SiC
cannot bend, and therefore exhibits only the Em stretching feature. The
10 and 20pm emission features in stellar objects are broad and generally
devoid of the structure generally diagnostic of crystaline silicate minerals
like Ol~vine and Enstatite (Rose 1979, Campins and ~kunaga 1987~. This
suggests that the silicateous minerals in stardust are amorphous, and that
the grains probably have a considerable spread in size distribution.
Some astrophysical sources exhibit near infrared emission or absorp-
tion features in the 3.1 to 3.4pm spectral region (see Figure 3) that have
been attributed to stretching vibrations in C-H molecular bonds associ-
ated with various hydrocarbon compounds (Allamandola 1984; Sakata e'
al. 1984; Allamandola et al. 1987; Allen and Wickramasinghe 1987~. The
hydrocarbon grain materials proposed to account for these features in-
clude polycyclic aromatic hydrocarbons (PAH's), hydrogenated amorphous
carbon (HAC's), and quenched carbonaceous composites (QCC's). There
is evidence for the presence of hydrocarbon grains in the near infrared
spectra of a handful of stellar objects (see de Muizon e' al. 1986; Gehrz
1989~.
Observations have confirmed the existence of dust in circumstellar
environments other than those associated with late-type stars. Dust is
known to have condensed around novae (Gehrz 1988) and probably can
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AMERICAN AND SOVIET RESEARCH
107
lo6
C~J 10
- 3 104
> 103
J
LLI
~ 102
0
1
129
, I 8.7 10.011.4 12.6
U B V R I ) ~ H 2.3 3.6 4.9 l J 1 1923
1 1 1 1 1< 1 1 1 1 1 ~ (< 1 1
r T T i l
,uCeP x
\x
_ \
RU Vi r / ~x/x x
·~~\ \~x
'0 o it\ ~
LW Serf \O\
VY CMa x_ ~ /\ x\>
. ~ ~ 690 K
i580 K ~ ~'
COMET ~ / / oo~
KOHOUTEK: / o /'~°
COMA ~ /
ANTITAIL /
_ /
/
SgrA 0
1 1 1 1 1 1
3 0 5.0 10.0 30.0
0.3 0.5 1.0
WAVELENGTH IN MICRONS
FIGURE 1 The infrared energy distributions of various objects that show emission or
absorption due to small astrophysical dust grains. VY CMa and ~ Cep are M supergiants
(oxygen-rich stars) that have strong 10 and 20pm silicate emission features (Geh~z 1972~.
These same emission features appear in the comae of comets (Comet Kohoutek) where the
grains are small (Ney 1974~. The superheat in the coma dust continuum shows that the
grains, probably amorphous carbon, producing this continuum are also small. The feature is
weak in the Kouhoutek antitail because the grains are large (Ney 1974~. General interstellar
silicate absorption at 10 and 20pm is evident in the nonthermal spectrum of the Galactic
Center source Sgr A (data from Hackwell et al. 1970~. Carbon stars (RU Vir) often show
a 11.3pm emission feature caused by SiC and a near infrared thermal continuum due to
amorphous carbon (Gehrz et al. 1984~. Novae (LW Ser) form carbon dust in their ejecta
(Gehrz et al. 1980~. The carbon produces a grey, featureless continuum from 2 to 23,um.
The superficial similarities in the spectra of these objects is striking.
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PLANETARY SCIENCES
form in the ejects from supernovae, though there is as yet no unambigu-
ous observational evidence for supernova dust formation (Gehrz and Ney
1987.
A small amount of dust is also present in the winds of planetary nebulae
(Gehrz 1989) and Wolf-Rayet (WR) stars (Hackwell et al. 197~, Gehrz
1989~. The Infrared Astronomical Satellite (IRAS) provided far infrared
data that show evidence for the existence of faint, extended circumstellar
dust shells around some main sequence (MS) stars (Aumann et al. 1984;
Paresce and Burrows 1987~. These shells, typified by those discovered
around Vega (a Lyr) and ~ Pic, are disk-like structures believed to be fossil
remnants of the star formation process. Although the material detected
by IRAS around MS stars is most likely in the form of small and large
grains, the presence of planets within the disks cannot be ruled out. The
existing data are not spatially or spectrally detailed enough to lead to
definitive conclusions about the mineral composition and size distribution
of these fossil remnants of star/planetary system formation. There are large
amounts of dust present in the circumstellar regions of many young stellar
objects (YSO's), often confined in disk-like structures that are associated
with strong bipolar outflows (Lade 1985~. In the case of YSO's, it is unclear
whether the dust is condensing in the wind or remains from the material
involved in the collapse phase.
Most main-sequence stars and older YSO's do not have strong infrared
excesses from dust shells, nor do they show evidence for visible extinction
that would be associated with such shells. It is tempting to conclude that
the shells in these objects have been cleared away in the early stages of
stellar evolution by stellar winds, by Poynting-Robertson drag, or by the
rapid formation of planets (see the contribution by Strom et al. in these
proceedings). Rapid clearing of the circumstellar material poses a problem
for the rather long time scale apparently required for the formation of
giant planets (see the contribution by Stevenson in these proceedings). An
alternative possibility is that dust grains grow to submillimeter or centimeter
sizes (radii from 100 microns to 10 centimeters) during the contraction
of the core to the Zero Age Main Sequence (ZAMS). Such grains will
produce negligible extinction and thermal emission compared to an equal
mass of the 0.1-10 micron grains that are believed to make up most of
the material in circumstellar shells that reradiate a substantial fraction of
the energy released by the central star. It can be shown that the opacity
of a circumstellar shell of mass M = N4~rpa3/3 (where N is the number
of grains in the shell, p is the grain density, and a is the grain radius) is
~ SN 1987a is believed to have condensed dust grains about 400 days after its eruption. The dust
formation is discussed in an analysis of recent infrared data by R.D. GehIz and E.P. Ney (1990.
Proc. Natl. Acad. Sci. 87:43544357).
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E
At
J
lo
o
131
1
RU Vir
. I. a. B N _ _
.
10 7
10 _
BI Cyg
1.8
1.6
1.4
1.2
1.0 _
0.8' . . 1 ,
COMET .
KOHOU TEK 1
/ l
/TRA PEZ IU M
.
i
..tA
.~. 1
~ . ,.
it,
a'
· :.
`* ~ .;
....
· ....e ·e
·. ·
.
-
·.#
\. ~
\
.
\.
, 1 1 1 1.
.
-1
6 8 10 12 14
WAVELENGTH IN M ICRONS
10
10
FIGURE 2 High-resolution infrared spectra of the 7-14 micron emission and absorption
features of different astrophysical sources illustrating some basic differences between extra-
solar-system sources and comets. The classical astrophysical 10,um silicate emission feature,
typified by the Trapezium emissivity profile (Gillett et al. 1975) and the M-supergiant BI
(;yg (Geh~z et al. 1984), peaks at 9.7,um. It is broad and without structure, suggesting
that the grains are amorphous with a wide range of grain sizes. The feature appears
in absorption in compact sources deeply embedded in molecular cloud cores such as the
BN (Becklin-Neugebauer) object in Orion (Gillett et al. 1975~. The carbon star RU Vir
exhibits a classical 11.3pm SiC emission feature (Geh~z et al. 1984~. Comet Kohoutek
data are from Merrill (1974) as presented by Rose (1979~. The 10p emission feature of
Kohoutec is similar to the classical astrophysical silicate feature. P/Halley~s emission feature
(Bregman et al. 1987) shows detailed structure suggesting that the grain mixture contains
significant quantities of crystaline anhydrous silicate minerals. The solid line to the P/Halley
data is a fit based on spectra of IDP's with Olivene and Pyroxene being the dominant
components (Sandford and Walker 1985~. The feature at 6.8pm may be due to carbonates
or hydrocarbons.
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PLANETARY SCIENCES
inversely proportional to the grain radius if M is held constant. A shell
of 0.1 micron grains would be reduced in opacity by a factor of 106 if the
grains were accreted into 10 cm planetesimals while the total circumstellar
dust mass remains constant. A 10 LO star would require the age of the
solar system to clear 10 cm planetesimals from a circumstellar radius of
10 AU by Poynting-Robertson drag, and the sweeping effects of radiation
pressure on 10 cm grains would be negligible. It would appear possible
to postulate scenarios for the accretion of large circumstellar bodies that
are consistent with both the relatively rapid disappearance of observable
circumstellar infrared emission and the long time scales required for giant
planet formation.
CIRCUMSTELLAR GRAIN FORMATION ANI) MASS LOSS
The observations described above suggest that many classes of evolved
stellar objects are undergoing steady-state mass loss that injects stardust
of various compositions into the interstellar medium. Gehrz (1989) has
estimated the rates at which various grain materials are ejected into the
ISM by different classes of stars. Stardust formation in most stars is a
steady-state process, and the detailed physics of the grain formation is
exceedingly difficult to resolve with current observational capabilities. In-
frared studies of objects exhibiting outbursts that lead to transient episodes
of dust formation, on the other hand, have revealed much about the for-
mation of stardust and its ejection into the ISM. The long-term infrared
temporal development of a single outburst is governed by the evolution of
the grains in the outflow. Observations have shown that it is possible in
principle to determine when and under what conditions the grains nucleate,
to follow the condensation process as grains grow to large sizes, to record
the conditions when grain growth ceases, and to observe behavior of the
grains as the outflow carries them into the ISM.
The primary examples of transient circumstellar dust formation have
been recorded in classical nova systems (Gehrz 19~) and WR Stars (Hack-
wel1 et al. 1979~. In both cases, grains nucleate and grow on a time scale of
100 to 200 days, and the grains are carried into the ISM in the high-velocity
outflow. The dust formation episodes apparently occur as frequently as ev-
ery five years in WR stars and about once per 100-10,000 years in classical
novae. About 10-6 to 10-5 solar masses of dust form in each episode, and
the grains can grow as large as 0.1 to 0.3 microns. There is evidence that the
grains formed in nova ejecta are evaporated or sputtered to much smaller
sizes before they eventually reach the ISM. Novae have been obseIved
to produce oxygen silicates, silicon carbide (SiC), amorphous carbon, and
perhaps hydrocarbons (Gehrz 1988; Hyland and MacGregor 1989~; WR
stars apparently condense iron or amorphous carbon (Hackwell e! al. 1979~.
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30
aD 20
° 10
x
Cot
3 ~
o - 3
x
2
In
a
LLI
C,
X
133
' 1 ' 1 ' 1
o
4
1
10
8
-
o
x
6
/ ~
ORION BAR
IRAS 21282+5050
I ~
t
t,
·e
+ t COMET
~ t p/ HALLEY -
. ~
tt, t. tett
. - - .
.
~ .- ~ ~ _
.
.
. .
· .. IRS 7
·—
in,
~ 1
3.0
3.2 3.4 3.6 3.8
WAVELENGTH IN MICRONS
FIGURE 3 High-resolution infrared spectra of the 3.3-3.4p hydrocarbon emission and
absorption bands in three extra-solar-systems sources and Comet Halley. The Orion Bar
is a shocked emission region in a molecular cloud; the Orion Bar curve is drawn after
data from Bregman et al. (1986, in preparation) as shown in Figure 1 of Allamandola et
al. (1987~. IRAS 21282+5050 is a compact star-like object of undetermined nature (after
data from de Muizon et al. 1986~. Comet P/Halley (Knacke et al. 1986) has features that
are broader and peak at longer wavelengths than the features of the comparison objects.
Bottom curve shows a 3.5pm interstellar absorption feature in the spectrum of IRS 7, a
highly reddened source near the Galactic Center (Jones et al. 1983~.
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PLANETARY SCIENCES
Classical novae typify the episodic circumstellar dust formation process.
Their infrared temporal development progresses in several identifiable
stages. The initial eruption results from a thermonuclear runaway on the
surface of a white dwarf that has been accreting matter from a companion
star in a close binary system. Hot gas expelled in the explosion is initially
seen as an expanding pseudophotosphere, or "fireball." Free-free and
line emission are observed when the expanding fireball becomes optically
thin. A dust condensation phase, characterized by rising infrared emission,
occurs in many novae within 50 to 200 days following the eruption. The
infrared emission continues to rise as the grains grow to a maximum radius.
Grain growth is terminated by decreasing density in the expanding shell.
The infrared emission then declines as the mature grains are dispersed by
the outflow into the ISM. The rate of decline of the infrared radiation and
the temporal development of the grain temperature suggest that the grain
radius decreases either by evaporation or sputtering during their dispersal.
Existing observations are consistent with the hypothesis that the nova grains
could be processed to interstellar grain sizes before they reach the ISM.
Hydrocarbon molecules described above (PAH's, ~C's, QCC's) may
produce some of the infrared emission features observed in planetary neb-
ulae, comets, and molecular cloud cores (see Figure 3 and Allamandola et
al. 1987). Although Hyland and MacGregor (1989) have reported possible
hydrocarbon emission from a recent nova, and Gerbault and Goebel (1989)
have argued that hydrocarbons may produce anomalous infrared emission
from some carbon stars, there is currently no compelling evidence that
hydrocarbon grains are an abundant constituent of the dust that is expelled
into the ISM in stellar outflows (Gehrz 1989~. Generally, circumstellar
hydrocarbon emission is observed only in sources with high-excitation neb-
ular conditions (Gehrz 1989~. There is circumstantial evidence that grains
condensed in the ejecta of novae, supernovae, and WR stars may contain
chemical abundance anomalies similar to those in solar system meteorite
inclusions (see below and Clayton 1982; Auras 1985; Gehrz 1988~.
INTERSTELLAR DUST GRAINS
Hackwell et al. (1970) showed that the same 1~ and 20-meter silicate
features responsible for emission in M-stars were present in absorption in
the infrared spectrum of the non-thermal Galactic Center source Sgr ~
They concluded that the absorption was caused by interstellar silicate grains
in the general ISM and that the grains are similar to those seen in M-stars.
Interstellar silicate absorption has since been confirmed for a variety of
other objects that are obscured by either interstellar dust or cold dust in
molecular clouds (see, for example, the BN object in Figure 2 and the other
objects embedded in compact HII regions discussed by Gillett et al. 1975~.
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AMERICAN AND S0~7ET RESEARCH
135
There is roughly 0.04 mag of silicate absorption per magnitude of visual
extinction to Sgr A. Observations of stellar sources with interstellar silicate
absorption along other lines of sight in the Galaxy yield similar results.
Continuum reddening by interstellar dust in the general ISM has been
measured by a number of investigators who compared opticaVinfrared
colors of reddened luminous stars with the intrinsic colors exhibited by
their unreddened counterparts (Sneden et al. 1978; Rieke and Lebofsky
1985~. Interstellar dust also polarizes starlight (Serkowski et al. 1975~.
An estimate of the grain size distribution for the grains causing this so-
called "general" interstellar extinction can be made given the wavelength
dependence of the reddening and polarization curves. The same reddening
and polarization laws appear to hold in all directions in the galaxy that
are not selectively affected by extinction by dense molecular clouds. The
reddening and polarization curves observed for stars deeply embedded in
dark and bright molecular clouds lead to the conclusion that the grains in
clouds are substantially larger than those causing the general interstellar
extinction (Breger e! al. 1981~.
The shape of the general interstellar extinction curve as determined
by opticaUinfrared measurements is consistent with the assumption that
the ISM contains carbon grains of very small radii (0.01-0.03pm) and a
silicate grain component (Mathis et al. 1977; Willner 1984; Draine 1985~.
Both components are also observed in emission in dense molecular cloud
cores where the dust is heated by radiation from embedded luminous
young stars (Gehrz et al. 1984~. The ISM dust in dense clouds contains a
probable hydrocarbon grain component that causes the 3.2-3.4pm emission
features (see Figure 3), and several other ~`unidentified', infrared emission
features that are seen in the ~14pm thermal infrared spectra of some
HII regions, molecular cloud cores, and young stellar objects (Allamandola
1984; Allamandola et al. 1987~. Jones et al. (1983) showed that a 3.4pm C-H
stretch absorption feature is present in the spectrum of the highly reddened
source IRS7 towards the Galactic Center (see Figure 3~. SiC has not been
observed in either the general extinction or in the extinctionJemission by
molecular cloud grains, but its presence may be obscured by the strong
silicate features.
At least some of the dust present in the ISM must be stardust produced
by the processes described above. Gehrz (1989) has reviewed the probable
sources for the production of the dust that is observed to permeate the
ISM. These include condensation in winds of evolved stars, condensation
in ejecta from nova and supernovae, and accretion in dark clouds. Most
of the silicates come from M stars and radio luminous OH/JR (RLOH/IR)
stars; carbon stars produce the carbon and SiC. Some stars, novae, and su-
pernovae may eject dust with chemical anomalies. Since there is apparently
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Pl~lNETARY SCIENCES
not a substantial stellar source of hydrocarbon grains, the ISM hydrocar-
bon component may be produced during grain processing or growth in
molecular clouds. The observation that there are large grains in molecular
clouds provides additional evidence that grains can grow efficiently in these
environments.
COMET DUST ANI) THE ZODIACAL CLOUD
The thermal infrared energy distributions of the comae and dust tails
of most comets (see Figures 1 and 2) show the characteristic near infrared
continuum dust emission that is probably caused by small iron or carbon
grains, and prominent 10 and 20m emission features characteristic of silicate
grains (Ney 1974; Gehrz and Ney 1986~. The cometary silicate features, first
discovered in Comet Bennett by Maas et al. (1970), suggest that comets
contain silicate materials similar to those observed in the circumstellar
shells of stars and in the ISM. Determinations of the composition of
Halley's coma grains by the Giotto PIA/PUMA mass spectrometers appear
to confirm the silicate grain hypothesis (Kissell et al. 1986~. There are some
basic differences however, between the cometary 10m emission features
and their stellar/interstellar counterparts (see Figure 2~. As discussed
above, the latter are broad and structureless suggesting a range of sizes
and an amorphous grain structure. The 10pm feature in P/Halley, on the
other hand, shows definite structure that suggests the presence of a grain
mixture containing 90% crystalline silicates (55% olivines, 35% pyroxene)
and only 10% lattice-layer silicates (Sandford and Walker 1985; Sandford
1987; Gehrz and Hanner 1987~. This observation would imply that the
grains in some comets may have undergone considerable high-temperature
processing compared to extra-solar-system grains. Some pristine comets,
like Kohoutek, show a 10m feature more like the stellar feature (see
Figure 2 and Rose 1979~. In the case of Kohoutek, the model fits indicate
that the mineral composition is almost entirely low-temperature hydrated
amorphous silicates (Rose 1979; Campins and ~kunaga 1987; Hanner and
Gehrz 1987; Brownlee 1987; and Sanford 1987~.
The 3 to 8pm thermal continuum radiation in the comae and Type II
dust tails of most comets are often hotter than the blackbody temperature
for the comet's heliocentric distance (Ney 1982~. This "superheat" suggests
that the grains are smaller than about 1 micron in radius. ISM grains may
be 10 to 100 times smaller than this. The antitail of Kohoutek was cold
with only weak silicate emission showing that comets also have much larger
grains frozen in their nuclei (Ney 1974~.
The 3.3-3.4,um feature (see Figure 3) in P/Halley suggests the presence
of hydrocarbon grains in the ablated material. It is obvious that the Halley
emission feature differs substantially both in width and effective wavelength
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137
from the 3.3-3.4pm emission seen in other astrophysical sources. The
implication Is that the material in P/Halley has been processed in some way
compared with the material observed in extra-solar-system objects.
Comets are presumably a Rosetta Stone for the formation of the
solar system because the contents of their nuclei were frozen in the very
early stages of the accretion of the solar nebula. The grains contained
therein may be indicative of interstellar material in the primitive solar
system, or may represent material processed significantly during the early
collapse of the solar system. These materials are ablated from comet
nuclei during perihelion passage. Cometary particles injected into the
interplanetary medium by ablation probably produce the shower meteors
and the zodiacal cloud. Studies of zodiacal dust particles may therefore
provide important information about the properties of cometary dust grains.
No cometary or zodiacal particles have yet been collected in situ. However,
Brownlee (1978) and his recent collaborators have collected grains believed
to be interplanetary dust particles (IDP's) from the stratosphere, on the
Greenland glaciers, and off the ocean floor. These particles yield infrared
absorption spectra showing that they are composed primarily of crystalline
pyroxene and olivines, and layer-lattice silicates (Sandford and Walker
1985). Composite spectra modeled by combinations of these particles
have been shown to match the Halley and Kohoutek data reasonably well
(Sandford and WaLker 1985; Sandford 1987). There is no evidence for
3.4pm hydrocarbon features in the laboratory spectra of IDP's, but there
are spectral pecularities that are associated with carbonaceous minerals.
WaLker (1987) has analyzed the mineralogy of IDP's and concludes that
they are comprised largely of materials that were formed in the solar system
and contain only a small fraction of ISM material in the form of very small
grains. The comparisons between IDP's and comets are, of course, only
circumstantial at present. It is therefore crucial to contemplate experiments
to collect zodiacal particles and cometary grains to establish the connections
between zodiacal, cometary, and interstellar/circumstellar particles.
THE SURVIVAL OF DUST GRAINS DURING STELLAR EVOLUTION
An intriguing question is whether significant numbers of stardust grains
can survive from the time that they condense in circumstellar outflows
until they are accreted into the cold solid bodies in primitive planetary
systems. While there is evidence that grains are rapidly destroyed in the
ISM by supernova shocks (Scab 1987) and are heated above the melting
point in the nebular phases of collapsing stellar systems (Boss 1988), there
is equally compelling evidence for the existence of solar-system grains
that are probably unaltered today from when they condensed long ago
in circumstellar outflows (Clayton 1982~. If stardust cannot survive long
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139
forbidden fine structure line emission has provided evidence for chemical
abundance anomalies that would be associated with the production of 22Na
and 26Al (Gehrz 1988~. Xe can be produced by a modified reprocess in
nucleosynthesis supernovae and trapped in grains that condense in the
ejecta (Black 1975~. Some of these anomalies also imply that the grains
survived intact from their sites of circumstellar condensation until their
accretion into the body of the meteorite. High-temperature processing
might be expected to drive off volatiles such as 22Ne and Xe which are
highly overabundant in some inclusions.
ESTABLISHING CONNECTIONS BETWEEN STARDUST ANI)
DUST IN THE SOLAR SYSTEM
The investigation of the properties of astrophysical dust grains is an
area that can benefit from studies that use the techniques of both astro-
physics and planetary science. It is now possible to conduct both remote
sensing and u' sau experiments to determine with certainty the mineral
composition and size distribution of the dust in the solar system. The Vega
and Giotto flybys of Comet P/Halley produced some tantalizing results that
demand confirmation. A sample return mission to a comet or asteroid is
of the highest priority. Any mission that returns a package to Earth after
a substantial voyage through the solar system should contain experiments
to collect interplanetary dust particles. It will be important to establish
whether IDP's that are collected from space resemble those collected on
the Earth and whether they have chemical anomalies that are similar to
those seen in meteorite inclusions. Examples of missions now planned that
could be modified to include IDP dust collection are Comet Rendezvous
and Asteroid Flyby (CRA]3 and the MARS SAMPLE RETURN missions.
The mineral composition of the zodiacal cloud remains uncertain. Infrared
satellite experiments to measure the spectrum of the cloud can provide sig-
nificant diagnostic information. Near infrared reflectance spectroscopy can
reveal the presence, mineral composition, and size distribution of various
types of silicate grains. These features have already been observed in the
spectra of asteroids. Emission spectroscopy can determine whether silicates
and silicon carbide are present. The contrast of the 10-20pm emission fea-
tures are related to the size distribution (Rose 1979~. Ground-based studies
of the mineralogy of stardust and solar system dust also require high signal
to noise high-resolution spectroscopy of the emission features shown in
Figures 1 and 3 in a wide variety of sources. New improvements in infrared
area detectors should make achievement of this objective realistic within
the coming decade.
OCR for page 140
140
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ACKNOWLEDGEMENTS
The author is supported by me National Science Foundation, Na-
tional Aeronautics and Space Administration, the U.S. Air Force, and the
Graduate School of the University of Minnesota.
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Representative terms from entire chapter:
dust grains
