The Core of the Meteor Stream Associated with Comet Halley

Hajduk, A.

doi:10.1017/s0074180900066651

Cited by 7 publications

(19 citation statements)

References 8 publications

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“…Svoreň & Kaňuchová (2017)'s recent analysis of a very similar data set identified two maxima of photographic Orionid activity at L = 208.5 • and L = 210.5 • , in good agreement with Stohl & Porubcan (1981) and Porubcan & Zvolankova (1984)'s results. A central dip was noticed close to the main peak of activity, as previously noted by McIntosh & Hajduk (1983) and Lindblad & Porubcan (1999) for the Orionids, and by Hajduk (1980) for the η-Aquariids.…”

Section: Average Activity Profilesupporting

confidence: 83%

“…Since the time of those earlier works, the location of the Orionids and η-Aquariids main peak of activity has been reexamined by several authors (e.g., McIntosh & Hajduk 1983;Hajduk 1980;Hajduk et al 1984;Cevolani & Hajduk 1985Koschack & Roggemans 1991). Covering periods of 5-10 yr, displacements in solar longitude of 0.3-0.75 degrees per year and 0.42-0.92 degrees per year have been claimed for the η-Aquariids and Orionids respectively (McIntosh & Hajduk 1983).…”

Section: Peak Locationmentioning

confidence: 99%

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Activity of the Eta-Aquariid and Orionid meteor showers

Egal

Brown

Rendtel

et al. 2020

A&A

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Aims. We present a multi-instrumental, multidecadal analysis of the activity of the Eta-Aquariid and Orionid meteor showers for the purpose of constraining models of 1P/Halley’s meteoroid streams. Methods. The interannual variability of the showers’ peak activity and period of duration is investigated through the compilation of published visual and radar observations prior to 1985 and more recent measurements reported in the International Meteor Organization (IMO) Visual Meteor DataBase, by the IMO Video Meteor Network and by the Canadian Meteor Orbit Radar (CMOR). These techniques probe the range of meteoroid masses from submilligrams to grams. The η-Aquariids and Orionids activity duration, shape, maximum zenithal hourly rates values, and the solar longitude of annual peaks since 1985 are analyzed. When available, annual activity profiles recorded by each detection network were measured and are compared. Results. Observations from the three detection methods show generally good agreement in the showers’ shape, activity levels, and annual intensity variations. Both showers display several activity peaks of variable location and strength with time. The η-Aquariids are usually two to three times stronger than the Orionids, but the two showers display occasional outbursts with peaks two to four times their usual activity level. CMOR observations since 2002 seem to support the existence of an ~12 yr cycle in Orionids activity variations; however, additional and longer term radar and optical observations of the shower are required to confirm such periodicity.

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Section: Average Activity Profilesupporting

confidence: 83%

Section: Peak Locationmentioning

confidence: 99%

Activity of the Eta-Aquariid and Orionid meteor showers

Egal

Brown

Rendtel

et al. 2020

A&A

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“…The very consistent Perseid shower is known to have an unusually dense core in an otherwise diffuse stream (Kaiser et al 1966, Lindblad 1986, Simek and Mcintosh 1986. The Orionid and r\ Aquarid showers exhibit a double peak in bright meteors and up to five peaks in fainter radar meteors (Stohl and Porubcan 1978, Hajduk 1980, Cevolani and Hajduk 1987. Quadrantid shower rates vary from year to year (Mcintosh and Simek 1984).…”

Section: Jrate Profilesmentioning

confidence: 99%

Debris from Comets: The Evolution of Meteor Streams

McIntosh¹

1989

International Astronomical Union Colloquium

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The evolution of meteor streams is controlled basically by: (a) the initial velocities with which the particles were ejected from the parent body; (b) gravitational perturbations by the planets; (c) radiation forces; and (d) collisions. This review focuses mainly on recent numerical modelling dealing with (b) and (a).Ejection velocities spread the particles around the orbit, closing the ring in a few tens of revolutions. The greater ejection velocities of smaller particles cause more rapid dispersion both around the orbit and in the cross section.A determination of the effects of gravitational perturbations must take into account the distributed properties of the stream. The stream’s evolution is dependent on the short-term impulse nature of planetary perturbations, as well as on long-term secular effects. The combined effects produce complex stream cross-sections as in the ribbon-like form of the Halley stream (Orionid and η Aquarid showers) or as in the changes in the annual position of peak shower activity shown by the Quadrantids. Perturbations may cause the orbit of a parent body to sweep rapidly across the orbit of the Earth. But the associated particle stream may not be lost as a meteor shower because it tends to become dispersed in a manner that ensures a continuing supply of particles in Earth-crossing orbits. The nodes of the observed meteoroid orbits may show very little motion compared with the rapid motion of the nodes of the orbit of the parent object.Radiation effects contribute to size separation of particles. Very small particles are blown out of the stream or spiral in toward the sun because of Poynting–Robertson drag. Older meteor streams usually show a predominance of large particles.

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“…However, almost no modeling effort had been made to explain the annual activity variations of the Orionids and η-Aquariids noticed by Hajduk (1970) and Hajduk (1973), until the observation of the recent Orionids outbursts. By investigating the role of resonances highlighted in previous works, numerical simulations of Sekhar and Asher (2014) successfully reproduced the apparition dates of recent and ancient Orionids outbursts, and predicted a future outburst of the shower in 2070.…”

Section: Introductionmentioning

confidence: 99%

Activity of the Eta-Aquariid and Orionid meteor showers

Egal,

Brown,

Rendtel

et al. 2020

Preprint

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Aims. We present a multi-instrumental, multidecadal analysis of the activity of the Eta-Aquariid and Orionid meteor showers for the purpose of constraining models of 1P/Halley's meteoroid streams. Methods. The interannual variability of the showers' peak activity and period of duration is investigated through the compilation of published visual and radar observations prior to 1985 and more recent measurements reported in the International Meteor Organization (IMO) Visual Meteor DataBase, by the IMO Video Meteor Network and by the Canadian Meteor Orbit Radar (CMOR). These techniques probe the range of meteoroid masses from submilligrams to grams. The η-Aquariids and Orionids activity duration, shape, maximum zenithal hourly rates (ZHR) values, and the solar longitude of annual peaks since 1985 are analyzed. When available, annual activity profiles recorded by each detection network were measured and are compared. Results. Observations from the three detection methods show generally good agreement in the showers' shape, activity levels, and annual intensity variations. Both showers display several activity peaks of variable location and strength with time. The η-Aquariids are usually two to three times stronger than the Orionids, but the two showers display occasional outbursts with peaks two to four times their usual activity level. CMOR observations since 2002 seem to support the existence of an ∼12 year cycle in Orionids activity variations; however, additional and longer term radar and optical observations of the shower are required to confirm such periodicity.

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The Core of the Meteor Stream Associated with Comet Halley

Cited by 7 publications

References 8 publications

Activity of the Eta-Aquariid and Orionid meteor showers

Activity of the Eta-Aquariid and Orionid meteor showers

Debris from Comets: The Evolution of Meteor Streams

Activity of the Eta-Aquariid and Orionid meteor showers

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