Mesospheric temperature estimation from meteor decay times during Geminids meteor shower

Kozlovsky, Alexander; Lukianova, Renata; Шалимов, С. Л.; Lester, M.

doi:10.1002/2015ja022222

Cited by 16 publications

(15 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The majority of meteor trails are underdense, and moreover, the detection algorithm may reject overdense trails as nonmeteor signals (Hocking et al, ). Nevertheless, some SKiYMET meteor radar detections lasting a few tenths of a second are from overdense trails (Kozlovsky et al, ).…”

Section: Meteor Radar Observationsmentioning

confidence: 99%

Multi‐Instrumental Observations of Nonunderdense Meteor Trails

Kozlovsky¹,

Шалимов

Kero

et al. 2018

JGR Space Physics

View full text Add to dashboard Cite

Using data from the Sodankylä Geophysical Observatory (67°22′N, 26°38′E, Finland) meteor camera from the whole year 2015, we identified and investigated 28 optical meteors with accompanying ionization trails unambiguously detected by the Sodankylä Geophysical Observatory ionosonde, which sounded the ionosphere once per minute with frequency rising from 0.5 to 16 MHz. These ionosonde reflections were obtained from heights around 90 km. The electron line densities of the trails were found to be between 1014 and 1016 m−1, which characterize the trails as nonunderdense (i.e., transitional and overdense). The ionosonde reflections were observed for a few minutes, with decreasing maximal frequency of the return. During the first 250 s, for the trails with initial line density about (2–3) · 1015 m−1 the return frequency decreased with time corresponding to the diffusional expansion of cylindrical meteor trails, that is, f ∝ t−γ, where the exponent γ = 0.5, whereas less dense trails decayed slower (γ ≈ 0.2) and more dense trails decayed faster (γ ≈ 1). In many cases the meteor events were accompanied by nonspecular long‐lived detections using a colocated all‐sky interferometric meteor radar with operating frequency 36.9 MHz. As a rule the meteor radar echo durations were longer than expected from diffusional expansion of cylindrical meteor trails and their amplitudes were highly variable. We suggest that the slower frequency decrease of the ionosonde echoes and the nonspecular long‐lived meteor radar echoes might be associated with the presence of meteoric dust.

show abstract

Section: Meteor Radar Observationsmentioning

confidence: 99%

Multi‐Instrumental Observations of Nonunderdense Meteor Trails

Kozlovsky¹,

Шалимов

Kero

et al. 2018

JGR Space Physics

View full text Add to dashboard Cite

show abstract

“…Kozlovsky et al . [] indicated that the temperature estimation from meteor decay times can be severely affected by meteor showers because of the peculiar distribution of the meteor decay time within the meteor showers. However, we found that the effects of meteor showers on the linear relationship between the FWHM and the temperature at 90 km are negligible.…”

Section: Height Distribution Of Meteor Echoesmentioning

confidence: 99%

“…This nearly invariable proportionality constant allows us to estimate the temperature at the meteor peak altitude (~90 km) by using only the FWHM data observed by the meteor radar. Kozlovsky et al [2016] indicated that the temperature estimation from meteor decay times can be severely affected by meteor showers because of the peculiar distribution of the meteor decay time within the meteor showers. However, we found that the effects of meteor showers on the linear relationship between the FWHM and the temperature at 90 km are negligible.…”

Section: Height Distribution Of Meteor Echoesmentioning

confidence: 99%

New method of estimating temperatures near the mesopause region using meteor radar observations

Lee

Kim

Jee

et al. 2016

Geophysical Research Letters

View full text Add to dashboard Cite

We present a novel method of estimating temperatures near the mesopause region using meteor radar observations. The method utilizes the linear relationship between the full width at half maximum (FWHM) of the meteor height distribution and the temperature at the meteor peak height. Once the proportionality constant of the linear relationship is determined from independent temperature measurements performed over a specific period of time by the Microwave Limb Sounder (MLS) instrument on board the Aura satellite, the temperature can be estimated continuously according to the measurements of the FWHM alone without additional information. The temperatures estimated from the FWHM are consistent with the MLS temperatures throughout the study period within a margin of 3.0%. Although previous methods are based on temperature gradient or pressure assumptions, the new method does not require such assumptions, which allows us to estimate the temperature at approximately 90 km with better precision.

show abstract

“…• 38 ′ E, Finland) reported by (Kozlovsky et al, 2016) have indicated that the mesospheric temperature at an average altitude of 91 km is systematically underestimated by 20 − 50 K during the Geminid meteor shower (with the peak activity on the 13 th of December). According to the SGO meteor radar observations and data obtained with the Earth Observing System (EOS) Microwave Limb Sounder (MLS) onboard the NASA Aura satellite during the Geminid meteor shower in 2008−2014 the peak night meteor rate accounted for 15, 000 − 20, 000 mete-ors d −1 .…”

Section: Kinetics Of Interaction Between Meteoric Matter and Ozone Layermentioning

confidence: 98%