Optical observations of enhanced activity  of the 2005 Draconid meteor shower

Koten, Pavel; Borovička, J.; Spurný, Pavel; Štork, R.

doi:10.1051/0004-6361:20066838

Cited by 24 publications

(11 citation statements)

References 11 publications

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“…Photographic (Jacchia et al ) and also more recent video (Suzuki et al ; Fujiwara et al ; Koten et al ) observations during previous Draconid outbursts have revealed that the Draconid beginning heights are significantly higher than those of other established meteor showers and that of an average sporadic meteor. An explanation suggested by Jacchia et al () is that Draconid meteoroids might be composed of soft materials and therefore more easily melt or vaporize, perhaps due to the recent dust release from the parent comet.…”

Section: Discussionmentioning

confidence: 96%

“…High Draconid detection altitudes have previously been found, e.g. among photographic (Jacchia, Kopal & Millman ) and video meteors (Suzuki et al ; Fujiwara et al ; Koten et al ).…”

Section: Introductionmentioning

confidence: 90%

“…Nevertheless, the good agreement with the predictions, as well as with reported video observations (Vaubaillon et al ), shows that the small (radar‐sized) MU Draconids and larger meteoroids had similar orbital characteristics. The mean radiant region of small (radar‐sized) particles of the 2005 Draconid outburst observed with the Canadian Meteor Orbit Radar (CMOR) reported by Campbell‐Brown et al () differed from the modelled and the optical (video and photographic) radiant with α = 1° and δ = 6° (Koten et al ).…”

Section: The 2011 Draconid Radiantmentioning

confidence: 99%

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MU radar head echo observations of the 2011 October Draconids

Kero

Fujiwara²,

Abo

et al. 2012

Monthly Notices of the Royal Astronomical Society

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On 2011 October 8, the Earth passed through a stream of dust ejected by the comet 21P/Giacobini–Zinner during its perihelion passage of the year 1900, causing an outburst of October Draconid meteors. 13 Draconids were observed among ∼6300 meteor head echoes with precisely determined orbits during an observational campaign ranging from October 8 05:00 ut to October 9 13:00 ut with the Shigaraki middle and upper atmosphere (MU) radar in Japan (34°.85 N and 136°.10 E). The meteor outburst occurred while the Draconid radiant was descending below and 2 h later rising up above the horizon. Therefore, 11 of the detections were from very low (<15°) elevation. The detection altitudes of the Draconids were high compared to sporadic meteors of the same velocity and radiant elevation. The weighted mean geocentric velocity of the 13 Draconids was 20.6 ± 0.4 km s−1, and the weighted mean radiant located at right ascension α = 263°.3 ± 0°.6 and declination δ = 55°.8 ± 0°.2.

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Section: Discussionmentioning

confidence: 96%

“…High Draconid detection altitudes have previously been found, e.g. among photographic (Jacchia, Kopal & Millman ) and video meteors (Suzuki et al ; Fujiwara et al ; Koten et al ).…”

Section: Introductionmentioning

confidence: 90%

Section: The 2011 Draconid Radiantmentioning

confidence: 99%

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MU radar head echo observations of the 2011 October Draconids

Kero

Fujiwara²,

Abo

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Our 2005 Draconid data were already presented in Koten et al (2007, hereafter referred to as Paper I), where we reported meteor frequencies, trajectories, radiants, orbits, masses, beginning and end heights, and light curves. The light curves were described in the classic statistical way, based on the position of the maximum.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric deceleration and light curves of Draconid meteors and implications for the structure of cometary dust

Borovička

Spurný

Koten

2007

A&A

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118

124

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Aims. The observation of Draconid meteors was used to infer information on the structure, porosity, strength, and composition of the dust of comet 21P/Giacobini-Zinner. Methods. Stereoscopic video and photographic observations of six faint and one bright Draconid meteors provided meteor morphologies, heights, light curves, and atmospheric decelerations. The spectrum of the bright meteor was also obtained. We developed a simple model of meteoroid ablation and fragmentation. The model assumes that cometary meteoroids are composed of constituent grains.Results. By fitting the observed decelerations and light curves, we have found that the grain mass range was relatively narrow in all meteoroids but differed from case to case. Some meteoroids were coarse grained with grain masses 10 −9 to 10 −10 kg, others were fine grained with grain masses one order of magnitude lower. Individual mm-sized meteoroids contained tens of thousands to almost a million grains (assuming grain density close to 3000 kg m −3 ). The meteoroids were porous aggregates of grains, having porosities of about 90% and bulk densities of 300 kg m −3 . Grain separation started after the surface of the meteoroid received energy of 10 6 J m −2 . The separation continued during the first half of meteor trajectories. We call this phase erosion. The energy needed for grain erosion was 15−30× lower than the energy of vaporization. However, 30% of the largest meteoroid was resistant to thermal erosion; this part disrupted later mechanically under a very low dynamic pressure of 5 kPa. The relative abundances of Na, Mg, and Fe were nearly chondritic, but differential ablation caused preferential loss of sodium at the beginning of the trajectory.

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“…The most important papers based on the video observations: (i) properties of the Perseid, Orionid, Leonid, Geminid and Taurid meteor showers [3], (ii) survey of meteor spectra and orbits [4], (iii) quadrantid meteor shower and implications for its parent body [5], (iv) radiation of the meteors above 130 km [6], (v) draconid meteor shower [7,8].…”

Section: Resultsmentioning

confidence: 99%

Double‐Station Automatic Video Observation of the Meteors

Vítek

Koten

Páta

et al. 2010

Advances in Astronomy

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The double station observation of the meteors by means of sensitive image intensifier technique started at the Ondrejov Observatory 10 years ago. The sensitivity of such instrumentation allows detection of the meteors down to masses of fractions of gram. Moreover, video technique provides us with a time resolution of the meteor events. On the other side, the precision of the video data is lower in comparison with the photographic data. We are introducing technological progress on the project—replacing of the S-VHS camcorders with gigabite, ethernet cameras and making the whole process of video observation automatic.

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Optical observations of enhanced activity of the 2005 Draconid meteor shower

Cited by 24 publications

References 11 publications

MU radar head echo observations of the 2011 October Draconids

MU radar head echo observations of the 2011 October Draconids

Atmospheric deceleration and light curves of Draconid meteors and implications for the structure of cometary dust

Double‐Station Automatic Video Observation of the Meteors

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