Plasma and electromagnetic wave simulations of meteors

Dyrud, L. P.; Wilson, Derek; Boerve, Steiner; Trulsen, J.; Pécseli, H. L.; Close, Sigrid; Chen, Chen; Lee, Yoon Jae

doi:10.1016/j.asr.2007.03.048

Cited by 24 publications

(25 citation statements)

References 16 publications

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“…Kero et al (2008b) have shown that the RCSs measured simultaneously at the three receivers are equivalent and that the targets have similar properties at aspect angles all the way out to 130 • from the direction of propagation of a meteoroid. This suggests that the head echo target is essentially spherical in the forward direction, consistent with the polarization measurements by Close et al (2002) and the plasma and electromagnetic simulations of meteor head echoes performed by Dyrud et al (2007).…”

Section: Resultssupporting

confidence: 72%

“…This suggests that the head echo target is essentially spherical in the forward direction, consistent with the polarization measurements by Close et al (2002) and the plasma and electromagnetic simulations of meteor head echoes performed by Dyrud et al (2007).…”

Section: Meteoroid Mass Estimationsupporting

confidence: 72%

“…Here we focus on the tristatic radar measurement technique and suffice it to say that the data could be employed together with any kind of physical model describing the atmosphere interaction processes, e.g., the ablation model described by Campbell-Brown and Koschny (2004), the analytical scattering model by Close et al (2004), or the numerical simulations by Dyrud et al (2007).…”

Section: Meteoroid Mass Estimationmentioning

confidence: 99%

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Determination of meteoroid physical properties from tristatic radar observations

et al. 2008

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Abstract. In this work we give a review of the meteor head echo observations carried out with the tristatic 930 MHz EISCAT UHF radar system during four 24 h runs between 2002 and 2005 and compare these with earlier observations. A total number of 410 tristatic meteors were observed. We describe a method to determine the position of a compact radar target in the common volume monitored by the three receivers and demonstrate its applicability for meteor studies. The inferred positions of the meteor targets have been utilized to estimate their velocities, decelerations and directions of arrival as well as their radar cross sections with unprecedented accuracy. The velocity distribution of the meteoroids is bimodal with peaks at 35-40 km/s and 55-60 km/s, and ranges from 19-70 km/s. The estimated masses are between 10 −9 -10 −5.5 kg. There are very few detections below 30 km/s. The observations are clearly biased to high-velocity meteoroids, but not so biased against slow meteoroids as has been presumed from previous tristatic measurements. Finally, we discuss how the radial deceleration observed with a monostatic radar depends on the meteoroid velocity and the angle between the trajectory and the beam. The finite beamwidth leads to underestimated meteoroid masses if radial velocity and deceleration of meteoroids approaching the radar are used as estimates of the true quantities in a momentum equation of motion.

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Section: Resultssupporting

confidence: 72%

Section: Meteoroid Mass Estimationsupporting

confidence: 72%

Section: Meteoroid Mass Estimationmentioning

confidence: 99%

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Determination of meteoroid physical properties from tristatic radar observations

et al. 2008

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“…They are based on studies of dust and meteoroids outside of the atmosphere (Hughes 1978;Grün et al 1985; Love and Brownlee 1993; and others), on atmospheric studies, as well as on studies of the deposition of extraterrestrial matter in glaciers and sediments (see Kane Gabrielli et al 2004; and others). Aside from the differences between the different observation methods, the uncertainties, as pointed out by Dyrud et al (2008), arise from the characteristics of different radar meteor observation techniques.…”

Section: Dust Flux In the Solar Wind And Into Earth Atmospherementioning

confidence: 99%

Dusty Plasma Effects in Near Earth Space and Interplanetary Medium

et al. 2011

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Dusty plasma effects in near earth space and interplanetary mediumSpace Science Reviews, 2011, Vol. 161, Issue 1-4: 1-47 10.1007/s11214-011-9762-3Access to the published version may require subscription. Published with permission from:Springer Science+Business Media B.V.Space Science Reviews manuscript No. (will be inserted by the editor) Dusty plasma effects in near Earth space and interplanetary mediumReceived: date / Accepted: date Abstract We review dust and meteoroid fluxes and their dusty plasma effects in the interplanetary medium near Earth orbit and in the Earth's ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the interplanetary medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process, as well as of the dust charging processes. The latter are also important for further studying nano dust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nano dust fluxes is still a challenge.

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“…For underdense trails the effect maximises as the plasma dielectric on the trail axis goes through ε pl ≈ −1.4 (Kaiser and Closs, 1952). The resonance will be observable as long as the trail plasma is Dyrud et al (2007) by permission. The meteor simulated here was moving against the surrounding atmosphere at 40 km s −1 , i.e.…”

Section: The Outliers -Polarized Echoesmentioning

confidence: 99%

Meteor head echo polarization at 930 MHz studied with the EISCAT UHF HPLA radar

2011

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Abstract. The polarization characteristics of 930-MHz meteor head echoes have been studied for the first time, using data obtained in a series of radar measurements carried out with the tristatic EISCAT UHF high power, large aperture (HPLA) radar system in October 2009. An analysis of 44 tri-static head echo events shows that the polarization of the echo signal recorded by the Kiruna receiver often fluctuates strongly on time scales of tens of microseconds, illustrating that the scattering process is essentially stochastic. On longer timescales (> milliseconds), more than 90 % of the recorded events show an average polarization signature that is independent of meteor direction of arrival and echo strength and equal to that of an incoherent-scatter return from underdense plasma filling the tristatic observation volume. This shows that the head echo plasma targets scatter isotropically, which in turn implies that they are much smaller than the 33-cm wavelength and close to spherically symmetric, in very good agreement with results from a previous EISCAT UHF study of the head echo RCS/meteor angle-of-incidence relationship.Significant polarization is present in only three events with unique target trajectories. These all show a larger effective target cross section transverse to the trajectory than parallel to it. We propose that the observed polarization may be a signature of a transverse charge separation plasma resonance in the region immediately behind the meteor head, similar to the resonance effects previously discussed in connection with meteor trail echoes by Herlofson, Billam and Browne, Jones and Jones and others.

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Plasma and electromagnetic wave simulations of meteors

Cited by 24 publications

References 16 publications

Determination of meteoroid physical properties from tristatic radar observations

Determination of meteoroid physical properties from tristatic radar observations

Dusty Plasma Effects in Near Earth Space and Interplanetary Medium

Meteor head echo polarization at 930 MHz studied with the EISCAT UHF HPLA radar

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