5. Meteoroid Populations and Orbits

Ceplecha, Z.

doi:10.1017/s0252921100070044

Cited by 25 publications

(35 citation statements)

References 8 publications

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“…He associated group A with ordinary chondrite material, group B with carbonaceous chondrites, group C with dense and regular cometary material, and D with weak cometary meteoroids (Ceplecha 1988). Later, Ceplecha (1988) group, Asteroidal, to the four mentioned here, for meteoroids with K B ≥ 8.…”

Section: Comparison Using the K B Parametermentioning

confidence: 78%

“…Later, Ceplecha (1988) group, Asteroidal, to the four mentioned here, for meteoroids with K B ≥ 8. He also divided group C into three subgroups based on orbital elements, but due to our small number statistics, we treat these as one.…”

Section: Comparison Using the K B Parametermentioning

confidence: 92%

“…Meteor beginning height has been used in past work as a measure of the strength of meteoroids in the millimeter size range (see Ceplecha 1958Ceplecha , 1967Ceplecha , 1968Ceplecha , 1988Borovicka et al 2005). For two meteoroids having the same pre-atmospheric velocity, a stronger/denser meteoroid will start to ablate at a lower height than a weaker/low density meteroid.…”

Section: Meteoroid Strength and Densitymentioning

confidence: 99%

“…Ceplecha (1988) K B parameter to separate meteoroids in the mm to cm-size range into four populations:…”

Section: Comparison Using the K B Parametermentioning

confidence: 99%

“…He also divided group C into three subgroups based on orbital elements, but due to our small number statistics, we treat these as one. Equation (5) was developed and first applied to meteors photographed by Super-Schmidt cameras (see Ceplecha 1967Ceplecha , 1988Bellot Rubio et al 2002). For the fainter meteors observed by intensified video systems, the parameter K B is calculated in the same way, but an offset of 0.15 is added (see Ceplecha 1988) because the K B criterion is based on meteor beginning heights, which depend on the sensitivity of the camera.…”

Section: Comparison Using the K B Parametermentioning

confidence: 99%

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Bulk density of small meteoroids

Kikwaya

Campbell-Brown

Brown

2011

A&A

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Aims. Here we report on precise metric and photometric observations of 107 optical meteors, which were simultaneously recorded at multiple stations using three different intensified video camera systems. The purpose is to estimate bulk meteoroid density, link small meteoroids to their parent bodies based on dynamical and physical density values expected for different small body populations, to better understand and explain the dynamical evolution of meteoroids after release from their parent bodies. Methods. The video systems used had image sizes ranging from 640 × 480 to 1360 × 1036 pixels, with pixel scales from 0.01 • per pixel to 0.05 • per pixel, and limiting meteor magnitudes ranging from M v = +2.5 to +6.0. We find that 78% of our sample show noticeable deceleration, allowing more robust constraints to be placed on density estimates. The density of each meteoroid is estimated by simultaneously fitting the observed deceleration and lightcurve using a model based on thermal fragmentation, conservation of energy and momentum. The entire phase space of the model free parameters is explored for each event to find ranges of parameters which fit the observations within the measurement uncertainty. Results. (a) We have analysed our data by first associating each of our events with one of the five meteoroid classes. The average density of meteoroids whose orbits are asteroidal and chondritic (AC) is 4200 kg m −3 suggesting an asteroidal parentage, possibly related to the high-iron content population. Meteoroids with orbits belonging to Jupiter family comets (JFCs) have an average density of 3100 ± 300 kg m −3 . This high density is found for all meteoroids with JFC-like orbits and supports the notion that the refractory material reported from the Stardust measurements of 81P/Wild 2 dust is common among the broader JFC population. This high density is also the average bulk density for the 4 meteoroids with orbits belonging to the Ecliptic shower-type class (ES) also related to JFCs. Both categories we suggest are chondritic based on their high bulk density. Meteoroids of HT (Halley type) orbits have a minimum bulk density value of 360 +400 −100 kg m −3 and a maximum value of 1510 +400 −900 kg m −3 . This is consistent with many previous works which suggest bulk cometary meteoroid density is low. SA (Sun-approaching)-type meteoroids show a density spread from 1000 kg m −3 to 4000 kg m −3 , reflecting multiple origins. (b) We found two different meteor showers in our sample: Perseids (10 meteoroids, ∼11% of our sample) with an average bulk density of 620 kg m −3 and Northern Iota Aquariids (4 meteoroids) with an average bulk density of 3200 kg m −3 , consistent with the notion that the NIA derive from 2P/Encke.

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Section: Comparison Using the K B Parametermentioning

confidence: 78%

Section: Comparison Using the K B Parametermentioning

confidence: 92%

Section: Meteoroid Strength and Densitymentioning

confidence: 99%

“…Ceplecha (1988) K B parameter to separate meteoroids in the mm to cm-size range into four populations:…”

Section: Comparison Using the K B Parametermentioning

confidence: 99%