METEOR STUDIES NETWORK
1. INTRODUCTION
The Meteor Studies Network was established following the recommendation
of the International Halley Watch (IHW) Steering Group (Prague, June 1984).
Its personnel is listed in Table I. The Discipline Specialist team was
responsible for the scientific program and coordination of meteor studies in
the IHW. The program provided an opportunity to coordinate and combine many
different types of observations relating to the Halley meteor showers. The
main observing techniques utilized meteor radars and visual recording (naked-
eye). Very few observations (direct or spectroscopic) were obtained with
cameras or with photoelectric devices, and none were archived.
Table I. The Meteor Studies Discipline Specialist Team
______________________________________________________________________________
Team Member Affiliation Responsibility
______________________________________________________________________________
P.B. Babadzhanov Tajik Astrophysical Institute Discipline Specialist
734042 Dushanbe
U.S.S.R.
A. Hajduk Astronomical Institute SAV Discipline Specialist
CS-84228 Bratislava
Czechoslovakia
B.A. Lindblad Lund Observatory, Box 43 Discipline Specialist
S-22100 Lund
Sweden
B.A. McIntosh National Research Council Canada Discipline Specialist
Ottawa
Canada K1A 0R6
______________________________________________________________________________
2. THE HALLEY METEOR SHOWERS
The Earth makes two close approaches to the comet orbit, once in early
May, and again in late October. In common with other comet-produced meteor
streams, the dust ejected from Halley is dispersed along the orbit and
laterally from the orbit; but, uncommonly in meteor astronomy, the Earth
passes twice every year through the band of Halley particles, thus producing
the long-known Eta-Aquarid (May) and Orionid (October) meteor showers. Most
of the meteor activity is confined to a period of about five days in each
case. However, this period is not well defined; shower meteors have been
observed over as long as fourteen days. Furthermore the activity is not
consistent from year to year -- the position in time of maximum flux shifts
significantly and there are secondary maxima. Hence an activity curve for one
year is not a reliable predictos for the activity in another year. If
averaged over many years, a broad flat curve results, which again is not
indicative of annual activity.
Traditional visual observations have never been carried out over suffici-
ently long intervals of time to define clearly the structure of the stream.
Radar observations have contributed to our understanding of the structure, but
they are also not without problems. A paper by Hajduk (1970) summarizes
visual and radar observations from 1900 to 1969. There are also some earlier,
medieval and ancient observations.
The geometric relation between the Earth's orbit and the comet's current
orbit suggests that the two showers should not be of equal strength or equal
duration, which is contrary to actual observations. A recent theory (McIntosh
and Hajduk 1983; McIntosh and Jones 1988) proposes that the long-term
evolution of comet and dust results in a flat ribbon of particles so that the
Earth's two crossings yield approximately equal-activity, equal-duration
showers.
Observationally the meteors are very fast (V > 65 km/s for both showers),
with persistent trains being common. Studies of the physical characteristics
and composition of the particles are sparse, but there is no evidence that
they are unusual.
The visual rates for the showers may be as high as 30 per hour depending
on the latitude of the observer. The low-declination radiant of the May
shower (in Aquarius, at R.A. = 335.5 deg, Dec = -1.9 deg) rises only a little
before sunrise, particularly at high northern latitudes, providing a very
limited period for visual or optical observations. More extensive coverage by
Southern Hemisphere observers was needed.
The observing period for the Orionids extends through nearly the entire
night because of the radiant's much greater elongation from the Sun (R.A. =
94.5 deg, Dec = +15.8 deg). The higher declination and time of the year
favour Northern Hemisphere observers.
Studies benefit also from observations at many longitudes around the
Earth. This is true of the Eta-Aquarids in particular.
3. SCIENTIFIC GOALS
Meteor observations are specifically oriented toward studies of comet-
meteor relationships. They contribute to comet science mainly in the areas of
dust production and the dust-particle dynamics. These aspects can be enhanced
by:
o determination of the number density and mass distribution of particles
in the showers,
o determination of the properties and composition of the particles,
o study of the evolution of the Halley meteor stream,
o study of the spatial structure of the stream, especially as a function
of particle mass.
The IHW program provided an opportunity to coordinate and combine many
different observations to determine the stream structure with high resolution
and to infer from this the production and dynamical evolution of the larger
dust particles.
This goal is independent of the current comet passage. No increase in
normal meteor shower rates was expected, and none was observed. It was thought
that the more rapid and wider dispersal of fine particles might contribute
fresh meteors observable on sensitive instruments. These were searched for
with the Canadian High-Power Meteor Radar, particularly at the time of the
Earth's passage through the comet orbit plane, but results were negative.
4. OBSERVATIONS
4.1 General
The disintegration of a meteoroid in the Earth's atmosphere produces
light and ionization, both of which have a complex relation to the enrgy (mass
and velocity) of the particle. A meteor trail can reflect radio waves,
producing "echoes" having measurable parameters such as amplitude and duration
which can be related to the properties and energy of the particle. Some
radars are able to determine meteor velocity.
The luminous meteor is a point source moving with sufficiently high
angular velocity that the human eye is a more sensitive detector than typical
lenses and photographic emulsions. However, the eye is not a particularly
satisfactory quantitative recorder of brightness and position. The current
sensitivity of electronic imaging devices much exceeds that of the human eye.
Spectral measurements are particularly simple because the meteor is a
self- produced "slit". However, orientation of the "slit" is not under
control and therefore not always optimum with respect to the spectral
dispersion. High dispersion spectra permit detailed studies of meteoroid
composition and thus give valuable information on the solid component of the
cometary nucleus.
4.2 Techniques and Methods
In order to cover as wide a mass range of meteors as possible, a variety
of ground-based techniques is required. The resulting data are of many types
and in many formats. In general the data occur in two basic forms --
statistical counts and single events. It was established that all statistical
counts would be for one-hour intervals. These observations range from a
simple count of meteors seen, to diversified radar echo counts in multiple
interval classes of range (distance) and/or echo duration or echo amplitude.
Details of observing procedures and data formats are given in Attachments
A (STANDARDS) and B (DATA FORMATS FOR METEOR STUDIES). Forms used for amateur
visual observations may be found in the IHW Amateur Observations Network.
It was stressed to all observers that it was important to distinguish
carefully between meteors belonging to the Halley showers and those that are
background or other shower meteors. Shower counts are at best slightly higher
than background counts and at worst only a small fraction thereof.
Visual observations require an almost instantaneous judgement on a
fleeting event, based primarily on extrapolating the trail back to the
radiant, and secondarily on consideration of the velocity of the meteor. The
much greater precision of photographs or photoelectric imaging makes
distinction easier. Some radars are able to distinguish on the basis of
velocity and/or the geometry of the trail, but for others, shower counts are
obtained only by subtraction of an assumed background rate.
Although careful counting of shower meteors was deemed paramount, experi-
enced observers were encouraged to estimate magnitudes to the nearest half or
whole magnitude. Less importance was attached to ancillary characteristics
such as meteor colour or train duration.
It was required that radar meteor echo counts be made in standardized
class intervals of echo duration and amplitude.
4.3 Periods for Observing
Major activity takes place at solar longitudes 42.5-47 deg (May 3-8) for
the Eta Aquarid shower and 206-210 deg (Oct 19-24). At least two other
relatively stable secondary maxima have been observed in both showers. They
are distinctly separated from the main zones at longitudes 38 deg and 50 deg
(Apr 28/29 and May 10/11) and at 203 deg and 215 deg (Oct 16/17 and 28/29).
The maximum at the beginning of each shower is of particular interest since
it is thought to contain particles of most recent vintage.
As noted earlier, activity extends over as much as fourteen days--between
solar longitudes 37 and 51 deg (Apr 27-May 11) and between 202 and 216 deg
(Oct 15-30), with priority given to the central interval. The lunar phase
is significant for visual observations and was reasonably good for the two
years: the new moon occurred on 28 October 1985 and 9 May 1986.
4.4 Results
The suite of data which has been archived consists of radar meteor counts
and visual observations. The radar stations which provided data are listed in
Attachment C. They range from latitude +54 deg to -33 deg, longitude 75 deg W
(285 deg) to 69 deg E. Observations of both the Eta Aquarid and Orionid
meteor showers from 1984 through 1988 are included--a total of 5662 hours of
data. (Note that this count includes duplicate hours.) The details are listed
in Attachment D.
The visual observations of meteors which were accumulated by the Amateur
Observations Network were processed by Dr. A. Hajduk and his colleagues at the
Interplanetary Matter Division, Slovak Astronomical Institute, Bratislava,
Czechoslovakia. Based on their considerable experience in processing visual
meteor observations, they found that approximately 2/3 of the sets of observa-
tions were of acceptable quality. The data encompass over 1600 hours of
observations of the showers in the years 1984 to 1987 with a few hours also
from 1982. A summary of the data is given in Attachment D; observing sites
and observers are listed in Attachment C.
5. REFERENCES
Hajduk, A. (1970). Bull. Astron. Inst. Czech. 21, 37.
McIntosh, B.A., and Hajduk, A. (1983). Mon. Not. R. Astron. Soc. 205, 931.
McIntosh, B.A., and Jones, J. (1988). Mon. Not. R. Astron. Soc. 235, 673.
P.B. Babadzhanov A. Hajduk
Tajik Astrophysical Institute Astronomical Institute SAV
734042 Dushanbe 84228 Bratislava
USSR Czechoslovakia
B.A. Lindblad B.A. McIntosh
Lund Observatory, Box 43 National Research Council Canada
S-22100 Lund Ottawa
Sweden Canada K1A 0R6
ATTACHMENT A: STANDARDS
A.1 Time
The time interval for counts--either visual or radar--shall be one hour.
A count for an interval of greater than, or equal to, one-half hour may be
prorated to an equivalent hour count. Intervals shorter than one-half hour
should be discarded. The tabulated absolute time for a count shall be the
beginning of the hour.
A.2 Radar Meteors
A.2.1 Range class intervals
Preference is for counts that are given in range class intervals which
are not less than 10 kilometres, and not greater than 20 kilometres.
A.2.2 Duration class intervals
Minimum standard. There shall be at least three duration classes:
(1) counts of long-duration echoes down to the value t1,
(2) counts of medium-duration between t1 and t2,
(3) counts of short-duration echoes having durations less than t2;
where either t1 or t2 shall be one (1) second, and the ratio t1/t2 shall be
>2.
A.2.3 Radio magnitudes
For purposes of standardization, meteor electron line densities q shall
be quoted in electrons/meter or on a logarithmic magnitude scale Mr, where
Mr = 40 - 2.5 x log10(q).
A.3 Visual Meteor Counts
Magnitude may be estimated to the nearest half or whole magnitude. A
value given as magnitude 3 shall be deemed to lie in the interval 2.5 to 3.5,
etc.
ATTACHMENT B: DATA FORMATS FOR METEOR STUDIES
FITS headers include the standard IHW Mandatory keywords. The notes
below apply to the keywords as used by the Meteor Discipline. The main
header is in Table B-I.
Table B-I. Main Header
__________________________________________________________________________
KEYWORD EXPLANATION FORMAT
__________________________________________________________________________
BITPIX = 8 \ 8-bit characters
EXTEND = T \ Yes, a table
DAT-FORM = 'ASCII '
OBJECT Name of meteor shower 'ORIONID' or 'ETA-AQUARID'
FILE NUM = File number--Beginning with 9 and
followed by a unique 5-digit num-
ber
DATE-OBS UT date of middle of observing pe-
riod. See notes for shower periods 'DD/MM/YY'
TIME-OBS UT time of middle of observation.
Not significant for meteor observa-
tions and therefore usually given
as 0.0
DISCIPLN IHW Discipline 'METEOR STUDIES'
SYSTEM Key to finding observing system in
discipline/station catalog. Insti-
tutes with long-standing observing
instruments are listed in Attach-
ment C '9uuuccnn'
OBSERVER 'Onename,I'
or or
SUBMITTR 'Oneperson,J/Otherperson,K'
or
'Firstperson,L/ET AL' if more than
two
DAT-FORM 'ASCII ' data are in character
form, usually implying tables and
BITPIX=8.
OBSVTORY name of submitting observatory 'Tadjik Astrophy Inst'
LOCATION location of submitting observatory 'Dushanbe, USSR'
LIM-SENS threshold sensitivity for obser-
vations not cataloged by SYSTEM.
Given as limiting magnitude (pho-
tographic, visual, or equivalent
radio magnitude or electron line '+8M radio'
density) '10**14 electron/m'
QUALITY estimate of the quality of the ob-
servation on a scale of: 1 = poor,
to 5 = excellent, with 0 = unknown 2
__________________________________________________________________________
An extension header is signalled by the lines shown in Table B-II.
Table B-II. Extension Header
________________________________________________________________________
XTENSION = 'TABLE '
BITPIX = 8 / 8-bit characters
NAXIS = 2
NAXIS1 is the width (or line length) of the table
NAXIS2 is the number of lines in the table - frequently the number of
hours represented by the observations if they are presented as
one hour per line
________________________________________________________________________
Data records are specific to a type of observation, a particular observa-
tory, etc., and cannot all be described here. We provide examples for a
meteor radar in Table B-III and for visual observations in Table B-IV. The
data in Table B-III are echo counts in class intervals of duration and range
in one-hour intervals. Time is included. It is to be emphasized that there
are differences among the formats set up by the various institutions.
Table B-III. Example of EXTENSION Header and Data for Meteor Radar
Observations
______________________________________________________________________________
XTENSION= 'TABLE ' / table extension
BITPIX = 8 / bits per character
NAXIS = 2 / dimensions of table
NAXIS1 = 100 / characters per line
NAXIS2 = 193 / hours of observations
PCOUNT = 0 / no random parameters
GCOUNT = 1 / only one group
TFIELDS = 35 / fields per line
EXTNAME = 'ORIONIDS 86' / name of table
COMMENT Description of the table columns.
COMMENT There is one space between each field.
TTYPE1 = 'YR ' / year
TBCOL1 = 1 / starting column
TFORM1 = 'I2 ' / 2-digit integer
TTYPE2 = 'MO ' / month
TBCOL2 = 4 / starting column
TFORM2 = 'I2 ' / 2-digit integer
TTYPE3 = 'DA ' / UT day
TBCOL3 = 7 / starting column
TFORM3 = 'I2 ' / 2-digit integer
TTYPE4 = 'HR ' / UT hour
TBCOL4 = 10 / starting column
TFORM4 = 'I2 ' / 2-digit integer
TTYPE5 = 'TOTAL ' / total hour count
TBCOL5 = 13 / starting column
TFORM5 = 'I3 ' / 3-digit integer
TTYPE6 = '>=1sec ' / count for durations >=1 sec
TBCOL6 = 17 / starting column
TFORM6 = 'I3 ' / 3-digit integer
TTYPE7 = '>=8sec ' / count for durations >=8 sec
TBCOL7 = 21 / starting column
TFORM7 = 'I2 ' / 2-digit integer
TTYPE8 = ' 75 ' / count in 10km range class 70-80 km
TBCOL8 = 24 / starting column
TFORM8 = 'I1 ' / 1-digit integer
TTYPE9 = ' 85 ' / count in 10km range class
TBCOL9 = 26 / starting column
TFORM9 = 'I2 ' / 2-digit integer
TTYPE10 = ' 95 ' / count in 10km range class
TBCOL10 = 29 / starting column
TFORM10 = 'I2 ' / 2-digit integer
TTYPE11 = '105 ' / count in 10km range class
TBCOL11 = 32 / starting column
TFORM11 = 'I2 ' / 2-digit integer
TTYPE12 = '115 ' / count in 10km range class
TBCOL12 = 35 / starting column
TFORM12 = 'I2 ' / 2-digit integer
TTYPE13 = '125 ' / count in 10km range class
TBCOL13 = 38 / starting column
TFORM13 = 'I2 ' / 2-digit integer
TTYPE14 = '135 ' / count in 10km range class
TBCOL14 = 41 / starting column
TFORM14 = 'I2 ' / 2-digit integer
TTYPE15 = '145 ' / count in 10km range class
TBCOL15 = 44 / starting column
TFORM15 = 'I2 ' / 2-digit integer
TTYPE16 = '155 ' / count in 10km range class
TBCOL16 = 47 / starting column
TFORM16 = 'I2 ' / 2-digit integer
TTYPE17 = '165 ' / count in 10km range class
TBCOL17 = 50 / starting column
TFORM17 = 'I2 ' / 2-digit integer
TTYPE18 = '175 ' / count in 10km range class
TBCOL18 = 53 / starting column
TFORM18 = 'I2 ' / 2-digit integer
TTYPE19 = '185 ' / count in 10km range class
TBCOL19 = 56 / starting column
TFORM19 = 'I2 ' / 2-digit integer
TTYPE20 = '195 ' / count in 10km range class
TBCOL20 = 59 / starting column
TFORM20 = 'I2 ' / 2-digit integer
TTYPE21 = '205 ' / count in 10km range class
TBCOL21 = 62 / starting column
TFORM21 = 'I2 ' / 2-digit integer
TTYPE22 = '215 ' / count in 10km range class
TBCOL22 = 65 / starting column
TFORM22 = 'I2 ' / 2-digit integer
TTYPE23 = '225 ' / count in 10km range class
TBCOL23 = 68 / starting column
TFORM23 = 'I2 ' / 2-digit integer
TTYPE24 = '235 ' / count in 10km range class
TBCOL24 = 71 / starting column
TFORM24 = 'I2 ' / 2-digit integer
TTYPE25 = '245 ' / count in 10km range class
TBCOL25 = 74 / starting column
TFORM25 = 'I2 ' / 2-digit integer
TTYPE26 = '255 ' / count in 10km range class
TBCOL26 = 77 / starting column
TFORM26 = 'I2 ' / 2-digit integer
TTYPE27 = '265 ' / count in 10km range class
TBCOL27 = 80 / starting column
TFORM27 = 'I2 ' / 2-digit integer
TTYPE28 = '275 ' / count in 10km range class
TBCOL28 = 83 / starting column
TFORM28 = 'I2 ' / 2-digit integer
TTYPE29 = '285 ' / count in 10km range class
TBCOL29 = 86 / starting column
TFORM29 = 'I2 ' / 2-digit integer
TTYPE30 = '295 ' / count in 10km range class
TBCOL30 = 89 / starting column
TFORM30 = 'I2 ' / 2-digit integer
TTYPE31 = '305 ' / count in 10km range class
TBCOL31 = 92 / starting column
TFORM31 = 'I1 ' / 1-digit integer
TTYPE32 = '315 ' / count in 10km range class
TBCOL32 = 94 / starting column
TFORM32 = 'I1 ' / 1-digit integer
TTYPE33 = '325 ' / count in 10km range class
TBCOL33 = 96 / starting column
TFORM33 = 'I1 ' / 1-digit integer
TTYPE34 = '335 ' / count in 10km range class
TBCOL34 = 98 / starting column
TFORM34 = 'I1 ' / 1-digit integer
TTYPE35 = '345 ' / count in 10km range class
TBCOL35 = 100 / starting column
TFORM35 = 'I1 ' / 1-digit integer
END
______________________________________________________________________________
Data Record
In the following, the first two lines would not appear in the data record
but are entered here to show the headings and column alignment. The third
line is the actual first line of the data record. It represents a string of
100 ASCII characters.
75 95 115 135 155 175 195 215 235 255 275 295 315 335
YR MO DA HR TOT >=1 >=8 85 105 125 145 165 185 205 225 245 265 285 305 325 345
86 10 16 14 304 8 2 0 0 0 0 4 6 28 20 30 26 22 22 22 24 12 12 6 8 8 14 8 6 6 4 8 2 6 0
Practices and procedures for visual meteor observing may be found in the
description of the Amateur Observations Network.
Table B-IV. Example of EXTENSION Header and Data for Visual Meteor
Observations
______________________________________________________________________________
XTENSION= 'TABLE ' / table extension
BITPIX = 8 / bits per character
NAXIS = 2 / dimensions of table
NAXIS1 = 40 / characters per line
NAXIS2 = 134 / number of lines in the table
PCOUNT = 0 / no random parameters
GCOUNT = 1 / only one group
TFIELDS = 10 / fields per line
EXTNAME = 'ETA-AQUARIDS85' / name of table
COMMENT Description of the table columns.
TTYPE1 = 'YR ' / year
TBCOL1 = 3 / starting column
TFORM1 = 'I2 ' / 2-digit integer
TTYPE2 = 'MO ' / month
TBCOL2 = 6 / starting column
TFORM2 = 'I2 ' / 2-digit integer
TTYPE3 = 'DAY ' / UT day & fraction
TBCOL3 = 10 / starting column
TFORM3 = 'E5.2 ' / 5-DIGIT 2 DECIMAL PLACES
TTYPE4 = 'TIME ' / total minute count
TBCOL4 = 16 / starting column
TFORM4 = 'I3 / 3-digit integer
TTYPE5 = 'OBS ' / observer number
TBCOL5 = 20 / starting column
TFORM5 = 'I3 ' / 3-digit integer
TTYPE6 = 'SITE ' / site number
TBCOL6 = 24 / starting column
TFORM6 = 'I3 ' / 3-digit integer
TTYPE7 = 'F-STAR ' / faintest magnitude visible
TBCOL7 = 29 / starting column
TFORM7 = 'E3.1 ' / 3-digit 1 decimal place
TTYPE8 = 'CLOUD ' / cloud cover in %
TBCOL8 = 33 / starting column
TFORM8 = 'I2 ' / 2-digit integer
TTYPE9 = 'NUM-SH ' / count shower meteors
TBCOL9 = 35 / starting column
TFORM9 = 'I3 ' / 3-digit integer
TTYPE10 = 'NUM-NS ' / count non-shower meteors
TBCOL10 = 38 / starting column
TFORM10 = 'I3 ' / 3-digit integer
END
______________________________________________________________________________
Data Record
In the following, the first line would not appear in the data record but
itis entered here to show the headings and column alignment. The second line
is the actual first line of the data record. It is a string of 40 ASCII
characters.
YR MO DAY TME OBS STE MAG CL SH NS
85 4 17.81 60 66 318 6.6 0 0 25
ATTACHMENT C: SYSTEM CATALOG
The keyword SYSTEM in the Meteor Studies data format is made up as
follows:
Meteor Studies Country
\ /
9uuuccnn
/ \
IAU observatory number (if Instrument (number assigned
one exists, otherwise 500) by Meteor Studies Network)
Of the detailed list of instrument types given in the Meteor Studies
Handbook, only that for meteor radars survived. No optical data were
received, and for naked-eye visual observations, the site numbers and observer
numbers listed below in Tables C-I and C-II are included in each data table.
Table C-I. Meteor Radar Stations
____________________________________________________________________________________________________________________________
SYSTEM Station Coord. Freq. Peak Pulse Pulse Min. Antenna system Notes, special
Long. power repet. durat. line. (observing method) programs, etc.
Lat. freq. dens.
(~) (MHz) (kW) (Hz) (fs) (el/m)
____________________________________________________________________________________________________________________________
95000700 Budrio 11.63 42.7 200 140 10 1.0 Interferometric; fixed Computer recording;
44.55 E14 elevation and azimuth Heights
95002401 Dushanbe 69.0 37.5 26 500 40 2.0 2 Yagi arrays pointing Computer recording;
38.5 E13 E and N; fixed elevation Velocities
95003508 Ondrejov 14.78 37.5 40 500 10 1.0 6 dipole array at 45 deg Film speed 3.36m/hr
49.92 E13 elev.; steerable in azimuth
95005409 Onsala 12.00 32.6 25 50 10 1.0 Half-wave dipole (Tx), Film speed 10.0m/hr
57.40 E14 steerable Yagi array (Rx)
95002110 Ottawa 284.53 32.7 25 120 20 2.5 Omnidirectional Film speed 1.25m/hr
45.20 E13 (crossed dipoles)
95001312 Grahamstown 26.52 28 40 500 1000 1.0 Array of half-wave dipoles; Direction of arrival;
-33.30 E13 fixed elevation and azimuth Doppler shifts (winds)
____________________________________________________________________________________________________________________________
Table C-II. Visual Sites
_____________________________________________________________
Site No. Long. Lat. Elev.
(deg,arcmin) (meter)
_____________________________________________________________
POTSDAM 102 13 01 52 23 34
RADEBEUL 103 13 38 51 06 180
ARNSTADT 104 10 54 50 48
CARLSFELD 105 12 35 50 26
BERLIN 106 13 34 52 25
LIMBACH 107 12 46 50 50
KARL-MARX-STADT 1 108 12 57 50 52
WEISSWASSER 109 14 38 51 29 160
MARSASCALA 110 14 34 35 52 56
AROSIO 111 9 38 46 42 1500
DEMEN 112 11 26 53 23
DRESDEN 113 13 48 50 58
GOLM 114 12 57 52 24 35
KARL-MARX-STADT 2 115 12 54 50 48 250
SCHNEEBERG 116 12 38 50 36
SOHLAND 117 14 25 51 01
HAVDRUP 118 12 07 55 32
KLOVBORG 119 9 28 55 55
HADERSLEV 120 9 35 55 17
CAMBRIDGE 121 357 39 51 45
BOLY 122 18 32 45 52 128
BAJA 123 18 57 46 11
FOT 124 19 12 47 39
LAJOS FORRAS 125 19 00 47 45 550
SULYSAP 126 19 32 47 27 200
TATA 127 18 24 47 40 200
KAJDACS 128 18 37 46 34
MEZOBERENY 129 21 00 46 48
OROSHAZA 130 20 41 46 34
VASAS 131 16 46 47 05
ZALAEGERSZEG 132 16 50 46 50
SATU-NOU 133 24 38 47 08
TAMPERE 135 23 37 61 30 150
RAUMA 136 21 29 61 08
PARTALANKOSKI 137 25 05 61 53
HELSINKI 138 25 11 60 11 2
HEGGEDAL 139 10 24 59 47
KONGSBERG 140 9 36 59 42
VIBY 141 10 42 55 30
RONNE 142 14 43 52 09
BRONDBY 143 12 25 55 39
ULM 144 10 02 48 27
NEAR FISCHEN 145 10 13 47 29
GROSS WOKERN 146 12 29 53 45
PAPA 147 17 27 47 22
GUSTROW 149 12 09 53 47
BASDORF 150 13 27 52 43 50
CATANZARO 151 16 36 38 54
COMO 152 9 3 45 49
FGURA 153 14 31 35 52 47
ZURRIEG 154 14 25 35 51 30
MOSTA 155 14 26 35 54
MSIDA 156 14 50 35 54
ZAVADA 157 19 44 48 32
VARTOVKA 158 19 09 48 43
DELHI 201 77 20 28 40
ARUYAMA 202 136 06 35 09 100
HOSHINOKITSUSASHITSU 203 141 08 39 28 71
MUROH-NARA 204 136 01 34 34 400
KINOE-CHO HIROSHIMA 205 132 55 34 13 2
MT. TSUKUBA 206 140 08 36 12 360
KANAYA TOYAMASHI 207 137 10 36 41 15
KITAJIMA TAINOHAMA 208 134 33 34 07 2
SAYAMA OBS. 209 139 28 35 51 46
KAWAUCHI KIRYU 210 139 20 36 10 55
MATSUE 211 133 07 35 26
OHCHI-GUN 212 132 27 34 53
KAWASAKI OBS. 213 135 23 34 23 75
KAWATANA 214 129 50 33 04 10
KAMI TOWN 215 134 53 35 06
FUKUMITMACHI TOYA 216 136 54 36 33 72
KITAOJI OTSU 217 135 53 34 58 233
HIGASHI-SON, OKINAWA 218 128 13 26 38 100
SHIROYAMA 219 137 14 34 54 136
NEAR FUJINOMIYA 220 138 48 35 20 1455
CARTER OBS. 301 174 46 -41 17
BROWN OWL OBS. 302 175 06 -41 06 140
MANA OBS. 303 174 52 -41 05
GLENEAGLE 304 116 25 -32 20
DRYANDRA 305 117 11 -32 49
DARKES FOREST 306 150 50 -34 13
BUNDABERG 307 152 21 -24 50
KARNET 308 116 05 -32 31
THORNLIE 309 115 58 -32 02
BYFORD 310 116 01 -32 15
BLACK BIRCH 311 173 48 -41 48
AUCKLAND 312 174 47 -36 51
GAWLER 314 138 45 -34 36
KALAMUNDA 315 116 04 -31 59
YORKRAKINE 316 117 35 -31 26
BELMONT 317 151 35 -33 00
BALLAJURA 318 115 50 -31 49
RIVERVALE 319 115 56 -31 56
ROLEYSTONE 320 116 05 -32 07
GIDGEGANUP 321 116 17 -31 42
BAROSSA VALLEY 322 138 56 -34 34
COOTAMUNDRA 323 148 03 -34 41
PAVAVTANANUI FIELD S 324 174 56 -41 08
TOODYAY 325 116 28 -31 35
JARRAHDALE 326 116 05 -32 20
COLO 327 149 36 -31 55
COONABARRAN 328 149 30 -31 06
BROOME 329 122 12 -18 00
PERTH 330 116 00 -32 00
EWA BEACH 401 201 59 21 20
BARBERS POINT 402 201 57 21 20
KIPAPA GULOH 403 201 59 21 26
PEARL HARBOUR 404 202 05 21 25
DALLAS 405 263 21 32 43
MC KENDREE 406 283 22 38 47
ROSEBURG 407 237 13 43 22
WHITTAKER PEAK 408 241 18 34 34 914
SAN DIEGO 409 242 59 32 42
NEAR BELLEFONTE 410 282 05 40 55
NUGGET 411 247 26 53 08
POLISH SETTLEMENT 413 247 11 53 53
ELK ISLE 414 247 09 53 31
HALIFAX 415 296 23 44 39
VALSAYN 416 298 36 10 38
SEBRING 417 278 40 27 20
WORCESTER 418 285 16 42 35 640
WEAVERS NEEDLE 419 248 34 33 24
PHILADELPHIA 420 284 51 39 56
CLARION PA 421 280 37 42 12 460
MIQUELON 422 247 05 53 14
WINNIPEG 423 262 36 49 54 232
ALPINE 424 243 22 32 50 885
CABRERA 425 249 03 31 19 1220
U.P.N. 426 249 02 31 20 1240
LAIE 427 202 04 21 39
PUNTA ARENAS 428 275 06 9 54
FT. DAVIS 429 256 03 30 36
LA SALLE STATE PARK 430 272 32 41 04
HERB'S FIELD 431 237 44 37 17 167
BELO HORIZONTE 501 315 10 -20 43 997
PORTO ALEGRE 1 502 308 50 -29 55 4
PORTO ALEGRE 2 503 308 48 -30 03 4
PORTO ALEGRE 3 504 308 30 -30 14 200
LA PAZ 2 506 291 55 -16 32 3360
LA PAZ 1 507 291 52 -16 31 3580
BRAZILIA 508 312 20 -15 55 1100
ARAMBARE 509 308 30 -30 55
PORTO ALEGRE 4 510 308 33 -30 55
PORTO ALEGRE 5 511 309 00 -30 23 4
PORTO ALEGRE 6 512 308 51 -30 04
IRAI 513 306 37 -27 21 522
PORTO ALEGRE 7 514 308 49 -30 05 295
PORTO ALEGRE 8 515 309 06 -29 51 30
PORTO ALEGRE 9 516 309 17 -30 12 15
FORTALEZA 517 321 00 -3 34
SANTA ANA, TARIJA 518 295 29 -21 37 1900
VILLA ELISA 519 301 57 -34 50 20
ABAGAZA, ZARATE 520 300 58 -34 07 26
PORTO ALEGRE 10 521 309 52 -29 48
PORTO ALEGRE 11 522 350 50 -30 03 6
PORTO ALEGRE 12 523 308 49 -30 05
SAO PAOLO 524 313 17 -23 32 780
_____________________________________________________________
The following two tables present the individual visual observers who
participated in the Meteor Studies Network activities. They are listed in
Table C-III alphabeticallyi, in Table C-IV by their identification numbers.
Table C-III. Visual
Observers Listed
Alphabetically
_______________________
Observer No.
_______________________
ABELA S. 222
ADIB C.A. 158
ALCARAZ D. 229
ALDRICH P.T. 001
ALMEIDA L.D. 159
ANDERSON C. 003
ANDRESEN B. 002
ANTHONY D. 004
AOTA T. 185
AQUILINA J. 220
ARAUJO P. 265
ARCE M. 233
ARCE V. 234
ARLT R. 005
AZEVEDO C. 157
AZOFEIFA D.E. 246
BABNIC S. 208
BALDACCHINO G. 091
BALDAUF P. 094
BALL J. 198
BARATA P. 274
BARKAT S. 006
BARROW R. 148
BEAZLEY I. 250
BERKO E. 132
BOSCHAT M.E. 147
BROWN P. 261
BURROWS J. 199
BUSSON A. 110
CAKE D. 007
CARLOS F. 117
CLARK M. 239
CLAY M. 008
COCKERAM L. 009
COCKERAM M. 010
COMOS G. 210
COOK A. 145
CORONEOS M. 228
COWIE F. 196
CSABAI I. 127
CZESCIK C. 011
DALAVIA O.D. 152
DARVANN T. 012
DA SILVA L.A. 153
DE ABREU E.R. 070
DE ARAUJO L. 268
DECONINCK M. 013
DIETEL F. 014
DOCKING G. 200
DOHRMANN M. 192
DOMENY G. 130
DOUGHTY S. 015
DURHAM D. 016
DYMOVA G. 213
ESPINOZA E. 112
EVANS S. 017
FARKAS E. 082
FERDINANDO D. 018
FETTIG S. 144
FITZGERALD P. 019
FODOR A. 086
FOLDESI F. 089
FOLEY C. 240
FORTUNATO H. 272
FROTA L.M. 116
FUJITA Y. 179
FUNANO K. 190
GHISOLFI E.S. 201
GILROY J. 021
GOLDSMITH J. 022
GOODKNECHT R. 140
GOODMAN D. 023
GRAY M. 024
GUHL K. 193
GYARMATI L. 084
HAAGH N. 029
HALMI G. 133
HARADA S. 181
HARNISCH T. 030
HARVEY N. 224
HASHIMOTO T. 248
HAYS R. 114
HILLESTAD T.E. 031
HINTON C. 275
HINZ W. 032
HIRAGA E. 189
HIROE T. 176
HOLLOSY T. 128
HOTAKAINEN,M 076
INOUE M. 187
INOUE S. 186
INWOOD N. 034
ITO O. 168
JAASKELAINEN P. 071
JENKINSON C. 033
KAALZ A. 095
KADLCIK M. 194
KAWASAKI Y. 177
KEIICHI F. 171
KERR S. 025
KESZTHELYI S. 134
KITAHATA K. 184
KNOEFEL A. 108
KOCH B. 026
KOSCHACK R. 027
KRAWIETZ A. 098
KRISTENSEN G.M. 028
KUROKAWA T. 173
LAM H. 035
LEPORI B. 216
LEVAI R. 069
LINKE P. 202
LOCKHART J.A. 149
LOHVINENKO T.W. 195
LOWE D. 036
LUNSFORD R. 146
MACAULEY B. 037
MACHADO L.A. 245
MAKELA V. 075
MALONE J. 238
MARAZITI A. 218
MARTIKAINEN M. 079
MARUYAMA T. 172
MATSUOKA K. 183
MCATEE W. 241
MCKINLAY G. 038
MCLOUGHLAN R. 242
MCMULLEN M. 039
MELANDRI F. 040
MELGAREJO M. 120
MEOLI F. 215
MERING G. 203
MITCHELL K. 258
MONTEON R. 230
MOORE R. 141
MORAIS D. 244
MORENO G. 270
MORITZ S. 097
MORROW M.J. 041
MUDGE R. 255
MULLER K. 042
MUNOZ S. 107
MUROTA M. 180
MUSCAT T. 221
NATOLI C. 043
NEGISHI M. 175
NELSON J. 257
NERY M.D. 154
NETO V.F. 151
NOLLE M. 044
NOSAL I. 211
NOUSIAINEN M. 080
NUNES H. 271
OCENAS D. 204
OCHIAI T. 174
OKA Y. 188
OLESEN J.O. 045
OLSSEN S. 264
OTTO F. 096
PAGE B. 263
PARADOWSKI M. 115
PARKER J. 047
PATAK A. 135
PAYNE J. 262
PEDERSEN V.T. 121
POSZTOBANY K. 087
PRICE R. 243
QUAN H. 048
RADANOVIC V. 259
RAJALA R. 073
RAMBERG P. 074
RANNERIES 122
RAPAVY P. 205
RAPHAEL W. 235
RASMUSSEN A. 123
RAVISCH I. 106
RAWLINGS P. 049
RENDTEL I. 050
RENDTEL J. 051
RENNER G.K. 155
RIDDLE D. 052
RITZL F. 126
ROBLER S. 273
ROCHA E. 267
RODRIGUEZ G. 231
ROLDAN R. 232
RUDD I. 251
RUTLEY J. 260
SAARENPURO M. 072
SAJTZ A. 137
SAKATA Y. 191
SALAS J. 138
SALM H.R. 053
SANCHEZ A. 236
SANTANA E. 266
SASSI A. 217
SCHEMBRI A. 092
SCHREYER T. 103
SCHROETER T. 104
SCHUTT S. 254
SCLOVSKY L. 156
SEARS K. 142
SEARS P. 143
SEIFERT H. 102
SEIPELT H. 109
SENTDORDIOVA I. 214
SHANKLIN J. 124
SHAVER J. 150
SHEPHERD A. 054
SHIBU Y. 118
SIMPSON D. 253
SINGH B. 119
SKJAERAASEN O. 055
SOMMER C. 269
SPANYI P. 085
STACEY P. 056
STEPHAN C. 057
SULE G. 083
SULLIVAN S. 058
SWANN D. 059
SWAVELY M. 160
SZABO J. 212
SZABO S. 125
TABORI S. 136
TACHIHARA Y. 182
TAIBI R.J. 060
TAKACS R. 209
TAME J. 061
TARNAY K. 129
TEPEL S. 105
TEPLICZKY I. 081
TIZZARD K. 249
TOMIHIRO H. 170
TOTH J. 131
TREASSURE M. 197
TRINH N. 227
UEDA K. 247
UEDA M. 169
VALDENASSI E. 062
VALJUS P. 077
VELLA I. 093
VENTURA F. 090
VILLA R. 237
WAKE S. 166
WATERS B. 139
WHITNEY A. 063
WHITNEY J. 064
WIBLIN B. 065
WIRTANEN P. 078
WITZSCHEL H. 101
WITZSCHEL S. 099
WOOD J. 066
YABU Y. 167
YAKIWARA H. 178
YAMAGUCHI W. 111
ZALCIK M. 067
ZALLES R. 113
ZIMNIKOVAL P. 207
ZNASIK M. 206
ZSCHOCHE M. 100
ZUTHER O. 068
_______________________
Table C-IV: Visual
Observers Listed by
Identification Number
_______________________
Observer No.
_______________________
ALDRICH P.T. 001
ANDRESEN B. 002
ANDERSON C. 003
ANTHONY D. 004
ARLT R. 005
BARKAT S. 006
CAKE D. 007
CLAY M. 008
COCKERAM L. 009
COCKERAM M. 010
CZESCIK C. 011
DARVANN T. 012
DECONINCK M. 013
DIETEL F. 014
DOUGHTY S. 015
DURHAM D. 016
EVANS S. 017
FERDINANDO D. 018
FITZGERALD P. 019
GILROY J. 021
GOLDSMITH J. 022
GOODMAN D. 023
GRAY M. 024
KERR S. 025
KOCH B. 026
KOSCHACK R. 027
KRISTENSEN G.M. 028
HAAGH N. 029
HARNISCH T. 030
HILLESTAD T.E. 031
HINZ W. 032
JENKINSON C. 033
INWOOD N. 034
LAM H. 035
LOWE D. 036
MACAULEY B. 037
MCKINLAY G. 038
MCMULLEN M. 039
MELANDRI F. 040
MORROW M.J. 041
MULLER K. 042
NATOLI C. 043
NOLLE M. 044
OLESEN J.O. 045
PARKER J. 047
QUAN H. 048
RAWLINGS P. 049
RENDTEL I. 050
RENDTEL J. 051
RIDDLE D. 052
SALM H.R. 053
SHEPHERD A. 054
SKJAERAASEN O. 055
STACEY P. 056
STEPHAN C. 057
SULLIVAN S. 058
SWANN D. 059
TAIBI R.J. 060
TAME J. 061
VALDENASSI E. 062
WHITNEY A. 063
WHITNEY J. 064
WIBLIN B. 065
WOOD J. 066
ZALCIK M. 067
ZUTHER O. 068
LEVAI R. 069
DE ABREU E.R. 070
JAASKELAINEN P. 071
SAARENPURO M. 072
RAJALA R. 073
RAMBERG P. 074
MAKELA V. 075
HOTAKAINEN,M 076
VALJUS P. 077
WIRTANEN P. 078
MARTIKAINEN M. 079
NOUSIAINEN M. 080
TEPLICZKY I. 081
FARKAS E. 082
SULE G. 083
GYARMATI L. 084
SPANYI P. 085
FODOR A. 086
POSZTOBANY K. 087
FOLDESI F. 089
VENTURA F. 090
BALDACCHINO G. 091
SCHEMBRI A. 092
VELLA I. 093
BALDAUF P. 094
KAALZ A. 095
OTTO F. 096
MORITZ S. 097
KRAWIETZ A. 098
WITZSCHEL S. 099
ZSCHOCHE M. 100
WITZSCHEL H. 101
SEIFERT H. 102
SCHREYER T. 103
SCHROETER T. 104
TEPEL S. 105
RAVISCH I. 106
MUNOZ S. 107
KNOEFEL A. 108
SEIPELT H. 109
BUSSON A. 110
YAMAGUCHI W. 111
ESPINOZA E. 112
ZALLES R. 113
HAYS R. 114
PARADOWSKI M. 115
FROTA L.M. 116
CARLOS F. 117
SHIBU Y. 118
SINGH B. 119
MELGAREJO M. 120
PEDERSEN V.T. 121
RANNERIES 122
RASMUSSEN A. 123
SHANKLIN J. 124
SZABO S. 125
RITZL F. 126
CSABAI I. 127
HOLLOSY T. 128
TARNAY K. 129
DOMENY G. 130
TOTH J. 131
BERKO E. 132
HALMI G. 133
KESZTHELYI S. 134
PATAK A. 135
TABORI S. 136
SAJTZ A. 137
SALAS J. 138
WATERS B. 139
GOODKNECHT R. 140
MOORE R. 141
SEARS K. 142
SEARS P. 143
FETTIG S. 144
COOK A. 145
LUNSFORD R. 146
BOSCHAT M.E. 147
BARROW R. 148
LOCKHART J.A. 149
SHAVER J. 150
NETO V.F. 151
DALAVIA O.D. 152
DA SILVA L.A. 153
NERY M.D. 154
RENNER G.K. 155
SCLOVSKY L. 156
AZEVEDO C. 157
ADIB C.A. 158
ALMEIDA L.D. 159
SWAVELY M. 160
WAKE S. 166
YABU Y. 167
ITO O. 168
UEDA M. 169
TOMIHIRO H. 170
KEIICHI F. 171
MARUYAMA T. 172
KUROKAWA T. 173
OCHIAI T. 174
NEGISHI M. 175
HIROE T. 176
KAWASAKI Y. 177
YAKIWARA H. 178
FUJITA Y. 179
MUROTA M. 180
HARADA S. 181
TACHIHARA Y. 182
MATSUOKA K. 183
KITAHATA K. 184
AOTA T. 185
INOUE S. 186
INOUE M. 187
OKA Y. 188
HIRAGA E. 189
FUNANO K. 190
SAKATA Y. 191
DOHRMANN M. 192
GUHL K. 193
KADLCIK M. 194
LOHVINENKO T.W. 195
COWIE F. 196
TREASSURE M. 197
BALL J. 198
BURROWS J. 199
DOCKING G. 200
GHISOLFI E.S. 201
LINKE P. 202
MERING G. 203
OCENAS D. 204
RAPAVY P. 205
ZNASIK M. 206
ZIMNIKOVAL P. 207
BABNIC S. 208
TAKACS R. 209
COMOS G. 210
NOSAL I. 211
SZABO J. 212
DYMOVA G. 213
SENTDORDIOVA I. 214
MEOLI F. 215
LEPORI B. 216
SASSI A. 217
MARAZITI A. 218
AQUILINA J. 220
MUSCAT T. 221
ABELA S. 222
HARVEY N. 224
TRINH N. 227
CORONEOS M. 228
ALCARAZ D. 229
MONTEON R. 230
RODRIGUEZ G. 231
ROLDAN R. 232
ARCE M. 233
ARCE V. 234
RAPHAEL W. 235
SANCHEZ A. 236
VILLA R. 237
MALONE J. 238
CLARK M. 239
FOLEY C. 240
MCATEE W. 241
MCLOUGHLAN R. 242
PRICE R. 243
MORAIS D. 244
MACHADO L.A. 245
AZOFEIFA D.E. 246
UEDA K. 247
HASHIMOTO T. 248
TIZZARD K. 249
BEAZLEY I. 250
RUDD I. 251
SIMPSON D. 253
SCHUTT S. 254
MUDGE R. 255
NELSON J. 257
MITCHELL K. 258
RADANOVIC V. 259
RUTLEY J. 260
BROWN P. 261
PAYNE J. 262
PAGE B. 263
OLSSEN S. 264
ARAUJO P. 265
SANTANA E. 266
ROCHA E. 267
DE ARAUJO L. 268
SOMMER C. 269
MORENO G. 270
NUNES H. 271
FORTUNATO H. 272
ROBLER S. 273
BARATA P. 274
HINTON C. 275
_______________________
ATTACHMENT D: OBSERVATIONS
This attachment lists the results of the radar observations in Table D-I
and of the visual observations in Table D-II.
Table D-I. Radar observations
______________________________________________________________
Object Source Number File
of hours number
______________________________________________________________
Eta Aquarids 1984 Hajduk, Bratislava 70 900201
Hajduk, Bratislava 14 900202
Lindblad, Lund 60 900203
Babadzhanov, Dushanbe 192 900204
Babadzhanov, Dushanbe 189 900205
Orionids 1984 Hajduk, Bratislava 68 900206
Hajduk, Bratislava 11 900207
Cevolani, Budrio 205 900208
Lindblad, Lund 45 900209
Babadzhanov, Dushanbe 224 900210
Babadzhanov, Dushanbe 225 900211
Eta Aquarids 1985 McIntosh, Ottawa 165 900212
Lindblad, Lund 59 900213
Cevolani, Budrio 42 900214
Hajduk, Bratislava 83 900215
Hajduk, Bratislava 38 900216
Babadzhanov, Dushanbe 267 900217
Babadzhanov, Dushanbe 265 900218
Orionids 1985 McIntosh, Ottawa 216 900219
Lindblad, Lund 54 900220
Hajduk, Bratislava 36 900221
Hajduk, Bratislava 25 900222
Poole, Grahamstown 8 900223
Babadzhanov, Dushanbe 269 900224
Babadzhanov, Dushanbe 269 900225
Eta Aquarids 1986 McIntosh, Ottawa 168 900226
(comet plane McIntosh, Ottawa 10 900227
crossing)
Cevolani, Budrio 63 900228
Lindblad, Lund 54 900229
Poole, Grahamstown 18 900230
Hajduk, Bratislava 37 900231
Hajduk, Bratislava 28 900232
Babadzhanov, Dushanbe 269 900233
Babadzhanov, Dushanbe 270 900234
Orionids 1986 McIntosh, Ottawa 193 900235
(comet plane McIntosh, Ottawa 10 900236
crossing)
Hajduk, Bratislava 23 900237
Hajduk, Bratislava 12 900238
Poole, Grahamstown 20 900239
Cevolani, Budrio 131 900240
Babadzhanov, Dushanbe 258 900241
Babadzhanov, Dushanbe 258 900242
Eta Aquarids 1987 Poole, Grahamstown 19 900243
Babadzhanov, Dushanbe 225 900244
Babadzhanov, Dushanbe 195 900245
Orionids 1987 Poole, Grahamstown 20 900246
Babadzhanov, Dushanbe 222 900247
Babadzhanov, Dushanbe 239 900248
Eta Aquarids 1988 Poole, Grahamstown 17 900249
Orionids 1988 Poole, Grahamstown 20 900250
______________________________________________________________
Total 5878 50
______________________________________________________________
Table D-II. Visual Observations
____________________________________________________________
Eta Aquarids Orionids
____________________ ____________________ File
number
Year Number Year Number
of hours of hours
____________________________________________________________
1982 59 900251
1984 134 900252
1984 368 900253
1985 134 900254
1985 546 900255
1986 218 900256
1986 33 900257
1987 93 900258
1987 39 900259
____________________________________________________________
Totals 579 1045 9
Grand Total 1624
____________________________________________________________