Seasonal variations in vertical distribution of meteor decay time as observed from meteor radars at 8.5°N and 80°N

Premkumar, B.; Reddy, K. Chenna; Yellaiah, G.; Kumar, Karanam Kishore

doi:10.1016/j.asr.2018.11.019

Cited by 4 publications

(6 citation statements)

References 49 publications

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“…Figure 7 presents statistics of meteor observations made by the EKB radar over the period from late January 2017 to August 2019. The statistics includes over 6.8 million meteor observations, or about 260 meteors per hour, which is close to the results obtained by special-purpose devices [Premkumar et al, 2019;Korotyshkin et al, 2019]. Figure 7, a shows the mean number of echo signals detected by the algorithm, depending on the local sidereal time (LST).…”

Section: Statistics Of Meteor Trail Observations With the Ekb Radarsupporting

confidence: 77%

“…Time resolution of these techniques corresponds to the ACF integration time and is typically 4-6 s [Arnold et al, 2003]. There are also algorithms that use raw IQ-components for complete cycle of detection and identification of scattering parameters [Yukimatu, Tsutsumi, 2002], or for preliminary selection of trailecho with subsequent determination of the scattering parameters from FitACF data [Parris, 2003].…”

Section: Ekb Istp Sb Ras Radarmentioning

confidence: 99%

“…To simulate a signal, we employ the well-known model [Parris, 2003] of exponential amplitude decrease and linear phase variation:…”

Section: Determination Of Scattered Signal Parametersmentioning

confidence: 99%

“…Another method of analyzing the radiant deals with aspect characteristics of the meteor trail [Lovell, 1954;Jones et al, 2005;Campbell-Brown, 2008]. According to the ratio of plasma frequency of ionized meteor trail to sounding frequency, meteor trails are generally classified as underdense and overdense [Parris, 2003], with less massive meteoroids in the former group and more massive meteoroids in the latter. There is also an intermediate type of meteor trails, usually omitted by SuperDARN radars.…”

Section: Introductionmentioning

confidence: 99%

“…Algorithms for examining scattering by meteor trails usually involve analyzing the variation of received signal power and searching for sharp peaks with an exponential decay, which is a signature of the underdense echo [Tsutsumi et al, 1999]. SuperDARN radars can detect the meteor echo both from mean correlation characteristics of the signal [Jenkins, Jarvis, 1999] and by analyzing the time dependence of amplitude of single pulse in the high sampling rate mode [Parris, 2003] or IQcomponents of the scattered signal representing a complex pulse sequence [Yukimatu, Tsutsumi, 2002].…”

Section: Introductionmentioning

confidence: 99%

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Monitoring observations of meteor echo at the EKB ISTP SB RAS radar: algorithms, validation, statistics

Fedorov

Berngardt

2021

Solar-Terrestrial Physics

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The paper considers the implementation of algorithms for automatic search for signals scattered by meteor trails according to EKB ISTP SB RAS radar data. In general, the algorithm is similar to the algorithms adopted in specialized meteor systems. The algorithm is divided into two stages: detecting a meteor echo and determining its parameters. We show that on the day of the maximum Geminid shower, December 13, 2016, the scattered signals detected by the algorithm are foreshortening and correspond to scattering by irregularities extended in the direction of the meteor shower radiant. This confirms that the source of the signals detected by the algorithm is meteor trails. We implement an additional program for indirect trail height determination. It uses a decay time of echo and the NRLMSIS-00 atmosphere model to estimate the trail height. The dataset from 2017 to 2019 is used for further testing of the algorithm. We demonstrate a correlation in calculated Doppler velocity between the new algorithm and FitACF. We present a solution of the inverse problem of reconstructing the neutral wind velocity vector from the data obtained by the weighted least squares method. We compare calculated speeds and directions of horizontal neutral winds, obtained in the three-dimensional wind model, and the HWM-14 horizontal wind model. The algorithm allows real-time scattered signal processing and has been put into continuous operation at the EKB ISTP SB RAS radar.

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Section: Statistics Of Meteor Trail Observations With the Ekb Radarsupporting

confidence: 77%

Section: Ekb Istp Sb Ras Radarmentioning

confidence: 99%

“…To simulate a signal, we employ the well-known model [Parris, 2003] of exponential amplitude decrease and linear phase variation:…”

Section: Determination Of Scattered Signal Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Monitoring observations of meteor echo at the EKB ISTP SB RAS radar: algorithms, validation, statistics

Fedorov

Berngardt

2021

Solar-Terrestrial Physics

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Latitudinal difference in meteor trail ionization heights and identification of meteor showers

Reddy

Premkumar

Yellaiah

2019

Astrophys Space Sci

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A Modeling Analysis of the Apparent Linear Relation Between Mesospheric Temperatures and Meteor Height Distributions Measured by a Meteor Radar

Lee

Kim

et al. 2022

JGR Space Physics

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A few hundred tons of cosmic dusts and meteoroids come into the Earth's atmosphere a day (Murad & Williams, 2002). When a meteoroid penetrates into the atmosphere, its surface is heated up by collision between the meteoroid and the neutral atmosphere. Given its high entry velocity, the surface temperature of an incoming meteoroid reaches the boiling point and the surface is ablated. In the ablation process, the surface temperature is increased to ∼1850 K, producing a cylindrical plasma trail, called a meteor trail (Baggaley, 2002). A low power VHF meteor radar (MR) can detect the meteor trail in the mesosphere and lower thermosphere (MLT) day and night under almost all weather conditions. The MR can measure decay times, Doppler velocities, meteor velocities, and heights of meteors (Elford, 2004;Holdsworth et al., 2004). Using these observed parameters of meteors, the MR can provide not only the vertical profile of a neutral wind (e.g., W. Lee et al., 2021) but the daily mesospheric temperature continuously (e.g., Hocking, 1999;C. Lee et al., 2016). Although high power large aperture (HLPA) radars can detect head echoes of meteors in nonspecular directions, providing more information on various processes in the meteor plasma than the MR, the current study addresses only data from the low power MR. Data from HPLA radars have been analyzed by other groups of researchers, in terms of diffusion, turbulence, scattering that may occur in nonspecular trails (

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Seasonal variations in vertical distribution of meteor decay time as observed from meteor radars at 8.5°N and 80°N

Cited by 4 publications

References 49 publications

Monitoring observations of meteor echo at the EKB ISTP SB RAS radar: algorithms, validation, statistics

Monitoring observations of meteor echo at the EKB ISTP SB RAS radar: algorithms, validation, statistics

Latitudinal difference in meteor trail ionization heights and identification of meteor showers

A Modeling Analysis of the Apparent Linear Relation Between Mesospheric Temperatures and Meteor Height Distributions Measured by a Meteor Radar

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