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(meteorobs) Radio Meteor Obs. Bull. Jan 1998: Quadrantids, no H-Bids (2 of 2)
12 " 1-2-0 6- 6- 2 10- 2- 1 57 " 30
13 " 4- 4- 1 4-10- 9 38 " 32
14 " 0-1-2 3- 4- 3 9- 3- 4 69 " 29
15 " 5- 4- 4 6- 8- 7 65 " 34
16 " 0-0-1 5- 4- 4 7- 5- 2 57 " 28
17 " 3- 4- 2 4- 5- 1 68 " 19
18 " 1- 1- 3 3- 8- 4 65 " 20
19 " 1-1-0 2- 1- 2 5- 1- 5 67 " 18
20 " 1-0-0 3- 5- 2 3- 6- 2 68 " 22
21 " 4- 4- 4 5-10- 7 41 " 34
22 " 1-0-0 1- 1- 5 2- 6-10 50 " 26
23 " 3- 2- 1 10- 5- 4 68 " 25
24 " 0- 1- 1 3- 1- 1 71 Lo- 07
25 " 2- 0- 1 0- 6- 9 77 None 18
26 " 4- 0- 3 3- 5- 6 48 " 21
27 " 2- 4- 3 8- 5-11 55 " 33
28 " 2- 3- 3 2- 3- 3 75 Lo 16
29 " 1- 2- 2 2-13- 8 32 None 28
30 " 7- 3- 3 7- 8- 1 69 " 29
31 1300-1400 0-1-0 7- 2- 1 8- 1- 2 68 None 22
Will Kelsey
---------------------------------------------------------------------------
Observer: Werfried Kuneth
Location: Ferndorf, Austria (13 37' E, 46 45' N)
Antenna: 3 element Yagi, direction south, elevation 65 deg
Receiver: IC-706 at 53.76060 MHz, CW-R mode, 500 Hz CW filter, fast AGC.
Transmitters: 1) 30 kW TV video carrier from Bari, Italy, distance 700 km,
direction south 2) a 30 kW TV video carrier from Sicilia,
Italy, distance 900 km, south. Both transmitters are processed
within the same 40 Hz virtual receiver channel.
Observing method: automatic setup using FFTDSP42t software by AF9Y to record
the audio signal. 20 channels of 2 Hz width are used for meteor
identification, pictures with interference, sporadic-E, E-layer
and FAI propagation are manually rejected.
All meteor counts below are corrected for a full hour observing time. If
the recording duration is 20-40 minutes, a dot is shown after the value.
Data for less than 20 minutes observing time are not shown here.
Counts of reflections longer than 6.5 seconds: assumed to be overdense.
| Dec 1997
UT| 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26
---+-----------------------------------------------------------------------
0| 8 11 4 6 9. 40 6 5 0 2 7 3 3 11 6 3 1 3
1| 4 5 6 5 28 0 1 0 0 3 1 6 7 5 5 4 3
2| 4 2 4 10 25 5 0 2 0 5 7 5 7 10 1 5 6
3| 1 2 9 2 11. 48 1 4 0 2 2 2 4 7 3 5 7 10
4| 5 4 4 4 8 35 0 2 4 1 5 1 0 6 8 6 7 4
5| 4 2 0. 7 6 28 2 2 1 1 6 1 2 10 5 1 3 4
6| 7 3 4 2 20. 20 3 0 0 2 6 5 7 7 5 4 4 5
7| 2 1 2 3 11 12 2 2 1 13 4 8 1 17 4 6 4 15
8| 1 2 4 8 3 11 3 3 1 8 4 3 2 12 5 6 6 0.
9| 4 0 3 4 4 7 4 4 1 9 5 3 3 17 3 5. 4.
10| 3 1 2 2 3 7 1 1 2 4 4. 7 5. 16. 0. 1
11| 6 1 0 1 4 2 1 0 7 4 4. 8 1 0. 3.
12| 3 0 3 1 4 0 3 0 3 4 0. 1 0. 2
13| 0 0 0 2 1 1 1 0 0 1 3 1 5 1 2 0
14| 1 1 1 1 3 0 0 0 1 3 1 0 1 2. 0 0
15| 1 0 0 1 0 2 2 3. 1 2 1 1 0. 2. 1
16| 0 0 0 0. 0 0. 0 0 0 1 5. 0. 3
17| 1 0 0 1 0 0 0 0. 1
18| 2 0 1 3 0 0 1 1 0 0 0
19| 0 2 2 8 0 2 0 1 1 1 0.
20| 1 1 3. 2 10 13. 0 0. 0. 1 5 1 0 0
21| 2 5 7 15 22 11 1 2 0 0 0 3 1 2 0 0
22| 6 15 13 45 14 5 0 2 1 5 3 3 0 1 1 1
23| 5 5. 7 29 68 10 1 3 1 2 7 6 6 1 3 1 2
---+-----------------------------------------------------------------------
UT| 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26
| Dec 1997
Notes:
. blank value means either few or no data available or interference.
There was no sporadic-E and no FAI propagation during Dec 1-26.
. Dec 13 and 14: Geminids meteor shower.
. Dec 22: Ursids meteor shower.
. Data from Dec 1 - 8 are available on request, but quite normal act.
. local time conversion: 1 hour ahead of UT (05h00 UTC is 06h00 local).
Werfried Kuneth
---------------------------------------------------------------------------
Observer : Kimio Maegawa JA9BOH
Transmitter : HAM beacon (JA6YBR) (50 W Morse coded, 50.017 MHz) by
Miyazaki-University Ham Club.
Antenna: 1 lambda crossed loop, Az Omnidirectional 20 m H
Location: Miyazaki city (131.43E, 31.82N) NE-SW path 650km
Receiver : FT655 with 600Hz IF filter
Sensitivity: -150 dBm or lower, detect 3 dB galaxy noise variation
Location: Ohno Observatory, Japan (136.5E, 36.0N) 180m ASL
Antenna: 8 element Yagi(12dBi) 12m above the ground with no elevation.
Observing method:Automatic Duty Cycle measurement every minute by Audimate
software by Mr. Mallama of AMS above -130 dBm threshold.
Notes:
. Duty Cycle Graph for Quadrantids 1998 can be found at
http://www.fukui-nct.ac.jp/~kmaegawa/hro/98quada.html
. Quadrantids peak occurred at around 06 to 08 JST on Jan 4.
(21h UT to 23h UT on Jan 3 1998) based on my observation.
The activity was better than those of Geminids and equal to Perseids
maximum on Aug 13, 1996.
. local time = JST = UT + 9 hours
Kimio Maegawa
---------------------------------------------------------------------------
Observer: Chikara Shimoda
Location: Asahi, Nagano, Japan (137 51' E, 36 07' N)
Frequency: 81.4 MHz
Transmitter Location: FM-Japan 81.3 MHz, 10 kW, distance 180 km
Antenna: 5 element Yagi directed to the zenith.
Receiver: AM-FM Tuner (TRIO KT-1100)
Observing method: Meteor echoes output from center-tuning meter were
recorded on a pen-recorder chart.
Jan | UT
1998 | 11 12 13 14 15 16 17 18 19 20 21 22 | *(1) **(2)
------+-------------------------------------------------+-----------
1 | 10 20 14 21 16 19 17 23 30 29 23 34 | 16.7 26.0
2 | 9 15 10 15 23 25 26 29 38 38 27 35 | 16.2 32.2
3 | 16 11 23 23 29 45 54 74 74 66 60 71 | 24.5 66.5
4 | 9 12 15 15 15 16 36 27 36 33 33 26 | 13.7 31.8
5 | 7 19 22 23 16 20 29 34 32 34 22 25 | 17.8 29.3
6 | 19 20 16 18 19 23 29 27 25 29 40 28 | 19.2 29.7
7 | 10 13 19 12 18 23 22 32 34 35 23 22 | 15.8 28.0
8 | 13 21 18 21 21 32 27 30 26 25 19 | 18.8 26.5
9 | 13 13 17 19 25 20 29 31 34 29 25 22 | 17.8 28.3
10 | 12 17 19 16 19 34 30 30 30 23 16 22 | 19.5 25.2
11 | 11 20 13 16 18 20 30 27 26 22 20 19 | 16.3 24.0
12 | 13 13 14 22 11 22 17 25 21 29 24 23 | 15.8 23.2
13 | 9 15 18 21 26 17 32 25 32 24 21 19 | 17.7 25.5
14 | 7 12 25 25 29 30 36 27 18 20 | 17.3 26.7
15 | 12 12 13 29 15 23 29 32 16 18 26 10 | 17.3 21.8
16 | 7 14 18 25 20 22 31 32 22 26 22 14 | 17.7 24.5
17 | 11 14 14 11 19 28 22 30 22 26 25 20 | 16.2 24.2
18 | 20 17 17 19 21 24 14 27 21 18 26 | 19.7 21.2
19 | 10 12 25 25 22 21 29 24 29 32 22 26 | 19.2 27.0
20 | 7 13 17 15 21 20 26 35 21 28 18 19 | 15.5 24.5
21 | 6 17 16 26 20 19 18 26 23 15 19 9 | 17.3 18.3
22 | 12 18 20 20 19 27 19 26 16 24 23 18 | 19.3 21.0
23 | 7 14 19 16 18 21 24 27 18 20 20 14 | 15.8 20.5
24 | 8 18 23 16 26 27 29 26 23 19 | 16.3 25.0
25 | 10 13 19 17 13 23 21 26 24 25 | 15.8 24.0
26 | 12 21 19 28 23 22 20 25 21 24 20 19 | 20.8 21.5
27 | 8 16 15 20 17 26 18 21 25 16 21 19 | 17.0 20.0
28 | 11 17 18 21 20 25 24 23 29 23 20 16 | 18.7 22.5
29 | 9 21 24 19 23 15 29 20 22 16 20 20 | 18.5 21.2
30 | 8 12 13 15 25 23 31 21 15 17 24 15 | 16.0 20.5
31 | 13 9 17 16 13 20 25 25 26 18 22 15 | 14.7 21.8
------+-------------------------------------------------+-----------
1998 | 11 12 13 14 15 16 17 18 19 20 21 22 | *(1) **(2)
Jan | UT
* (1) average hourly rate between 11h -17h UT
**(2) average hourly rate between 17h -23h UT
. local time = JST = UT + 9 hours
Chikara Shimoda
---------------------------------------------------------------------------
Observer: Ilkka Yrjola
Location: Finland (26 35' E, 60 54' N)
Frequency: 87.360 MHz
Receiver: Salora SRP-22 modified, narrow band FM (B=15 kHz).
detected signal level >-122 dBm.
FM detection, no pulse noise rejection required.
Antenna: 2 element Yagi with 4 dBd gain to SW, azimuth 45 deg (SW)
Data sampling system: threshold triggering, sampling rate 64 ms.
Computer logs total hourly elapsed reflection time, number of
threshold crossings for the hour, the longest time the signal was
continuously above detection level for the hour.
Data stored in the Compact MS-Soft format. Software for viewing
available from FTP.FUNET.FI pub/ham/vhf-work/mssoft43.zip (420 K).
You can download the V5.0 software package from my homepage
www.sci.fi/~oh5iy
Meteor counts in one hour intervals starting at:
Quadrantids 1998
UT | 02 Jan 03 Jan 04 Jan 05 Jan
----+----------------------------------
0 | 294 301 426 195
1 | 293 302 449 251
2 | 346 352 617 261
3 | 294 431 574 289
4 | 394 471 481 268
5 | 288 481 366 210
6 | 257 384 298 255
7 | 309 472 272 235
8 | 227 360 295 186
9 | 449 484 225 216
10 | 513 811 307 215
11 | 411 907 278 252
12 | 366 810 295 202
13 | 324 774 253 205
14 | 224 683 174 172
15 | 184 592 140 137
16 | 233 563 106 124
17 | 195 488 154 116
18 | 173 464 171 104
19 | 203 548 161 148
20 | 246 634 185 192
21 | 274 633 200 188
22 | 355 906 226 190
23 | 287 545 209 168
----+----------------------------------
UT | 02 Jan 03 Jan 04 Jan 05 Jan
Ilkka Yrjola
---------------------------------------------------------------------------
Observer : W.T. Zanstra
Location : Appingedam, Netherlands (6 51' E, 53 19' N)
Frequency: 72.11 MHz
Transmitter Location:
Wroclaw (16 43' E, 50 52' N), Poland, 135 kW, distance 735 km
Antenna : Yagi, 5 elements, geographical azimuth 108 deg (ESE),
elevation 14 deg
Receiver : Bearcat UBC 177XLT Scanning Radio, sensitivity 0.3 uV
Observing method: listening
Forward scatter observations of Hale-Boppids and Quadrantids in
January 1998.
Raw counts of reflections, corrected for dead time, during one
hour intervals starting at:
| January 1998 | mean sporadic background
UT | 02 03 04 | during 1995 and 1996
----+------------------------------------------------
00 | 40 40 | 81
01 | 21 | 86
02 | 31 | 90
03 | 36 | 92
-----------------------------------------------------
09 | 28 | 73
10 | 33 | 67
11 | 32 | 60
12 | 56 | 52
13 | 52 | 46
14 | 61 | 42
15 | 49 | 39
16 | 43 | 39
17 | 31 | 40
18 | 60 | 44
19 | 37 | 50
20 | 49 | 56
21 | 34 54 | 62
22 | 23 | 68
23 | 24 61 | 75
----+-----------------------------------------------
Notes:
. the reason for the low rate of Hale-Boppids and Quadrantids,
including sporadics, is an overall decrease of reflections of
50-70 percent. Control counts until January 13 confirm this decrease.
Wim Zanstra / via Ton Schoenmaker
2. ANNOUNCEMENT
Further to the observations of Wim Zanstra, Ton Schoenmaker communicates that
during his observation runs between Jan 1-3 1998, he noticed a sudden
decrease in number of reflections on Jan 1 at precisely 23h00 UT. This was a
permanent decrease, lasting the next two days. The frequency was 72.11 MHz of
Wroclaw in Poland.
"I suppose that Wroclaw stopped (or considerably reduced the power of) its
transmissions, and that the remaining reflections are coming from other
stations at almost this frequency. Probably this is related to the switch in
Poland from the 66-73 MHz to the 88-108 MHz FM band".
3. ERRATUM
Erratum in RMOB9711 (No. 52): heading of the third table of Leonid
observations of Peter Bus:
"Total reflection time of long-duration reflections > 20 s
in seconds during one hour starting at UT:"
read:
"Total reflection time of long-duration reflections > 7 s
in seconds during one hour starting at UT:"
4. ABOUT THE RMOB
The RMOB is an independent initiative of some workers in the field of radio
meteor scatter observations and data reduction. It started in August 1993 in
order to spread rapidly the Perseid results via E-mail. Since then, it has
appeared monthly, and it has gradually been expanded. In regularly publishing
summaries of observations, potential radio observers are kept up to date of
existing installations, possibilities and limitations of radio meteor
observations. In the long run, there should be sufficient observing stations
to cover the whole globe, allowing to detect stream outbursts which may
remain unnoticed visually.
RMOB contains typically: summaries of recent observations, equipment data,
first results of stream activity by radio methods, relations between radio
and optical meteors, references to other publications in the field of meteor
astronomy and radio scatter techniques, announcements of meetings, short
questions and answers, non-commercial (second hand) sale of radio equipment,
available software.
Contributors are mentioned, and interested persons are asked to contact them
directly.
RMOB can be copied freely in unabridged and unmodified form. Extracts should
indicate the source (Radio Meteor Obs Bulletin, month and year).
If you want to subscribe (or un-subscribe) to the E-mail distribution list,
please send a message to C. Steyaert.
Those not having access to E-mail can obtain a printed copy free of charge
from J. Van Wassenhove (current or back-issues).
5. CONTRIBUTORS / USEFUL ADDRESSES
Enric Fraile Algeciras (EA3BTZ)
Frederic Corominas 58, Torrelles de llobregat, E-08629 Barcelona
E-mail: EA3BTZ@mx3.redestb.es
http://www.redestb.es/personal/ea3btz (in Spanish)
Eisse Pieter Bus
Groningen, Netherlands
E-mail: epbus@wxsdot nl
Maurice De Meyere
Hullekensstraat 24, B-9831 Deurle, Belgium
tel: +32 (9) 282 35 26
Call: ON4NU, packet: on4nu@on1ced
E-mail: via Chris Steyaert
University of Ghent, Astronomical Observatory
Krijgslaan 281(S9), B-9000 Gent, Belgium
E-mail contact: Paul.Vauterin@omadot be, Pierredot deGroote@rug.acdot be
Ou Yang Tian Jing
Wu Han,Hu Bei, P.R. of China
E-mail: via jxpsky@neasedot net
H. W. Kelsey, A.L.P.O.
Santa Maria, CA, USA
E-mail: 73073.1464@compuserve.com
Werfried Kuneth
Ferndorf, Austria
Call: OE8FNK, packet: OE8FNK@OE8XPK.#CAR.AUT.EU
E-mail: kuneth@net4you.co.at
Kimio Maegawa
Fukui National College of Technology, Electro-Information Course
Geshi, Sabae Fukui 916 JAPAN
Call:JA9BOH,JA9YDB
E-mail: kmaegawa@fukui-nct.ac.jp and/or HAG00032@niftyserve.or.jp
http://www.fukui-nct.ac.jp/~kmaegawa/hro
Alastair McBeath
IMO: International Meteor Organization
12A Prior's Walk, Morpeth, Northumberland, NE61 2RF, England, U.K.
E-mail: via Chris Steyaert
Chikara Shimoda
178, Hario, Asahi-mura, Higashitikuma-gun Nagano, Japan
Fax: +81-263-99-3532
E-mail: c-shimo@mtd.biglobe.ne.jp
Chris Steyaert, VVS
Kruisven 66, B-2400 Mol, Belgium
tel: +32 (14) 31 51 04
E-mail: steyaert@vvs.innetdot be
Compuserve: 72650,3513
Jeroen Van Wassenhove, VVS
's Gravenstraat 66, B-9810 Nazareth, Belgium
tel: +32 (9) 385 61 09
E-mail: 100101.734@compuserve.com
Ilkka Yrjola
Jukolantie 16, FIN-45740 Kuusankoski, Finland
E-mail: upm20.ky.yrjolil@elvi.vtkk.fi
http://www.sci.fi/~oh5iy/
Call: OH5IY, packet radio: OH5IY@OH5RBG.#KVL.FIN.EU
W.T. Zanstra
Spijkerlaan 13, 9903 BB Appingedam, Netherlands
tel: +31 (0)596 625617
E-mail: via tonsch@nfradot nl
--
Christian Steyaert (RMOB9801) 7 February 1998
--