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1 y of nanoparticles at planetary surfaces, in interplanetary dust and in the biosphere, will depend on
2 atmosphere and sunlight reflected from local interplanetary dust, and large discrepancies in the infe
3 ations of helium-3, a tracer of fine-grained interplanetary dust, and large impacts indicates that th
4 s of the solar system-asteroids, comets, and interplanetary dust-are chaotic and undergo large change
5 n of L-chondrite-like near-Earth objects and interplanetary dust concentrated at 1.4 degrees (refs. (
6 produced a transient increase in the flux of interplanetary dust-derived 3He.
7 xtraterrestrial accretion from meteoroids or interplanetary dust is proposed as a mechanism that coul
8 to the atmosphere by comets, meteorites, and interplanetary dust or synthesized in the atmosphere fro
9                                           An interplanetary dust particle contains a submicrometer cr
10 ciated with a 15N enrichment in an anhydrous interplanetary dust particle.
11 ith delivery of intact exogenous organics in interplanetary dust particles (IDPs) and ultraviolet pro
12                                              Interplanetary dust particles (IDPs) collected in the Ea
13 naceous Renazzo-type (CR) chondrites and two interplanetary dust particles (IDPs) originating from co
14 ed spectral properties of silicate grains in interplanetary dust particles (IDPs) were compared with
15 he Solar System, Earth has been bombarded by interplanetary dust particles (IDPs), which are asteroid
16 ature in interstellar grains embedded within interplanetary dust particles (IDPs).
17 ied six circumstellar silicate grains within interplanetary dust particles (IDPs).
18 tes (originating from the asteroid belt) and interplanetary dust particles (possibly from comets) pre
19  are similar, but not identical, to those in interplanetary dust particles and carbonaceous meteorite
20 ilicates with amorphous rims are observed on interplanetary dust particles and on lunar and asteroid
21 able silicate materials in chondritic porous interplanetary dust particles appear to be absent from t
22                                              Interplanetary dust particles are generally regarded as
23 mportance of stratospheric chondritic porous interplanetary dust particles as a precious source of th
24 e was expected to resemble chondritic porous interplanetary dust particles because many, and possibly
25                 At this time, meteorites and interplanetary dust particles delivered organics such as
26  hydrogen and nitrogen isotopic anomalies in interplanetary dust particles have been associated with
27 logical similarity with anhydrous chondritic interplanetary dust particles having a probable cometary
28                                              Interplanetary dust particles hit the surfaces of airles
29 onaceous material in interstellar grains and interplanetary dust particles indicate that condensed or
30 mates of ultraviolet degradation of accreted interplanetary dust particles or carbonaceous chondrite
31 dust detector indicate a daily mass input of interplanetary dust particles ranging from 100 to 300 to
32 merical modeling of the orbital evolution of interplanetary dust particles revealed that, over the pa
33  infrared and the study of chondritic porous interplanetary dust particles that were thought, but not
34 s aliphatic hydrocarbons similar to those in interplanetary dust particles thought to be derived from
35 terials via comets, (micro-) meteorites, and interplanetary dust particles to the primitive Earth mig
36                        Primitive meteorites, interplanetary dust particles, and comets contain dust g
37 t exogenous materials, including meteorites, interplanetary dust particles, and interstellar ice anal
38 oss certain Comet 81P/Wild 2 organic solids, interplanetary dust particles, and primitive IOM.
39 ent or very depleted in fragile, carbon-rich interplanetary dust particles, some of which enter the a
40  primarily meteoritic in origin and not from interplanetary dust particles.
41 e mineral grains on the exterior surfaces of interplanetary dust particles.
42  poorer in aromatics than are meteorites and interplanetary dust particles.
43  matter reach and even exceed those found in interplanetary dust particles.
44 gate particles, similar to chondritic porous interplanetary dust particles.
45 ed into the inner solar system as comets and interplanetary dust particles.
46 lar to those found in meteorites and in some interplanetary dust particles.
47 nar surface is exposed to the same stream of interplanetary dust particles.
48 ding of the sources, sinks, and transport of interplanetary dust throughout the inner solar system an
49  helium-3, a tracer of the accretion rate of interplanetary dust to Earth.
50  of pick-up ions has also been used to study interplanetary dust, Venus' tail and the interstellar me
51 s from pyrrhotite ([Fe, Ni](1-x)S) grains in interplanetary dust, which show a broad FeS feature cent
52 zed during entry of, meteorites, comets, and interplanetary dust would have been scavenged by cloud d