The Detection of a Dust Trail in the Orbit of an Earth‐threatening Long‐Period Comet

Jenniskens, Peter; Betlem, Hans; Lignie, Marc de; Langbroek, Marco

doi:10.1086/303853

Cited by 49 publications

(58 citation statements)

References 15 publications

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“…However, the α-Monocerotids -meteoroids of a long period shower with unknown parent body -have somewhat similar properties. They are stronger than Perseids (Jenniskens et al 1997) and have lower content of sodium (Fig. 2).…”

Section: Probable Cometary Crust Materialsmentioning

confidence: 97%

Properties of meteoroids from different classes of parent bodies

Borovička

2006

Proc. IAU

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Abstract. Meteoroids observed to disintegrate in the terrestrial atmosphere can be directly linked to their parent bodies in case that they belong to certain meteor showers. We present a list of two dozens of parent bodies reliably associated with well recognized meteor showers. Among the parent bodies are long period comets, Halley-type comets, Jupiter family comets, comets of the inner solar system (such as 2P/Encke) and asteroids.Physical and chemical properties of meteoroids coming from various parents are compared on the basis of meteor heights, decelerations, light curves and spectra. Jupiter family comets produce meteoroids with the lowest strength, namely porous aggregates of dust grains with bulk densities of about 0.3 g cm −3 or less. Halley type material is somewhat stronger and the material related to comet Encke is even stronger. In addition, small strong constituents, perhaps similar to carbonaceous chondrites, can be encountered within the normal cometary material. The strength of cometary material is also enhanced by long-term exposure to cosmic rays and by solar heating in the vicinity to the Sun (r < 0.2 AU). Both these processes lead to the loss of volatile sodium. Southern δ-Aquariids, Geminids and partly also Quadrantids were influenced by solar radiation. We argue that these showers, the asteroids associated with them ((3200) Phaethon and 2003 EH 1), and the whole interplanetary complexes they belong to are of cometary origin. The argument is supported by lower than chondritic Fe/Mg ratio found in Geminids as well as in Halley type comets. The typical property of stony meteoroids of asteroidal origin is the presence of internal cracks which cause that the incoming meteoroids are much weaker than the recovered meteorites.

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Section: Probable Cometary Crust Materialsmentioning

confidence: 97%

Properties of meteoroids from different classes of parent bodies

Borovička

2006

Proc. IAU

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“…Using this argument, Jenniskens et al (1997) concluded that the main component of the Quadrantids is only about 500 years old, since they found a very narrow main peak in the activity curve. However, the perturbation action of Jupiter can cause a more complicated structural evolution of a stream or filament.…”

Section: Some Notes On the Aging Of Filamentsmentioning

confidence: 98%

The meteor-shower complex of 96P/Machholz revisited

Neslušan

Kaňuchová

Tomko

2013

A&A

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Aims. The structure of the complex of meteoroid particles released from comet 96P/Machholz is studied to reveal a relationship among the meteor showers observed in the Earth's atmosphere that belong to this complex. Methods. For eight perihelion passages of the parent comet in the past, we model theoretical streams associated with comet 96P and follow their dynamical evolution until the present. Subsequently, we analyze the orbital characteristics of the streams, especially of their parts approaching the Earth's orbit. Results. The dynamics of the stream is controlled by Jupiter, which changes the initial orbits of the particles into the orbits situated within several specific corridors. It thus creates a filamentary structure of the complex. Six filaments approach the orbit of the Earth producing four well-known meteor showers and two showers, whose identification with κ-Velids and α-Cetids is not certain. The known showers, in order of the predicted abundance of meteors, are daytime Arietids, Southern δ-Aquarids, Quadrantids, and Northern δ-Aquarids. The filaments corresponding to the Arietids, δ-Aquarids S and N, and possibly α-Cetids constitute the ecliptical component and those corresponding to the Quadrantids and possibly κ-Velids constitute the toroidal component of the complex.

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“…The formation of these dust trails is well understood ever since the first detection of a dust trail from an unknown long-period comet in 1995, which caused the alphaMonocerotid meteor shower [Jenniskens et 1935,1986,1994, and 2007 atmosphere than other meteoroids of similar size and speed [Jenniskens et al, 1997]. It is theorized that this difference occurs because these meteoroids were crumbs of the comet's pristine crust.…”

Section: Long-period Comets and Their Dust Trailsmentioning

confidence: 99%

An unusual meteor shower on 1 September 2007

Jenniskens¹,

Vaubaillon²

2007

EoS Transactions

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Around 83 B.C., give or take a century, comet Kiess (C/1911 N1) passed by the Sun, ejecting a cloud of dust particles. The comet returned in 1911, after completing one orbit. The dust particles were pushed by solar radiation pressure into slightly wider orbits and have been returning ever since, forming a thin ongoing stream of dust that usually passes just outside Earth's orbit. On occasion, the combined gravity of the solar system's planets moves this dust trail into Earth's path. Earth encountered this 2000‐year‐old dust in 1935, 1986, and 1994, causing a meteor shower known as the Aurigids.

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The Detection of a Dust Trail in the Orbit of an Earth‐threatening Long‐Period Comet

Cited by 49 publications

References 15 publications

Properties of meteoroids from different classes of parent bodies

Properties of meteoroids from different classes of parent bodies

The meteor-shower complex of 96P/Machholz revisited

An unusual meteor shower on 1 September 2007

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