ライフサイエンスコーパス: interplanetary dust

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 produced a transient increase in the flux of interplanetary dust-derived 3He.

6 xtraterrestrial accretion from meteoroids or interplanetary dust is proposed as a mechanism that coul

7 to the atmosphere by comets, meteorites, and interplanetary dust or synthesized in the atmosphere fro

8 An interplanetary dust particle contains a submicrometer cr

9 ciated with a 15N enrichment in an anhydrous interplanetary dust particle.

10 ith delivery of intact exogenous organics in interplanetary dust particles (IDPs) and ultraviolet pro

11 Interplanetary dust particles (IDPs) collected in the Ea

12 naceous Renazzo-type (CR) chondrites and two interplanetary dust particles (IDPs) originating from co

13 ed spectral properties of silicate grains in interplanetary dust particles (IDPs) were compared with

14 he Solar System, Earth has been bombarded by interplanetary dust particles (IDPs), which are asteroid

15 ature in interstellar grains embedded within interplanetary dust particles (IDPs).

16 ied six circumstellar silicate grains within interplanetary dust particles (IDPs).

17 tes (originating from the asteroid belt) and interplanetary dust particles (possibly from comets) pre

18 are similar, but not identical, to those in interplanetary dust particles and carbonaceous meteorite

19 ilicates with amorphous rims are observed on interplanetary dust particles and on lunar and asteroid

20 able silicate materials in chondritic porous interplanetary dust particles appear to be absent from t

21 Interplanetary dust particles are generally regarded as

22 mportance of stratospheric chondritic porous interplanetary dust particles as a precious source of th

23 e was expected to resemble chondritic porous interplanetary dust particles because many, and possibly

24 At this time, meteorites and interplanetary dust particles delivered organics such as

25 hydrogen and nitrogen isotopic anomalies in interplanetary dust particles have been associated with

26 Interplanetary dust particles hit the surfaces of airles

27 onaceous material in interstellar grains and interplanetary dust particles indicate that condensed or

28 mates of ultraviolet degradation of accreted interplanetary dust particles or carbonaceous chondrite

29 dust detector indicate a daily mass input of interplanetary dust particles ranging from 100 to 300 to

30 merical modeling of the orbital evolution of interplanetary dust particles revealed that, over the pa

31 infrared and the study of chondritic porous interplanetary dust particles that were thought, but not

32 s aliphatic hydrocarbons similar to those in interplanetary dust particles thought to be derived from

33 terials via comets, (micro-) meteorites, and interplanetary dust particles to the primitive Earth mig

34 Primitive meteorites, interplanetary dust particles, and comets contain dust g

35 t exogenous materials, including meteorites, interplanetary dust particles, and interstellar ice anal

36 oss certain Comet 81P/Wild 2 organic solids, interplanetary dust particles, and primitive IOM.

37 ent or very depleted in fragile, carbon-rich interplanetary dust particles, some of which enter the a

38 primarily meteoritic in origin and not from interplanetary dust particles.

39 e mineral grains on the exterior surfaces of interplanetary dust particles.

40 poorer in aromatics than are meteorites and interplanetary dust particles.

41 matter reach and even exceed those found in interplanetary dust particles.

42 gate particles, similar to chondritic porous interplanetary dust particles.

43 ed into the inner solar system as comets and interplanetary dust particles.

44 lar to those found in meteorites and in some interplanetary dust particles.

45 nar surface is exposed to the same stream of interplanetary dust particles.

46 ding of the sources, sinks, and transport of interplanetary dust throughout the inner solar system an

47 helium-3, a tracer of the accretion rate of interplanetary dust to Earth.

48 of pick-up ions has also been used to study interplanetary dust, Venus' tail and the interstellar me

49 s from pyrrhotite ([Fe, Ni](1-x)S) grains in interplanetary dust, which show a broad FeS feature cent

50 zed during entry of, meteorites, comets, and interplanetary dust would have been scavenged by cloud d