A technique for reconstructing the spatial characteristics of a long-lived meteor trails on all-sky cameras

2020 ◽  
Author(s):  
Tatiana Syrenova ◽  
Roman Vasilyev ◽  
Alexander Beletsky ◽  
Alexander Mikhalev ◽  
Eselevich Maxim
Keyword(s):  
Basic Research ◽  
Solar Observatory ◽  
Meteor Shower ◽  
Meteor Showers ◽  
Main Attention ◽  
Optical Instruments ◽  
Meteor Trail ◽  
Leonid Meteor Shower ◽  
Meteor Trails ◽  
Python Programming

<p>Over the years, reports of meteor trails lasting up to one hour have periodically appeared in the literature. These observations are usually associated with particularly strong meteor showers, such as Leonids. In [Kelley et al. 2000] some interesting observations of such trails related to the 1998 Leonid meteor shower event are presented [2]. In publications devoted to the study of this phenomenon in the optical range, the main attention is paid to processes that cause a prolonged luminescence of meteor showers [Kelley et al., 2000]. Meanwhile, this phenomenon is of great interest for diagnosing the Earth upper atmosphere state and the ionosphere. The bulk of the work in this direction is based on radar observations of ionization traces, the duration of which in some cases reaches several minutes [Kashcheev et al., 1967].</p><p>This paper reports on long-lived meteor trails (LMT), which was recorded simultaneously using two optical instruments recording night sky emissions. The first all-sky camera is located at the Geophysical Observatory of the ISTP SB RAS, near the Tory (51.80 N, 103.10 E) and is designed to record the spatial picture of the 630 nm emission intensity [http: // atmos. iszf.irk.ru/ru/data/keo]. The second all-sky camera is located in the Sayan Solar Observatory of the ISTP SB RAS, near the Mondy (51.60 N, 100.90 E). A meteor trail lasting 35-40 minutes was recorded on November 18, 2017 after a meteoroid explosion on 22.23.19 UT with two cameras from different directions. Further, an algorithm was developed with the Python programming language the geographical coordinates of this event were calculated, as well as the height of the highlight</p><p>. The meteoroid explosion height and the ellipsoidal trail was being 65-70 km. Then the meteor track bow spread horizontally in a southward for 30-40 minutes at an average velocity of 58 m/s. This technique can be used to determine the main characteristics of various phenomena in the atmosphere, such as waves, SAR-arcs, meteor tracks and others.</p><p>This work was supported by a grant from the Russian Foundation for Basic Research N19-35-90093.</p>

scholarly journals Observations on Stratospheric-Mesospheric-Thermospheric temperatures using Indian MST radar and co-located LIDAR during Leonid Meteor Shower (LMS)

2002 ◽  
Vol 20 (11) ◽  
pp. 1869-1876
Author(s):  
R. Selvamurugan ◽  
C. V. Devasia ◽  
A. R. Jain ◽  
C. Raghava Reddi ◽  
P. B. Rao ◽  
...  
Keyword(s):  
Middle Atmosphere ◽  
Fold Increase ◽  
Meteor Shower ◽  
Atmospheric Composition ◽  
Temperature History ◽  
Good Time ◽  
Maximum Height ◽  
Mst Radar ◽  
Leonid Meteor Shower ◽  
Meteor Trails

Abstract. The temporal and height statistics of the occurrence of meteor trails during the Leonid meteor shower revealed the capability of the Indian MST radar to record large numbers of meteor trails. The distribution of radio meteor trails due to a Leonid meteor shower in space and time provided a unique opportunity to construct the height profiles of lower thermospheric temperatures and winds, with good time and height resolution. There was a four-fold increase in the meteor trails observed during the LMS compared to a typical non-shower day. The temperatures were found to be in excellent continuity with the temperature profiles below the radio meteor region derived from the co-located Nd-Yag LIDAR and the maximum height of the temperature profile was extended from the LIDAR to ~110 km. There are, how-ever, some significant differences between the observed profiles and the CIRA-86 model profiles. The first results on the meteor statistics and neutral temperature are presented and discussed below.  Key words. Atmospheric composition and structure (pres-sure, density, and temperature) History of geophysics (at-mospheric sciences) Meteorology and atmospheric dynamics (middle atmosphere dynamics)

scholarly journals On the validity of the ambipolar diffusion assumption in the polar mesopause region

2008 ◽  
Vol 26 (11) ◽  
pp. 3439-3443 ◽  
Author(s):  
A. P. Ballinger ◽  
P. B. Chilson ◽  
R. D. Palmer ◽  
N. J. Mitchell
Keyword(s):  
Ambient Temperature ◽  
Decay Time ◽  
Ambipolar Diffusion ◽  
Northern Sweden ◽  
Mesopause Region ◽  
Decay Times ◽  
Meteor Trail ◽  
Temperature And Pressure ◽  
Ion Recombination ◽  
Meteor Trails

Abstract. The decay of underdense meteor trails in the polar mesopause region is thought to be predominantly due to ambipolar diffusion, a process governed by the ambient temperature and pressure. Hence, observations of meteor decay times have been used to indirectly measure the temperature of the mesopause region. Using meteor observations from a SKiYMET radar in northern Sweden during 2005, this study found that weaker meteor trails have shorter decay times (on average) than relatively stronger trails. This suggests that processes other than ambipolar diffusion can play a significant role in trail diffusion. One particular mechanism, namely electron-ion recombination, is explored. This process is dependent on the initial electron density within the meteor trail, and can lead to a disproportionate reduction in decay time, depending on the strength of the meteor.

The Leonid meteor shower of 1898

1898 ◽  
Vol 19 ◽  
pp. 156
Author(s):  
Edwin F. Sawyer
Keyword(s):  
Meteor Shower ◽  
Leonid Meteor Shower

scholarly journals On the influence of neutral turbulence on ambipolar diffusivities deduced from meteor trail expansion

2002 ◽  
Vol 20 (11) ◽  
pp. 1857-1862 ◽  
Author(s):  
C. M. Hall
Keyword(s):  
Middle Atmosphere ◽  
Atmospheric Dynamics ◽  
Meteorology And Atmospheric Dynamics ◽  
Middle Atmosphere Dynamics ◽  
Radar Echoes ◽  
Meteor Trail ◽  
Meteor Trails

Abstract. By measuring fading times of radar echoes from underdense meteor trails, it is possible to deduce the ambipolar diffusivities of the ions responsible for these radar echoes. It could be anticipated that these diffusivities increase monotonically with height akin to neutral viscosity. In practice, this is not always the case. Here, we investigate the capability of neutral turbulence to affect the meteor trail diffusion rate.Key words. Meteorology and atmospheric dynamics (middle atmosphere dynamics; turbulence)

scholarly journals Ablation in Meteors

1971 ◽  
Vol 13 ◽  
pp. 259-269
Author(s):  
V. N. Lebedinets
Keyword(s):  
Physical Theory ◽  
Line Density ◽  
Radar Observations ◽  
Electron Line ◽  
Ablation Mechanism ◽  
Meteor Trail ◽  
Meteor Trails

Photographic and Radar Observations of meteors reveal essential discrepancies from the simplest physical theory of meteors. The simplest theory (Whipple, 1943; Herlofson, 1948; Kascheev et al., 1967) proceeds from the following suppositions: (1) the meteoroid is a dense non-fragmenting body; (2) the sole ablation mechanism is evaporation; and (3) the whole energy transferred to a body by colliding air molecules is spent on evaporation. In addition, the simplest theory of radiowave reflection from meteor trails that does not take into account diffusive and thermodiffusive expansion of a meteor trail and change of the electron line density along the trail is used for the interpretation of the results of radar observations.

scholarly journals <i>Letter to the Editior</i>Testing the hypothesis of the influence of neutral turbulence on the deduction of ambipolar diffusivities from meteor trail expansion

2005 ◽  
Vol 23 (3) ◽  
pp. 1071-1073 ◽  
Author(s):  
C. M. Hall ◽  
T. Aso ◽  
M. Tsutsumi ◽  
S. Nozawa ◽  
A. H. Manson ◽  
...  
Keyword(s):  
Ambient Temperature ◽  
Lower Thermosphere ◽  
Radar Echoes ◽  
Meteor Trail ◽  
Meteor Trails

Abstract. Fading times of radar echoes from underdense meteor trails in the upper mesosphere/lower thermosphere are commonly used to determine ambipolar diffusivities and hence ambient temperature. Diffusivities are generally expected to increase exponentially with height through the region from which the meteor trail echoes are obtained, viz., typically 70-110km altitude for a ~30-MHz radar. In practice, however, this is more the exception: unexpectedly large diffusivities are obtained in the lower part of the regime, and unexpectedly low values are obtained in the upper part; only in the few kilometres on either side of the maximum in echo occurrence (viz., 90km for a 30-MHz radar) does the diffusivity profile behave as expected. Hall (2002) hypothesised that neutral turbulence might be enhancing expansion of the meteor trail in the lower part of the regime. In this communication, due to results only available since the publication of Hall's suggestion, we are able to refute the hypothesis.

scholarly journals Investigation of the Motion of Periodic Comet Giacobini-Zinner and the Origin of the Draconid Meteor Showers of 1926, 1933 and 1946

1972 ◽  
Vol 45 ◽  
pp. 173-180
Author(s):  
Yu. V. Evdokimov
Keyword(s):  
Meteor Shower ◽  
Meteor Showers ◽  
Orbital Elements ◽  
Periodic Comet

Orbital elements of P/Giacobini-Zinner have been obtained from 577 observations at the eight apparitions 1900 to 1965 by linking apparitions in pairs. By this technique we established that the comet has a nongravitational secular deceleration amounting, on the average, to 0.081 day/(period)2. As a result of the comet's approach to Jupiter in 1969, a return of the Draconid meteor shower is possible on 1972 October 8d15h45m UT. The 1946 meteor shower was due to meteoroids ejected forward along the orbit of the comet in 1940 with velocities of 14 m s- 1. The meteor showers of 1933 and 1926 were apparently produced by meteoroids ejected in 1900 with velocities of 15.0 m s- 1 forward and 14.5 m s- 1 backward, respectively.

Occurrence and altitude of the non-specular long-lived meteor trails during meteor showers at high latitudes

2020 ◽  
Author(s):  
Alexander Kozlovsky ◽  
Renata Lukianova ◽  
Mark Lester
Keyword(s):  
Aerosol Particles ◽  
Height Distribution ◽  
High Latitudes ◽  
Meteor Showers ◽  
Height Difference ◽  
The Earth ◽  
Meteor Trails ◽  
June July ◽  
Two Parameters ◽  
Field Aligned Irregularities

&lt;p&gt;Meteoroids entering the Earth&amp;#8217;s atmosphere produce ionized trails, which are detectable by radio sounding. Majority of such radar detections are the echoes from cylindrical ionized trails, which occur if the radar beam is perpendicular to the trail, i.e., the reflection is specular. Typically such echoes detected by VHF radars last less than one second. However, sometimes meteor radars (MR) observe unusually long-lived meteor echoes and these echoes are non-specular (LLNS echoes). The LLNS echoes last up to several tens of seconds and show highly variable amplitude of the radar return. The LLNS echoes are received from the non-field-aligned irregularities of ionization generated along trails of bright meteors and it is believed that key role in their generation belongs to the aerosol particles arising due to fragmentation and burning of large meteoroids. The occurrence and height distributions of LLNS are studied using MR observations at Sodankyl&amp;#228; Geophysical Observatory (SGO, 67&amp;#176; 22' N, 26&amp;#176; 38' E, Finland) during 2008-2019. Two parameters are analyzed: the percentage and height distribution of LLNS echoes. These LLNS echoes constitute about 2% of all MR detections. However during certain meteor showers (Geminids, Perseids, Quadrantids, Arietids or/and Daytime &amp;#950;-Perseids, and Lyrids) the percentage of LLNS echoes is noticeably higher (about 6, 5, 4, 4, and 3%, respectively). Typically, the LLNSs occur ~2 km higher than other echoes (in June-July the height difference is reduced to ~1 km). Due to this elevation, a larger percentage of LLNSs is manifested as an upward shift of the height distribution of meteor trails during meteor showers. Moreover, during Lyrids, &amp;#951;-Aquariids, Perseids, Orionids, and Leonids the LLNS echoes occur noticeably, up to 3-6 km, higher than the echoes from other types of trails. Thus, enhanced heights of meteor detections during major meteor showers (Quadrantids, Lyrids, &amp;#951;-Aquariids, Arietids or/and Daytime &amp;#950;-Perseids, Perseids, Orionids, Leonids, and Geminids) are predominantly due to long-lived non-specular echoes from the non-field-aligned irregularities associated with large meteoroids.&lt;/p&gt;

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