Some evolving thoughts regarding radar meteor observations

2014 ◽  
Author(s):  
J.D. Mathews
Keyword(s):  
Radar Meteor

scholarly journals The Influence of the Atmosphere on Radar Meteor Rates

1980 ◽  
Vol 90 ◽  
pp. 101-104
Author(s):  
W.G. Elford.
Keyword(s):  
Initial Diameter ◽  
Meteor Trail ◽  
Radio Studies ◽  
The Difference ◽  
Sporadic Meteors ◽  
Radar Meteor ◽  
Sharp Cutoff ◽  
Selection Of

The majority of radio studies of meteors have been carried out at frequencies higher than 17MHz and most of the rate observation at frequencies above 30MHz. At these frequencies a severe height selection of meteors occurs. In Figure 1(a) are shown the normalized height distributions of sporadic meteors observed at Adelaide on frequencies of 27MHz and 2MHz (Brown, 1976). The sharp cutoff of the latter distribution below 87 km is instrumental. The difference in the height distributions is due to the effect of the finite diameter of a meteor trail on its radar detectability. If the trail diameter is ≪ λ signals from the near and far edges reinforce but as the trail expands due to diffusion and the diameter becomes ≃ λ/4, interference reduces the amplitude. A meteor trail, produced by a particle with a velocity of 30 km s−1, has an initial diameter of 0.4m at 80 km, 2.0m at 104 km and 4.0m at 116 km.

scholarly journals 1. The radar meteor echo (survey paper)

1968 ◽  
Vol 33 ◽  
pp. 3-13 ◽  
Author(s):  
P. M. Millman
Keyword(s):  
World War Ii ◽  
Meteor Shower ◽  
New Technique ◽  
World War ◽  
The Real ◽  
Survey Paper ◽  
Radar Meteor

From about 1930 on various scattered notes appeared from time to time, pointing out certain radio effects that probably resulted from meteors. However, the real birth of the serious observation of meteors by radio took place on the night of October 9–10, 1946, when the Giacobinid meteor shower returned in considerable strength. This was observed with re-built World-War II radar equipment in both England and the U.S.A., and the results achieved left no doubt concerning the value of the new technique in meteoric astronomy. Figure 1 illustrates two historic examples of meteor echoes recorded in England on this occasion (Appleton and Naismith, 1947; Hey et al., 1947). Since this date the field has expanded rapidly. Useful general summaries may be found in a number of monographs, e.g., Lovell (1954), McKinley (1961).

scholarly journals Mesospheric winds derived from SuperDARN HF radar meteor echoes at Halley, Antarctica

1999 ◽  
Vol 51 (7-8) ◽  
pp. 685-689 ◽  
Author(s):  
Barbara Jenkins ◽  
Martin J. Jarvis
Keyword(s):  
Hf Radar ◽  
Radar Meteor

Extensive meteoroid fragmentation in V/UHF radar meteor observations at Arecibo Observatory

2010 ◽  
Vol 37 (4) ◽  
Author(s):  
J. D. Mathews ◽  
S. J. Briczinski ◽  
A. Malhotra ◽  
J. Cross
Keyword(s):  
Arecibo Observatory ◽  
Uhf Radar ◽  
Radar Meteor

Growth and decline of a scientific speacialty: The case of radar meteor research

Eos ◽  
1977 ◽  
Vol 58 (5) ◽  
pp. 273 ◽  
Author(s):  
G. Nigel Gilbert
Keyword(s):  
Radar Meteor

The structure of meteor streams associated with Comet Halley: Eta Aquarids and Orionids

1974 ◽  
Vol 22 ◽  
pp. 309-311
Author(s):  
Anton Hajduk
Keyword(s):  
Density Distribution ◽  
Meteor Shower ◽  
Point Of View ◽  
Orbital Elements ◽  
Statistical Point ◽  
Radar Observations ◽  
Meteor Streams ◽  
Stream Structure ◽  
Comet Halley ◽  
Radar Meteor

The association of Comet Halley with the Orionid and Eta Aquarid meteor streams is not commonly accepted at present. Southworth (1961) has determined the differences in the orbital elements of the Orionid stream and Comet Halley on the basis of 19 photographic meteors and found them to be rather large.Extensive observational material obtained since the beginning of this century, including a homogeneous series of the radar observations, carried out at the Springhill Meteor Observatory during the periods of the Orionid meteor shower activity in 1957–1967 has been used by the author (Hajduk 1971) to study the stream structure and its association with Comet Halley from a statistical point of view.The present analysis is an extension of the paper mentioned, based mainly on the radar observations of the Eta Aquarid meteor shower carried out at the Springhill Observatory during the period 1958–67. The total number of 240,000 radar meteor echoes observed in 670 hours between May 1 and May 10 during each of the years previously cited was used in this investigation. The observed variations in the hourly rates of echoes of different duration enable us to study the density distribution and size distribution of meteoric particles along and across the stream.

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