Modeling the meteor head echo using Arecibo radar observations

Dyrud, L. P.; Janches, Diego

doi:10.1016/j.jastp.2008.06.016

Cited by 35 publications

(50 citation statements)

References 35 publications

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“…These characteristic meteoroid parameters were chosen because this is a commonly measured size class of meteoroids among the billions of daily meteors ; Dyrud and Janches, 2008). The meteor simulation of the type shown in Fig.…”

Section: Global Model Resultsmentioning

confidence: 99%

“…This figure displays the head echo trace as a diagonal colored line, with color corresponding to the trail electron line density per meter divided by 10 6 , such that it may appear on the same color bar as the FBGD growth rate shown in the non-specular trail portion of the RTI plot that appears after the head-echo. We have developed numerous head echo models (see Dyrud and Janches, 2008) and have opted to plot a parameter which is related to head echo strength, but is also of direct physical relevance to the development of plasma instability in the trail. To the right of the head echo, this plot displays the calculated, non-negative, FBGD growth rate as a function of time and altitude for a diffusing meteor column.…”

Section: Model Descriptionmentioning

confidence: 99%

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Global variation of meteor trail plasma turbulence

et al. 2011

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Abstract. We present the first global simulations on the occurrence of meteor trail plasma irregularities. These results seek to answer the following questions: when a meteoroid disintegrates in the atmosphere, will the resulting trail become plasma turbulent? What are the factors influencing the development of turbulence? and how do these trails vary on a global scale? Understanding meteor trail plasma turbulence is important because turbulent meteor trails are visible as non-specular trails to coherent radars. Turbulence also influences the evolution of specular radar meteor trails; this fact is important for the inference of mesospheric temperatures from the trail diffusion rates, and their usage for meteor burst communication. We provide evidence of the significant effect that neutral atmospheric winds and ionospheric plasma density have on the variability of meteor trail evolution and on the observation of non-specular meteor trails. We demonstrate that trails are far less likely to become and remain turbulent in daylight, explaining several observational trends for non-specular and specular meteor trails.

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Section: Global Model Resultsmentioning

confidence: 99%

Section: Model Descriptionmentioning

confidence: 99%

Global variation of meteor trail plasma turbulence

et al. 2011

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“…Subsequent measurements at ALTAIR, with more dynamic mass estimates as well as scattering masses, are described by Close et al [2002cClose et al [ , 2004Close et al [ , 2005. Dynamic mass measurements together with computer model simulations are described by Bass et al [2008] and Dyrud and Janches [2008].…”

Section: Discussionmentioning

confidence: 99%

Analysis of ALTAIR 1998 meteor radar data

Zinn

Colestock

et al. 2011

J. Geophys. Res.

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[1] We describe a new analysis of a set of 32 UHF meteor radar traces recorded with the 422 MHz Advanced Research Project Agency Long-Range Tracking and Identification Radar facility in November 1998. Emphasis is on the absolute velocity measurements and inferences that can be drawn from them regarding the meteoroid masses and mass densities. We find that the 3-D velocity versus altitude data can be fitted as quadratic functions of the path integrals of the atmospheric densities versus distance, and deceleration rates derived from those fits all show the expected behavior of increasing with decreasing altitude. We also describe a computer model of the coupled processes of collisional heating, radiative cooling, evaporative cooling and ablation, and deceleration for meteoroids composed of defined mixtures of mineral constituents. For each of the cases in the data set, we ran the model starting with the measured initial velocity and trajectory inclination and with various trial values of the quantity mr s 2 (initial mass times mass density squared) and then compared the computed deceleration versus altitude curves versus the measured ones. In this way we arrived at the best fit values of the mr s 2 for each of the measured traces. Then further, assuming various trial values of the density r s , we compared the computed mass versus altitude curves with similar curves for the same set of meteoroids determined previously from the measured radar cross sections and an electrostatic scattering model. In this way we arrived at estimates of the best fit mass densities r s for each of the cases.

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“…Particles entering the atmosphere with velocities >11 km/s produce luminous trails of ionized gas that allow for the detection and characterization of individual meteors [10][11][12][13] . Radar observations of meteors are sensitive to particles with masses between 10 −9 − 10 −3 g. The interpretation of meteor observation using radar techniques is subject to a number of biases, as the ablation and ionization are functions of the particles' mass, density and incoming velocity and angle.…”

Section: A Motivation and Importancementioning

confidence: 99%

Experimental setup for the laboratory investigation of micrometeoroid ablation using a dust accelerator

Thomas

Simolka

DeLuca

et al. 2017

Review of Scientific Instruments

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A facility has been developed to simulate the ablation of micrometeoroids in laboratory conditions. An electrostatic dust accelerator is used to generate iron particles with velocities of 10-70 km/s. The particles are then introduced into a chamber pressurized with a target gas, where the pressure is adjustable between 0.01 and 0.5 Torr, and the particle partially or completely ablates over a short distance. An array of biased electrodes above and below the ablation path is used to collect the generated ions/electrons with a spatial resolution of 2.6 cm along the ablating particles’ path, thus allowing the study of the spatiotemporal evolution of the process. For completely ablated particles, the total collected charge directly yields the ionization coefficient of a given dust material-target gas combination. The first results of this facility measured the ionization coefficient of iron atoms with N2, air, CO2, and He target gases for impact velocities >20 km/s, and are reported by Thomas et al. [Geophys. Res. Lett. 43, 3645 (2016)]. The ablation chamber is also equipped with four optical ports that allow for the detection of the light emitted by the ablating particle. A multichannel photomultiplier tube system is used to observe the ablation process with a spatial and temporal resolution of 0.64 cm and 90 ns. The preliminary results indicate that it is possible to calculate the velocity of the ablating particle from the optical observations, and in conjunction with the spatially resolved charge measurements allow for experimental validation of ablation models in future studies.

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Modeling the meteor head echo using Arecibo radar observations

Cited by 35 publications

References 35 publications

Global variation of meteor trail plasma turbulence

Global variation of meteor trail plasma turbulence

Analysis of ALTAIR 1998 meteor radar data

Experimental setup for the laboratory investigation of micrometeoroid ablation using a dust accelerator

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