207:
33:
549:. Topics covered are: historical perspectives; cometary dust; near-Earth environment; meteoroids and meteors; properties of interplanetary dust, information from collected samples; in situ measurements of cosmic dust; numerical modeling of the Zodiacal Cloud structure; synthesis of observations; instrumentation; physical processes; optical properties of interplanetary dust; orbital evolution of interplanetary dust; circumplanetary dust, observations and simple physics; interstellar dust and circumstellar dust disks.
292:
560:. Included are discussions of dust in various environments: from planetary atmospheres and airless bodies over interplanetary dust, meteoroids, comet dust and emissions from active moons to interstellar dust and protoplanetary disks. Diverse research techniques and results, including in-situ measurement, remote observation, laboratory experiments and modelling, and analysis of returned samples are discussed.
372:
969:
K. E.; Magnes, W.; McNutt, R. L.; Miller, J.; Moebius, E.; Mostafavi, P.; Opher, M.; Paxton, L.; Plaschke, F.; Poppe, A. R.; Roelof, E. C.; Runyon, K.; Redfield, S.; Schwadron, N.; Sterken, V.; Swaczyna, P.; Szalay, J.; Turner, D.; Vannier, H.; Wimmer-Schweingruber, R.; Wurz, P.; Zirnstein, E. J. (2023).
968:
Brandt, P. C.; Provornikova, E.; Bale, S. D.; Cocoros, A.; DeMajistre, R.; Dialynas, K.; Elliott, H. A.; Eriksson, S.; Fields, B.; Galli, A.; Hill, M. E.; Horanyi, M.; Horbury, T.; Hunziker, S.; Kollmann, P.; Kinnison, J.; Fountain, G.; Krimigis, S. M.; Kurth, W. S.; Linsky, J.; Lisse, C. M.; Mandt,
383:
Interplanetary dust has been found to form rings of dust in the orbital space of
Mercury and Venus. Venus's orbital dust ring is suspected to originate either from yet undetected Venus trailing asteroids, interplanetary dust migrating in waves from orbital space to orbital space, or from the remains
271:
The lifetimes of these dust particles are very short compared to the lifetime of the Solar System. If one finds grains around a star that is older than about 10,000,000 years, then the grains must have been from recently released fragments of larger objects, i.e. they cannot be leftover grains from
537:
which contained chapters on comets along with zodiacal light as indicator of interplanetary dust, meteors, interstellar dust, microparticle studies by sampling techniques, and microparticle studies by space instrumentation. Attention is also given to lunar and planetary impact erosion, aspects of
847:
Horányi, M.; Hoxie, V.; James, D.; Poppe, A.; Bryant, C.; Grogan, B.; Lamprecht, B.; Mack, J.; Bagenal, F.; S. Batiste; Bunch, N.; Chantanowich, T.; Christensen, F.; Colgan, M.; Dunn; Drake, G.; Fernandez, A.; Finley, T.; Holland, G.; Jenkins, A.; Krauss, C.; Krauss, E.; Krauss, O.; Lankton, M.;
408:
predicted that micrometeorites smaller than 100 micrometers in diameter might be decelerated on impact with the Earth's upper atmosphere without melting. The modern era of laboratory study of these particles began with the stratospheric collection flights of
424:
nature and unequilibrated cosmic-average composition of other particles suggested that they began as fine-grained aggregates of nonvolatile building blocks and cometary ice. The interplanetary nature of these particles was later verified by
361:
At least 2 resonant dust rings are known (for example, the Earth-resonant dust ring, although every planet in the Solar System is thought to have a resonant ring with a "wake") (Jackson and Zook, 1988, 1992) (Dermott, S.F. et al., 1994,
922:
While there is good evidence now that Mars, the dustiest planet we know of, is the source of the zodiacal light, Jørgensen and his colleagues cannot yet explain how the dust could have escaped the grip of
Martian
283:
Particles which are affected primarily by radiation pressure are known as "beta meteoroids". They are generally less than 1.4 × 10 g and are pushed outward from the Sun into interstellar space.
240:
It was believed that IDPs had originated from comets or asteroids whose particles had dispersed throughout the extent of the cloud. However, further observations have suggested that Mars
276:(Backman, private communication). Therefore, the grains would be "later-generation" dust. The zodiacal dust in the Solar System is 99.9% later-generation dust and 0.1% intruding
1209:
Hudson, B.; Flynn, G. J.; Fraundorf, P.; Hohenberg, C. M.; Shirck, J. (January 1981). "Noble Gases in
Stratospheric Dust Particles: Confirmation of Extraterrestrial Origin".
94:. This system of particles has been studied for many years in order to understand its nature, origin, and relationship to larger bodies. There are several methods to obtain
906:
538:
particle dynamics, and acceleration techniques and high-velocity impact processes employed for the laboratory simulation of effects produced by micrometeoroids.
1684:
Dermott, S.F.; Jayaraman, S.; Xu, Y.L.; Gustafson, A.A.S.; Liou, J.C. (30 June 1994). "A circumsolar ring of asteroid dust in resonant lock with the Earth".
237:
grains (Backman, D., 1997). The origins of the zodiacal cloud have long been subject to one of the most heated controversies in the field of astronomy.
1678:
299:, comparable to images of simulations of the Solar System's interplanetary dust cloud, which has been suggested to be imaged from beyond it in the
1030:
1660:
1509:
1471:
1430:
499:
189:
171:, this dust cloud is visible as the zodiacal light in a moonless and naturally dark sky and is best seen sunward during astronomical
1356:
206:
530:
1532:
789:(1999). "Irradiated interplanetary dust particles as a possible solution for the deuterium/hydrogen paradox of Earth's oceans".
935:
32:
252:
The main physical processes "affecting" (destruction or expulsion mechanisms) interplanetary dust particles are: expulsion by
1730:
1495:
679:
553:
526:
Collections of review articles on various aspects of interplanetary dust and related fields appeared in the following books:
511:
1140:
Brownlee, D. E. (December 1977). "Interplanetary dust - Possible implications for comets and presolar interstellar grains".
102:
307:
The interplanetary dust cloud has a complex structure (Reach, W., 1997). Apart from a background density, this includes:
1252:
Bradley, J. P.; Brownlee, D. E.; Fraundorf, P. (December 1984). "Discovery of nuclear tracks in interplanetary dust".
458:
1142:
In: Protostars and
Planets: Studies of Star Formation and of the Origin of the Solar System. (A79-26776 10-90) Tucson
1799:
1056:
445:
448:(not to mention being small astronomical objects in their own right) available for study in laboratories today.
1751:
Reach, W.T.; Franz, B.A.; Weiland, J.L. (1997). "The Three-Dimensional
Structure of the Zodiacal Dust Bands".
834:"Pioneer 10 observations of zodiacal light brightness near the ecliptic - Changes with heliocentric distance"
420:
Although some of the particles found were similar to the material in present-day meteorite collections, the
265:
257:
210:
95:
1794:
579:
971:"Future Exploration of the Outer Heliosphere and Very Local Interstellar Medium by Interstellar Probe"
436:
In that context a program for atmospheric collection and curation of these particles was developed at
1804:
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1693:
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1386:
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864:
798:
752:
714:
652:
482:
476:
437:
389:
488:
589:
296:
277:
273:
241:
234:
1167:& Walker, R. M. (1982) . "Laboratory studies of interplanetary dust". In Wilkening, L. (ed.).
1709:
1588:
1412:
1380:
1338:
1293:
1164:
880:
740:
702:
569:
515:
410:
385:
376:
327:
316:
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253:
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1426:
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1234:
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1008:
990:
814:
323:
198:
probe was designed to detect impacts of the dust from the zodiacal cloud in the Solar System.
109:
556:, Jesús Martín-Pintado, Veerle J. Sterken, and Andrew Westphal collected reviews in the book
1768:
1701:
1648:
1623:
1606:
1580:
1563:
1459:
1269:
1226:
1112:
1102:
998:
982:
872:
848:
Mitchell, C.; Neeland, M.; Resse, T.; Rash, K.; Tate, G.; Vaudrin, C.; Westfall, J. (2008).
806:
760:
707:
Proceedings of Lunar and
Planetary Science Conference 10th, Houston, Tex., March 19–23, 1979
599:
542:
393:
291:
218:
141:
129:
87:
1453:
225:
The sources of interplanetary dust particles (IDPs) include at least: asteroid collisions,
441:
943:
1764:
1697:
1619:
1576:
1422:
1390:
1348:
1265:
1222:
1195:
1149:
1098:
868:
802:
756:
718:
1117:
1082:
1003:
970:
604:
594:
347:
335:
185:
133:
67:
37:
1735:
Physics, Chemistry and
Dynamics of Interplanetary Dust, ASP Conference series, Vol 104
1783:
1627:
786:
764:
355:
331:
280:
dust. All primordial grains from the Solar System's formation were removed long ago.
132:
typically range 10–100 μm. Microscopic impact craters on lunar rocks returned by the
121:
54:, in this composite image of the night sky above the northern and southern hemisphere
1297:
884:
1713:
1639:
1592:
849:
584:
494:
414:
405:
351:
343:
194:
91:
1273:
1230:
833:
657:
574:
430:
230:
145:
137:
79:
71:
46:
1499:
1087:
Proceedings of the
National Academy of Sciences of the United States of America
986:
375:
First ever panorama image of the dust ring of Venus's orbital space, imaged by
268:, mutual collisions, and the dynamical effects of planets (Backman, D., 1997).
1463:
876:
624:
470:
464:
421:
371:
339:
312:
261:
180:
117:
17:
1281:
994:
1635:
1498:; Martín-Pintado, Jesús; Sterken, Veerle J.; Westphal, Andrew, eds. (2019).
1057:"Parker Solar Probe Captures First Complete View of Venus Orbital Dust Ring"
426:
214:
113:
51:
1772:
1289:
1238:
1182:
Walker, R. M. (January 1986). "Laboratory studies of interplanetary dust".
1126:
1107:
1012:
818:
703:"Properties of microcraters and cosmic dust of less than 1000 Å dimensions"
1670:
Backman, Dana (1997). "Exozody
Workshop, NASA-Ames, October 23–25, 1997".
1652:
810:
172:
168:
160:
125:
105:
653:"What scientists found after sifting the dust in the solar system - bri"
1031:"What Scientists Found After Sifting Through Dust in the Solar System"
163:
of radius 15 km (with density of about 2.5 g/cm). Straddling the
1705:
1584:
1083:"The Theory of Micro-Meteorites. Part I. In an Isothermal Atmosphere"
552:
2019 Rafael
Rodrigo, Jürgen Blum, Hsiang-Wen Hsu, Detlef V. Koschny,
164:
83:
1601:
1558:
1494:
Rodrigo, Rafael; Blum, Jürgen; Hsu, Hsiang-Wen; Koschny, Detlef V.;
1311:
440:
in Texas. This stratospheric micrometeorite collection, along with
144:
distribution of interplanetary dust at 1 AU, describes the flux of
1742:
Reach, W. (1997). "General Structure of the Zodiacal Dust Cloud".
907:"Serendipitous Juno Detections Shatter Ideas About Zodiacal Light"
545:, Bo Gustafson, Stan Dermott, and Hugo Fechtig published the book
370:
290:
226:
188:
with the interplanetary dust cloud in the Solar System. Also, the
101:
In the Solar System, interplanetary dust particles have a role in
31:
1721:
Dermott, S.F. (1997). "Signatures of Planets in Zodiacal Light".
1343:. Chichester, New York: John Wiley & Sons. pp. 607–670.
151:
The total mass of the interplanetary dust cloud is approximately
75:
1602:"Orbital evolution of dust particles from comets and asteroids"
322:
A number of dust bands, the sources of which are thought to be
1411:
Grün, E.; Gustafson, B.A.S.; Dermott, S.; Fechtig, H. (2001).
1733:(1996). "Optical and Thermal Properties of Zodiacal Dust".
739:
Grün, E.; Zook, H.A.; Fechtig, H.; Giese, R.H. (May 1985).
50:
and the rest of its band, which is visually crossed by the
1559:"A Solar System Dust Ring with the Earth as its Shepherd"
36:
The interplanetary dust cloud illuminated and visible as
1641:
A Survey of Radial Velocities in the Zodiacal Dust Cloud
1260:(4681): 1432–1434.ResearchsupportedbyMcCroneAssociates.
413:
and collaborators in the 1970s using balloons and then
244:
may be responsible for the zodiacal cloud's formation.
1744:
Extrasolar Zodiacal Emission - NASA Study Panel Report
1723:
Extrasolar Zodiacal Emission - NASA Study Panel Report
1672:
Extrasolar Zodiacal Emission - NASA Study Panel Report
850:"The Student Dust Counter on the New Horizons Mission"
480:(heliocentric orbit out to the distance of Jupiter),
264:
pressure (with significant electromagnetic effects),
1316:
NASA – Johnson Space Center program, Cosmic Dust Lab
456:
Spacecraft that have carried dust detectors include
229:activity and collisions in the inner Solar System,
1679:NASA Panel Report on Extrasolar Zodiacal Emission
510:The Solar interplanetary dust cloud obscures the
1171:. University of Arizona Press. pp. 383–409.
184:spacecraft observations in the 1970s linked the
741:"Collisional balance of the meteoritic complex"
1533:"Cosmic Dust from the Laboratory to the Stars"
1024:
1022:
647:
645:
112:, which is the most prominent feature of the
8:
1501:Cosmic Dust from the Laboratory to the Stars
1458:. Astronomy and Astrophysics Library. 2001.
713:. New York: Pergamon Press Inc.: 1649–1663.
558:Cosmic Dust from the Laboratory to the Stars
140:particles bombarding the lunar surface. The
116:'s radiation, with wavelengths ranging 5–50
330:. The three strongest bands arise from the
785:Pavlov, Alexander A.; Pavlov, Anatoli K.;
1116:
1106:
1002:
791:Journal of Geophysical Research: Planets
205:
963:
961:
616:
444:from meteorites, are unique sources of
701:Morrison, D.A.; Clanton, U.S. (1979).
258:Poynting-Robertson (PR) radiation drag
514:, making observations of it from the
7:
905:Shekhtman, Svetlana (8 March 2021).
342:. Other source families include the
500:Venetia Burney Student Dust Counter
1081:Whipple, Fred L. (December 1950).
136:revealed the size distribution of
82:) that pervades the space between
25:
1600:Jackson A.A.; Zook, H.A. (1992).
1557:Jackson A.A.; Zook, H.A. (1988).
1496:Levasseur-Regourd, Anny-Chantal
315:—their source is thought to be
27:Small particles between planets
1217:(4480): 383–386(SciHomepage).
1055:Rehm, Jeremy (15 April 2021).
554:Anny-Chantal Levasseur-Regourd
512:extragalactic background light
219:extrasolar interplanetary dust
1:
1274:10.1126/science.226.4681.1432
1029:Garner, Rob (12 March 2019).
832:Hannter; et al. (1976).
358:families (Reach et al. 1996).
148:from nm to mm sizes at 1 AU.
124:of grains characterizing the
1628:10.1016/0019-1035(92)90057-E
1379:McDonnell, J. A. M. (1978).
1231:10.1126/science.211.4480.383
765:10.1016/0019-1035(85)90121-6
940:GENESIS Discovery 5 Mission
936:"Micrometeorite Background"
392:and then itself, the Solar
1821:
987:10.1007/s11214-022-00943-x
1464:10.1007/978-3-642-56428-4
1337:McDonnel, J.A.M. (1978).
942:. Caltech. Archived from
877:10.1007/s11214-007-9250-y
446:extraterrestrial material
60:interplanetary dust cloud
522:Major Review Collections
400:Dust collection on Earth
248:Life cycle of a particle
1731:Levasseur-Regourd, A.C.
680:Levasseur-Regourd, A.C.
1773:10.1006/icar.1997.5704
1647:. New York: Springer.
1108:10.1073/pnas.36.12.687
492:(Saturn orbiter), and
384:of the Solar System's
380:
304:
222:
96:space dust measurement
66:(as the source of the
55:
975:Space Science Reviews
857:Space Science Reviews
661:. NASA. 12 March 2019
580:Interplanetary medium
374:
294:
217:, with light from an
209:
40:, with its parts the
35:
1504:. Berlin: Springer.
1417:. Berlin: Springer.
811:10.1029/1999JE001120
438:Johnson Space Center
433:track observations.
390:proto-planetary disc
159:, or the mass of an
1765:1997Icar..127..461R
1698:1994Natur.369..719D
1620:1992Icar...97...70J
1577:1989Natur.337..629J
1455:Interplanetary Dust
1423:2001indu.book.....G
1414:Interplanetary Dust
1391:1978codu.book.....M
1349:1978codu.book..607F
1266:1984Sci...226.1432B
1223:1981Sci...211..383H
1196:1986NASCP2403...55W
1150:1978prpl.conf..134B
1099:1950PNAS...36..687W
869:2008SSRv..140..387H
803:1999JGR...10430725P
757:1985Icar...62..244G
719:1979LPSC...10.1649M
590:Dust storms on Mars
547:Interplanetary Dust
486:(Jupiter Orbiter),
388:, out of which its
350:, and possibly the
317:short-period comets
297:protoplanetary disk
278:interstellar medium
274:protoplanetary disk
235:interstellar medium
570:Circumstellar disk
516:Inner Solar System
411:Donald E. Brownlee
386:circumstellar disc
381:
377:Parker Solar Probe
328:main asteroid belt
305:
301:Outer Solar System
254:radiation pressure
223:
213:of a view from an
192:instrument on the
56:
1800:Planetary science
1662:978-0-387-77705-4
1636:May, Brian Harold
1571:(6208): 629–631.
1511:978-94-024-2009-8
1473:978-3-642-62647-0
1432:978-3-540-42067-5
946:on 26 August 2007
797:(E12): 30725–28.
787:Kasting, James F.
691:Backman, D., 1997
324:asteroid families
110:thermal radiation
88:planetary systems
16:(Redirected from
1812:
1776:
1747:
1738:
1737:. pp. 301–.
1726:
1717:
1706:10.1038/369719a0
1692:(6483): 719–23.
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1585:10.1038/337629a0
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1318:. 6 January 2016
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863:(1–4): 387–402.
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621:
600:Exozodiacal dust
533:edited the book
506:Obscuring effect
394:planetary system
287:Cloud structures
233:collisions, and
211:Artist's concept
158:
156:
108:and in emitting
21:
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1551:Further reading
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1165:Brownlee, D. E.
1163:Fraundorf, P.;
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1093:(12): 687–695.
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442:presolar grains
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70:), consists of
28:
23:
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5:
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1759:(2): 461–484.
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751:(2): 244–272.
731:
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672:
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615:
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607:
605:Zodiacal light
602:
597:
595:Micrometeoroid
592:
587:
582:
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562:
531:Tony McDonnell
523:
520:
518:very limited.
507:
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364:
363:
359:
336:Koronis family
320:
295:An image of a
288:
285:
249:
246:
203:
200:
186:zodiacal light
134:Apollo Program
128:emission near
122:particle sizes
90:, such as the
68:zodiacal light
64:zodiacal cloud
38:zodiacal light
26:
24:
18:Zodiacal cloud
14:
13:
10:
9:
6:
4:
3:
2:
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1358:0-471-99512-6
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1312:"Cosmic Dust"
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543:Eberhard Grün
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332:Themis family
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1795:Solar System
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1653:10044/1/1333
1645:(PhD thesis)
1640:
1614:(1): 70–84.
1611:
1605:
1568:
1562:
1536:. Retrieved
1527:
1515:. Retrieved
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1064:. Retrieved
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948:. Retrieved
944:the original
939:
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910:
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890:17 September
888:. Retrieved
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748:
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722:. Retrieved
710:
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663:. Retrieved
656:
632:. Retrieved
628:
625:"False Dawn"
619:
585:Martian soil
557:
551:
546:
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534:
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525:
509:
495:New Horizons
493:
487:
481:
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469:
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457:
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435:
419:
406:Fred Whipple
403:
382:
306:
282:
270:
251:
239:
224:
195:New Horizons
193:
179:
177:
150:
100:
92:Solar System
78:floating in
63:
59:
57:
45:
41:
29:
1805:Outer space
1790:Cosmic dust
1382:Cosmic Dust
1340:Cosmic Dust
1144:: 134–150.
658:EurekAlert!
634:14 February
629:www.eso.org
575:Cosmic dust
535:Cosmic Dust
452:Experiments
431:solar flare
313:dust trails
311:At least 8
266:sublimation
242:dust storms
231:Kuiper belt
146:cosmic dust
138:cosmic dust
80:outer space
72:cosmic dust
47:gegenschein
1784:Categories
1538:5 February
1517:5 February
1479:5 February
1438:5 February
1396:5 February
1364:22 January
1066:21 January
1040:21 January
770:23 January
724:3 February
611:References
471:Pioneer 11
465:Pioneer 10
422:nanoporous
417:aircraft.
396:, formed.
340:Eos family
338:, and the
262:solar wind
167:along the
157:10 kg
103:scattering
42:false dawn
1282:0036-8075
995:0038-6308
427:noble gas
404:In 1951,
256:, inward
215:exoplanet
114:night sky
76:particles
52:Milky Way
1638:(2008).
1322:14 March
1298:27703897
1290:17788999
1239:17748271
1127:16578350
1013:36874191
950:4 August
923:gravity.
885:17522966
819:11543198
665:12 March
564:See also
529:In 1978
227:cometary
173:twilight
169:ecliptic
161:asteroid
142:’’Grün’’
126:infrared
106:sunlight
1761:Bibcode
1714:4345910
1694:Bibcode
1616:Bibcode
1593:4351090
1573:Bibcode
1419:Bibcode
1387:Bibcode
1345:Bibcode
1262:Bibcode
1254:Science
1219:Bibcode
1211:Science
1192:Bibcode
1184:In NASA
1146:Bibcode
1118:1063272
1095:Bibcode
1004:9974711
865:Bibcode
799:Bibcode
753:Bibcode
715:Bibcode
489:Cassini
483:Galileo
477:Ulysses
354:and/or
348:Eunomia
326:in the
181:Pioneer
86:within
84:planets
74:(small
1753:Icarus
1712:
1686:Nature
1659:
1607:Icarus
1591:
1564:Nature
1508:
1470:
1429:
1355:
1296:
1288:
1280:
1237:
1190:: 55.
1169:Comets
1125:
1115:
1061:JHUAPL
1011:
1001:
993:
883:
817:
745:Icarus
682:, 1996
459:Helios
356:Hygiea
334:, the
202:Origin
165:zodiac
120:. The
1710:S2CID
1589:S2CID
1294:S2CID
981:(2).
916:8 May
881:S2CID
853:(PDF)
541:2001
498:(see
362:1997)
352:Vesta
344:Maria
221:cloud
190:VBSDC
62:, or
1657:ISBN
1540:2022
1519:2022
1506:ISBN
1481:2022
1468:ISBN
1440:2022
1427:ISBN
1398:2022
1366:2022
1353:ISBN
1324:2016
1286:PMID
1278:ISSN
1235:PMID
1188:2403
1123:PMID
1068:2023
1042:2023
1035:NASA
1009:PMID
991:ISSN
952:2008
918:2022
911:NASA
892:2022
815:PMID
772:2022
726:2022
667:2019
636:2017
429:and
272:the
178:The
58:The
1769:doi
1757:127
1702:doi
1690:369
1649:hdl
1624:doi
1581:doi
1569:337
1460:doi
1270:doi
1258:226
1227:doi
1215:211
1113:PMC
1103:doi
999:PMC
983:doi
979:219
873:doi
861:140
807:doi
795:104
761:doi
502:).
415:U-2
153:3.5
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155:×
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