Leonids 2006 observations of the tail of trails: Where is the comet fluff?

Jenniskens, Peter; Kleer, K. de; Vaubaillon, Jérémie; Trigo-Rodríguez, J. M.; Madiedo, J. M.; Haas, Roland; Kuile, Casper R. Ter; Miskotte, Koen; Vandeputte, Michel; Johannink, Carl; Bus, Peter; Leven, J. van 't; Jobse, Klaas; Koop, M.

doi:10.1016/j.icarus.2008.02.026

Cited by 8 publications

(7 citation statements)

References 25 publications

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“…Lyytinen & Van Flandern 2000;. This activity was really observed with the peak occurring within 10 min of the predicted time (Jenniskens et al 2008;Koten et al 2008).…”

Section: Introductionmentioning

confidence: 75%

Activity of the Leonid meteor shower on 2009 November 17

Koten

Borovička

Кохирова

2011

A&A

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“…Lyytinen & Van Flandern 2000;. This activity was really observed with the peak occurring within 10 min of the predicted time (Jenniskens et al 2008;Koten et al 2008).…”

Section: Introductionmentioning

confidence: 75%

Activity of the Leonid meteor shower on 2009 November 17

Koten

Borovička

Кохирова

2011

A&A

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“…Further modelling to account for the deceleration of a meteoroid in the Earth's atmosphere, will need to be performed when observing meteors with low entry velocities. Inferences on the meteoroid material and parent body can be made by studying the light curves of the stream meteors (Koten et al 2004;Jenniskens et al 2008;Subasinghe et al 2016). These topics are reserved for a future study.…”

Section: Discussionmentioning

confidence: 99%

Characterisation of the Perseid meteoroid stream through SPOSH observations between 2010–2016

Margonis

Christou

Oberst

2019

A&A

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We have characterised the Perseid meteoroid stream from data acquired in a series of observing campaigns between 2010 and 2016. The data presented in this work were obtained by the Smart Panoramic Optical Sensor Head (SPOSH), an all-sky camera system designed to image faint transient noctilucent phenomena on dark planetary hemispheres. For the data reduction, a sophisticated software package was developed that utilises the high geometric and photometric quality of images obtained by the camera system. We identify 934 meteors as Perseids, observed over a long period between late July (∼124 • ) and mid-to-late August (∼147 • ). The maximum meteor activity contributing to the annual shower was found at λ = 140. • 08 ± 0. • 07. The radiant of the shower was estimated at RA = 47. • 2 and Dec = 57. • 5 with a median error of 0. • 6 and 0. • 2, respectively. The mean population index of the shower between solar longitudes of 120. • 68 and 145. • 19 was r = 2.36 ± 0.05, showing strong temporal variation. A predicted outburst in shower activity for the night of August 11-12, 2016 was confirmed, with a peak observed 12.75 hr before the annual maximum at 23:30 ± 15 UT. We measure a peak flux of 6.1 × 10 −4 km −2 hr −1 for meteoroids of mass 1.6 × 10 −2 g or more, appearing in the time period between 23:00 and 00:00 UT. We estimate the measured flux of the outburst meteoroids to be approximately twice as high as the annual meteoroid flux of the same mass. The population index of r = 2.19 ± 0.08, computed from the outburst Perseids in 2016, is higher than the value of r = 1.92 ± 0.06 derived from meteors observed in 2015 belonging to the annual Perseid shower which was active near the time of the outburst. A dust trail with an unusually high population index of r = 3.58 ± 0.24 was encountered in 2013 between solar longitudes 136. • 261 and 137. • 442. The relatively high r-value implies an encounter with a dust trail rich in low-mass particles.

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“…The annual Leonid shower was expected to peak approximately at the same time but with much lower activity. Figure 2 shows the radiant positions of Leonids observed that night together with the predicted radiants for the 1466 and 1533 trails (Vaubaillon et al 2009), the radiant of the annual shower according to various authors, and the so-called filament circle along which the radiants were spread during 2006 Leonids (Jenniskens et al 2008). The error of the radiants of two Leonids (D and F) is too large to judge their origin.…”

Section: Radiants and Heliocentric Orbits Of Fireballsmentioning

confidence: 98%

Observations of the 2009 Leonid activity by the Tajikistan fireball network

Кохирова

Borovička

2011

A&A

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The fireball network in Tajikistan operates since 2009. Observations of the 2009 Leonid activity were carried out on November 13−21. In this period 16 Leonid fireballs were photographed. As a result of astrometric and photometric reductions, the precise data including atmospheric trajectories, velocities, orbits, light curves, and photometric masses were determined for ten fireballs. Low-resolution video spectra were obtained for six fireballs.The radiant positions during the maximum night suggest that the majority of the fireball activity was caused by the annual stream component with only minor contribution of the 1466 trail. According to their end heights, nearly half of Leonid fireballs belonged to the most fragile and weak fireball group IIIB and the rest to the slightly more dense cometary group IIIA. However, one detected Leonid belonged to the fireball group I. This is the first detection of an anomalously strong Leonid individual. Its chemical composition was not markedly different from other Leonids.

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Leonids 2006 observations of the tail of trails: Where is the comet fluff?

Cited by 8 publications

References 25 publications

Activity of the Leonid meteor shower on 2009 November 17

Activity of the Leonid meteor shower on 2009 November 17

Characterisation of the Perseid meteoroid stream through SPOSH observations between 2010–2016

Observations of the 2009 Leonid activity by the Tajikistan fireball network

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