On the dynamics of meteoroid streams

Jenniskens, Peter

doi:10.1186/bf03352149

Cited by 43 publications

(24 citation statements)

References 50 publications

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“…Such models can not account for the observed dispersion. If the radiant dispersion is due to ejection velocities only, then the typical ejection velocity should be -100 d s , which is much larger than typically a s s u m e d -o n the order of 1-10 m/s for the relevant mass range (Jenniskens, 1998). It is possible that the observed narrow peak is due t o relatively old ejecta, because Earth did not pass close to debris trails ejected in recent returns.…”

Section: Discussionmentioning

confidence: 99%

“…Ground stations were set up in the Peoples Republic of China at locations +I and +2 time zones west from Leonid MAC at Okinawa, Japan (for a map, see Jenniskens and Butow, 1999). During a storm, it is possible to measure the orbits and debris distribution of relatively recent cometary ejecta at an unprecedented precision for addressing outstanding questions in meteor physics and meteoroid stream dynamics (Ceplecha et al, 1998;Jenniskens, 1998). The purpose of the ground campaign was to measure the meteor flux and to measure precise meteor trajectories and orbits of relatively bright meteors.…”

Section: Introductionmentioning

confidence: 99%

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Very precise orbits of 1998 Leonid meteors

Betlem¹,

Jenniskens²,

Leven³

et al. 1999

Meteorit & Planetary Scien

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Abstract-Seventy-five orbits of Leonid meteors obtained during the 1998 outburst are presented. Thirtyeight are precise enough to recognize significant dispersion in orbital elements. Results from the nights of 1998 November 16/17 and 17/18 differ, in agreement with the dominant presence of different dust components. The shower rate profile of 1998 November 16/17 was dominated by a broad component, rich in bright meteors. The radiant distribution is compact. The semimajor axis is conjined to values close to that of the parent comet, whereas the distribution of inclination has a central condensation in a narrow range. On the other hand, 1998 November 17/18 was dominated by dust responsible for a more narrow secondary peak in the flux curve. The declination of the radiant and the inclination of the orbit are more widely dispersed. The argument of perihelion, inclination, and the perihelion distance are displaced. These data substantiate the hypothesis that trapping in orbital resonances is important for the dynamical evolution of the broad component.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Very precise orbits of 1998 Leonid meteors

Betlem¹,

Jenniskens²,

Leven³

et al. 1999

Meteorit & Planetary Scien

View full text Add to dashboard Cite

show abstract

“…These counts are scaled to the zenith hourly rates calculated from visual observations in The Netherlands (•, left), and similar observations in Japan, calculated by Masaaki Takanashi of the Nippon Meteor Society (NMS electronic circular, Dec. 2000). Radio meteorscatter observations were provided by five stations of the Global Meteor Scatter Network (Jenniskens 1998b). Ten-minute counts were obtained by Esko Lyytinen and Ilkka Yrjölä in Finland, Hiroshi Ogawa and Kazuhiro Suzuki in Japan, and Pierre de Groote in Belgium.…”

Section: Ursid Activitymentioning

confidence: 99%

Dust Trails of 8P/Tuttle and the Unusual Outbursts of the Ursid Shower

Jenniskens¹,

Lyytinen²,

Lignie

et al. 2002

Icarus

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We calculate the position of dust trails from comet 8P/Tuttle, in an effort to explain unusual Ursid meteor shower outbursts that were seen when the comet was near aphelion. Comet 8P/Tuttle is a Halley-type comet in a 13.6-year orbit, passing just outside of Earth's orbit. We find that the meteoroids tend to be trapped in the 12:14 mean motion resonance with Jupiter, while the comet librates in a slightly shorter period orbit around the 13:15 resonance. It takes 6 centuries to decrease the perihelion of the meteoroid orbits enough to intersect Earth's orbit, during which time the meteoroids and comet separate in mean anomaly by 6 years, thus explaining the 6-year lag between the comet's return and Ursid outbursts. The resonances also prevent dispersion along the comet orbit and limit viewing to only one year in each return. We identified past dust trail encounters with dust trails from 1392 (Dec. 1945) and 1378 (Dec. 1986) and predicted another outburst on 2000 December 22 at around 7:29 and 8:35 UT, respectively, from dust trails dating to the 1405 and 1392 returns. This event was observed from California using video and photographic techniques. At the same time, five Global-MS-Net stations in Finland, Japan, and Belgium counted meteors using forward meteor scatter. The outburst peaked at 8:06 ± 07 UT, December 22, at zenith hourly rate ∼90 per hour, and the Ursid rates were above half peak intensity during 4.

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“…In 1983, the InfraRed Astronomical Satellite IRAS detected thermal emission of comet dust trails in the orbit of short-period comets (Davies et al 1984, Sykes et al 1986, 1990. In recent years, it has become clear that Earth-threatening long-period comets with orbital periods of order 200 to 10,000 years can have associated dust trail too, which betray the comet's presence by causing short-lived outbursts of meteors (Kresák 1993, Jenniskens 1995, but only when that trail of dust is directed in Earth's path by planetary perturbations (Lewin 1961, Jenniskens 1998). …”

Section: Introductionmentioning

confidence: 99%

Meteor outbursts from long-period comet dust trails

Lyytinen¹

2003

Icarus

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Long-period comets have narrow 1-revolution old dust trails that can cause meteor outbursts when encountered by Earth. To facilitate observing campaigns that will characterise and perhaps help find Earth threatening long-period comets from their trace of meteoric debris, we use past accounts of outbursts from 14 different showers to calculate the future dust trail positions near Earth orbit. We also examine known near-Earth long-period comets and identify six potential new showers, which can be utilised to learn more about these objects. We demonstrate that it is the 1-revolution trail that is responsible for meteor outbursts. A method is presented that calculates in what year these showers are likely to return and at what hour. The calculations improve on earlier approximate methods that used the Sun's reflex motion to gauge the trail motion relative to Earth's orbit.

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On the dynamics of meteoroid streams

Cited by 43 publications

References 50 publications

Very precise orbits of 1998 Leonid meteors

Very precise orbits of 1998 Leonid meteors

Dust Trails of 8P/Tuttle and the Unusual Outbursts of the Ursid Shower

Meteor outbursts from long-period comet dust trails

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