Abstract

This senior project aims to design a system to detect the presence of Meteors depending on the reflected radio signal.

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Radio telescope provides a practical and economical alternative to optical telescope to detect the occurrence of unknown objects. We developed an inexpensive radio telescope to collect, focus and record the presence of a certain type of electromagnetic radiation.

We tested the project in Al-Jubaiha-Amman at coordinate’s 32°1’34″N 35°54’9″E, this location has a clear view with the horizon from the north direction

Table of Contents

 

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Acknowledgments

Abstract

Table of Contents

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List of Figures

Software Specification

Introduction

1.1 Overview

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1.2 What is Radio Telescope

1.3 Types of Radar

1.4 Radio Telescope vs. Optical Telescope

1.5 What is the Meteor

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1.6 Electromagnetic spectrum

1.7 Radio Waves Propagation

1.8 Experiments

1.8.1 AM Signals

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1.8.2 UHF signals

1.8.3 FM signals

1.9 system structure and motivation

Radio Telescope Hardware

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2.1 System Hardware

2.2 The Antenna

2.2.1 Yagi Antenna

2.2.2 Operation of the Yagi Antenna

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2.2.3 Yagi Antenna design

2.2.4 Yagi antenna simulation

2.3 FM Radio Receiver

2.4 Analog to Digital Converter (ADC)

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2.4.1 Function of the Analog Input Subsystem

2.5 Computer

Radio Telescope Software

3.1 The objective of radio telescope software

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3.1.1 Create a device object

3.1.2 Acquire Data

3.1.3 Logging Data

3.1.4 Trigger Types

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3.1.5 Trigger Delays

3.1.6 Logging data to Disk

3.2 Software Flow Chart

3.3 Software Codes

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Test and Results

4.1 Introduction

4.2 Observation

4.3 Results

4.4 Discussions

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Conclusions and Future Work

5.1 Conclusion

5.2 Future work

List of Figures

Figure 1. 1: Principle of Radio Telescope

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Figure 1. 2: Electromagnetic spectrum

Figure 1. 3: Reflection in Layer E

Figure 1. 4: AM signal propagation

Figure 2. 1: Radio Telescope Hardware…………………………………………………………11

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Figure 2. 2: The 3-Element Yagi Antenna……………………………………………………. 13

Figure 2. 3: Radiation pattern of Yagi Antenna in horizontal plan ………………….. 16

Figure 2. 4: Radiation pattern of Yagi Antenna in Vertical plan …………………….. 17

Figure 2. 5: view for Radiation pattern of Yagi Antenna ……………………………….. 18

Figure 2. 6 : Frequency Sweep Impedance Response ……………………………………. 19

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Figure 2. 7: RG-6 Coaxial cable …………………………………………………………………  20

Figure 2. 8: Analog to Digital Block Diagram ……………………………………………..  22

Figure 3. 1: Radio Telescope Software principle…………………………………………… 24

Figure 3. 2: Flow of Acquired Data…………………………………………………………….. 26

Figure 3. 3: Software Trigger……………………………………………………………………… 27

Figure 3. 4: Pre-triggering Delay………………………………………………………………..  27

Figure 3. 5: Logged Data in Memory or Disk………………………………………………. 28

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Figure 3. 6: Software Flow Chart……………………………………………………………….. 29

Figure 4. 1: Tests Histogram……………………………………………………………………… 32

Figure 4. 2: Test settings…………………………………………………………………………… 33

Figure 4. 3: Data Histogram ……………………………………………………………………… 33

Figure 4. 4: Data of all trigger during the first hour ……………………………………… 34

Figure 4. 5: Data of all trigger during the second hour………………………………….. 35

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Figure 4. 6: Data of all trigger during the third hour…………………………………….. 36

Figure 4. 7: Data of all trigger during the fourth hour…………………………………… 37

Figure 4. 8: Data of all trigger during the fifth hour……………………………………… 38

Figure 4. 9: Data of all trigger during the sixth hour…………………………………….. 38

Figure 4. 10: Data of all trigger during the seventh hour……………………………….. 39

Figure 4. 11: Voltage level of Triggers……………………………………………………….. 39

Software Specification

Our code was developed based on Data Acquisition Toolbox™ which provides functions for connecting MATLAB® to data acquisition hardware. The toolbox supports PC-compatible data acquisition hardware from multiple vendors, including Advantech, Measurement Computing, and National Instruments. The toolbox also supports Microsoft Windows® compatible sound cards. In addition, it is compatible with hardware from several data acquisition vendors via third-party adaptors

With the toolbox helped in configuring data acquisition hardware and reading data into MATLAB® and Simulink® for immediate analysis, also sending out data over analog and digital output channels provided by data acquisition hardware. The toolbox’s data acquisition software includes functions for controlling analog input, analog output and counter/timer.

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The toolbox provides common base properties that apply to all supported hardware, such as sample rate, trigger settings, and channel properties. These properties promote code reuse and reduce the need to change code when changing hardware, also data is analyzed acquired or saved for post-processing.

The legacy interface supports hardware from multiple vendors and all sound cards on 32-bit versions of MATLAB®, the legacy interface also supports voltage measurements of analog input, analog output, and digital I/O subsystems.

 

Chapter 1

Introduction

Introduction

1.1 Overview

Since using optical telescope requires atmosphere that is not cloudy or rainy also cannot be used during daylight, we designed a telescope to detect the Meteors without any constraints depending on radio wave rather than the optical wave as used in optical telescope.

The general principle of meteor observation in our design is illustrated in Figure 1.1 a radio receiver is located at a large distance from a transmitter at the same frequency. Direct radio contact is impossible due to the curvature of the Earth. When a meteor enters the atmosphere, its trail may reflect the radio waves from the transmitter to the receiver.

At the receiver end, where the signal of the transmitter is normally not received, the transmission at the presence of the meteor trail can be received for a moment. The radio waves reflections can last from a tenth of a second to a few minutes. The received signal characteristics are related to physical parameters of the meteoric event.

Figure 1. 1: Principle of Radio Telescope

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1.2 What is Radio Telescope

Radio telescope is an astronomical instrument consisting of a radio receiver and an antenna that is used to detect radio frequency radiation reflected by meteors .Because radio wavelengths are much longer than those of visible light, radio telescopes must be very large in order to attain the resolution of optical telescopes.

Radio telescopes vary widely, but they all have two basic components a large radio antenna and radio receiver. The sensitivity of radio telescope depends on the area and efficiency of the antenna.

1.3 Types of Radar

• Passive Radar: It’s a system that detects and track objects by processing reflections from non-cooperative sources of illumination in the environment, such as commercial broadcast and communications signals, for that there is no dedicated transmitter.

• Active radar: it’s a system that consist and control both a transmitter and receiver were usually located at the same site .It’s a technique of observing nearby objects by reflecting the transmitted signals off target objects and analyzing the echoes. This type can determine the distance to an object and the speed of the object too.

In our project we constructed a system that works as passive radar, because there is no dedicated transmitter and the reflections observed is coming from commercial broadcast.

1.4 Radio Telescope vs. Optical Telescope

Radio telescope and optical telescope both examine electromagnetic radiation originating from outside the Earth’s atmosphere. Where they differ is in the tools used to detect this radiation where in radio telescope its inexpensive compare to optical telescope its very expensive. And in the wavelength or frequency of the waves because radio waves are much longer than optical waves the radio telescopes must be much larger than optical telescopes.

As we said before radio telescope can works in cloudy or rainy day also during daylight and telescope does not require the observer to be in monitoring site during all the observation period.

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1.5 What is the Meteor

Meteors or shooting stars are the streaks of light produced when a meteoroid burns up in the Earth’s atmosphere. The meteoroids which produce the meteors are dust and rocks in space. If the meteor hits the ground, it is then called a meteorite and it will leave a hole in the ground.

1.6 Electromagnetic spectrum

The electromagnetic spectrum is the range of all possible frequencies of electromagnetic radiation.

Radio waves are a type of electromagnetic radiation with wavelengths in the electromagnetic spectrum longer than visible light as illustrated in figure 1.2. Have frequencies from 3 kHz to 300 GHz and the corresponding wavelengths are from 1 millimeter to 100 kilometers.

Figure 1. 2: Electromagnetic spectrum

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The table below gives detailed information about the frequency range, the length of waves for each band and some typical uses of that portion of the radio spectrum.

Band	Frequency	Wavelength	Some Uses
VLF	3 – 30 kHz	100 km – 10 km	Long range navigation and marine radio
LF	30 – 300 kHz	10 km – 1 km	Aeronautical and marine navigation
MF	300 kHz – 3 MHz	1 km – 100 m	AM radio  and radio telecommunication
HF	3 – 30 MHz	100 m – 10 m	Amateur radio bands, NRC time signal
VHF	30 – 300 MHz	10 m – 1 m	TV, FM, cordless phones, air traffic control
UHF	300 MHz – 3 GHz	1 m – 10 cm	UHF TV, satellite, air traffic radar, etc
SHF	3 – 30 GHz	10 cm – 1 cm	Mostly satellite TV and other satellites
EHF	30 – 300 GHz	1 cm – 1 mm	Remote sensing and other satellites

1.7 Radio Waves Propagation

The radio signals interact with the objects and the media on its way, this interaction causes the radio signals to be reflected, refracted or diffracted which leads this signal to change direction and reach areas that it would be impossible to be reached if the radio waves travelled in a direct path.

Most radio communication applications depend on the ionosphere region, since this region in the atmosphere enables radio communications signal to be reflected or more correctly refracted back to earth using sky wave.

Sky Wave

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The radio signals leave the Earth’s surface and travel towards the ionosphere where some of the signals are returned to Earth; these radio signals are called sky waves, in fact there are more than one layer inside the ionosphere that are responsible for the process of reflection.

1. Layer D

When radio signals leave the Earth’s surface and travel upward the first region of ionosphere that is called the D region; this region attenuates the signals as they pass through it.

The D region attenuates signals because the radio signals cause the free electrons in this region to vibrate. As they vibrate the electrons collide with molecules, at each collision there is a small loss of energy, With countless numbers of electrons vibrating, the amount of energy loss becomes noticeable and manifests itself as a reduction in the overall signal level.

The level of attenuation depends on the frequency because when frequency increases, the wavelength of the vibration shortens, and the number of collisions between the free electrons and gas molecules decreases. This means that low frequency signals are often prevented from reaching the higher regions except at night when the region disappears.

2. Layer E

Once a signal passes through the D layer, it enters E layer where the air density is very low .this means that when the free electrons are excited by radio signals and vibrate a fewer collisions occur.

Therefore the electrons are set again in motion by the radio signal, causing the signal to travel in medium where the density of electrons is high, this will cause the signal to get refracted from the area that has higher electron density, when the refracted signal reaches the earth it appears as a reflected signal.

Figure 1. 3: Reflection in Layer E

1.8 Trials

In our project we need a source of radiation to be available in most areas where the observation must be done and is easy to use:

1.8.1 AM Signals

SinceAM signals travel by reflection from the ionosphere as shown in figure 1.4.It was inapplicable to use it because we cannot determine if the signals are reflected from objects or from the ionosphere as the original signals propagate. It was hard to use this type in our project so we moved to a different type.

Figure 1. 4: AM signal propagation

1.8.2 UHF signals

We started our attempts using TV tuning, since this type of receiver is available in old equipment in the university, but we have faced problems in obtaining the data sheet of this type of tuner and the equipment needed to operate on this frequency “UHF”.

1.8.3 FM signals

Because of the difficulties that we faced using AM and UHF frequencies we moved to FM radio frequency this type of radiation require line of sight between transmitter and receiver to propagate in the normal situation and now it available everywhere.

Receiving radio wave from far away FM station is almost impossible due to the curvature of the Earth but when a meteor streaks through Earth’s atmosphere a part of its energy is released as light, the remainder is dispersed in a trail as ionized air, this electrified air will reflect the radio waves which are coming from commercial FM station. As a result, commercial radios are recommended to serve as a receiver.

When tuning the radio to a FM radio station from the location of observation, music or voices can be heard if a meteor passes between the transmitter (the radio station) and the receiver.

1.9 System structure and motivation

The aim of this project is to design a very simple system with the lowest expenses to detect the presence of meteors and connect to it a unidirectional antenna to cover only the area of observation where its propagation pattern is in one direction, then this antenna is connected to a FM radio receiver because the FM signals operate by line of sight and also the FM radio has better sound quality than AM radio.

 

Chapter 2

Radio Telescope Hardware

Radio Telescope Hardware

As explained previously, this project aims to detect meteors when it enters the atmosphere. The non-local FM radio signal will be reflected due to the occurrence of meteors. To achieve this objective our system must consist of two main parts:

• Hardware
• Software

2.1 System Hardware

The easiest way to observe meteors by radio is to use commercial FM radio and connect it to a Yagi antenna as shown in Figure 2.1 then try to find an empty frequency from 88-108 MHz, where you do not hear any kind of music or voice and is being used by a distant transmitter mostly a distant FM radio station about 500-2000 km away from your location. After selecting the best FM Radio receiver; took the audio signal as an analog input to the sound card ”ADC” in the computer through the microphone port using 3.5mm Jack cable in order to convert it to digital signal. In addition, we need method to recording data and analyze it.

Figure 2. 1: Radio Telescope Hardware

2.2 The Antenna

Antenna is an electromagnetic device that collects or emits radio waves. It consists of materials that conduct electricity arranged in such a way that it is in tune with the frequency of a radio signal, the antenna tuned to a particular frequency will resonate to a radio signal of the same frequency. When properly tuned an antenna will collect this energy and make it available to drive the amplifiers in a radio receiver.

For the detection of meteors we constructed and attached an antenna to the receiver to collect the radio waves that cannot be heard by the human ear.

2.2.1 Yagi Antenna

In our project we built a 3-element Yagi antenna, which is a useful form of RF antenna design and is widely used in applications where an RF antenna design is required to provide gain and directivity, as a result the optimum transmission and reception conditions can be obtained. It will efficiently collect the radiated energy of a distant FM radio station where its waves have been reflected by a meteor.

The Yagi antenna as shown in figure 2.2 is one of the most popular and widely used antennas because of its simplicity, low cost, directional radiation and relatively high gain. The design has a dipole as the driven element, furthermore parasitic elements are added which pick up power from the dipole and re-radiate it in such a manner that affects the properties of the RF antenna as a whole.

High gain is attained by the addition of parasitic elements positioned either in front or behind the driven element. These parasitic elements are called directors and reflectors depending on their lengths and positioning with respect to the driven element.

2.2.2 Operation of the Yagi Antenna

The parasitic elements of the Yagi antenna operate by re-radiating their signals in a slightly different phase to that of the driven element. In this way the signals are reinforced in some directions and cancelled out in others. It is found that the amplitude and phase of the current that is induced in the parasitic elements is dependent upon their length, the spacing between them and the dipole or driven element.

Figure 2. 2: The 3-Element Yagi Antenna

Using a parasitic element it is hard to have complete control over both the amplitude and phase of the currents in all the elements. This means that it is difficult to obtain complete cancellation in one direction. Nevertheless it is still possible to obtain a high degree of reinforcement in one direction with a high gain and a high degree of cancellation in the other direction to provide a good front to back ratio.

To obtain the required phase shift an element can be made either inductive or capacitive. If the parasitic element is made inductive it is found that the induced currents are in such a phase that they reflect the power away from the parasitic element, this causes the RF antenna to radiate more power away from it and this element is called a reflector. The parasitic element should be tuned below resonance by physically adding some inductance to the element in the form of a coil. Generally it is made about 5% longer than the driven element.

If the parasitic element is made capacitive it will be found that the induced currents are in such a phase that they direct the power radiated by the whole antenna in the direction of the parasitic element and this element is called a director. The parasitic element should be tuned above resonance by physically adding some capacitance to the element in the form of a capacitor or more commonly by making it about 5% shorter than the driven element.

2.2.3 Yagi Antenna design

As we discussed earlier, this radio telescope will operate at a very high frequency band and specifically at FM radio frequency band, this band starts at 88 MHz and ends at 108 MHz, to make our antenna operates effectively at any frequency within this band we will choose the center frequency and designed the antenna based on it.

set(AIVoice,’SampleRate’,s);    %Setting the sample rate for analog input object

ActualRate = get(AIVoice,’SampleRate’);

set(AIVoice,’Timeout’,time);      %Setting the timeout for analog input object

set(AIVoice,’SamplesPerTrigger’,ActualRate*duration );%setting specify number of samples to acquire for each trigger that occurs

set(AIVoice,’TriggerChannel’,chan); %setting the channel serving as trigger source

set(AIVoice,’TriggerType’,’Software’); %setting the trigger type

set(AIVoice,’TriggerCondition’,’Entering’);%Indicate required condition before trigger event occurs

set(AIVoice,’TriggerConditionValue’,[NF 1]); %Specify voltage value that must be satisfied before trigger executes

set(AIVoice,’TriggerRepeat’,inf); %Specify number of additional times to execute trigger

set(AIVoice,’TriggerDelayUnits’,’Samples’)

set(AIVoice,’TriggerDelay’,-s*60)

set(AIVoice,’BufferingMode’,’Auto’); %Specify how memory is allocated

set(AIVoice,’LoggingMode’,’Disk&memory’); %Specify destination for logged data

set(AIVoice,’LogFileName’,’Test.daq’)

set(AIVoice,’LogToDiskMode’,’Index’); %Specify whether data, events, and hardware information are saved to one or more disk files

%Initial Trigger

ao = analogoutput(‘winsound’);

addchannel(ao,1);

set(ao, ‘SampleRate’, 8000);

t = linspace(0,2*pi,16000);

y = sin(100000*t);

putdata(ao, y’);

set(ao, ‘TriggerType’, ‘Immediate’);

start(ao);

%Finish

start(AIVoice) %start analog device

%wait until required time finished then plot

z=get(AIVoice,’Timeout’);

pause(z)

returndata = ActualRate*duration*(AIVoice.TriggersExecuted);%get number of samples that executed

[d,t] = getdata(AIVoice,returndata); %Extract analog input data, time, and event information from data acquisition engine

plot(t,d) %plot data

xlabel(‘Time (sec.)’)

ylabel(‘Signal Level (Volts)’)

title(‘Data of all Triggers’)

grid on

stop(AIVoice)

disp(‘ ‘)

disp(‘ ‘)

disp(‘ ‘)

disp(‘ ‘)

disp(‘*************************************************************’)

disp(‘                   Result of Test     ‘)

disp(‘*************************************************************’)

disp(‘ ‘)

disp(‘ ‘)

%date and the time of start

abstime = AIVoice.InitialTriggerTime;

t = fix(abstime);

x=sprintf(‘%d/%d/%d    %d:%d:%d’,t(3),t(2),t(1),t(4),t(5),t(6));

disp([‘This test start at: ‘, num2str(x)]);

disp(‘ ‘)

NUMOFOBJ=AIVoice.TriggersExecuted-1;%-1 from initial triiger

disp([‘Number of unknown object that passed during this test : ‘, num2str(NUMOFOBJ)]);

disp(‘ ‘)

if NUMOFOBJ>0

disp(‘In these times…. ‘)

showdaqevents(AIVoice)

else

end

2. Result Code

clc

disp(‘*************************************’)

disp(‘  ‘)

disp(‘To preview all triggers waveform press 1’)

disp(‘If you want listen and plot a specific trigger press 2’)

disp(‘To show the time of all triggers press 3’)

disp(‘  ‘)

x=input(‘Press ?’);

disp(‘*************************************’)

if (x==1);

daqinfo = daqread(‘Test.daq’,’info’);

NumOfTrigger=daqinfo.ObjInfo.TriggersExecuted;

for t=2:NumOfTrigger

[data,time] = daqread(‘Test.daq’,’triggers’,[t]);

figure

plot(time,data)

title([‘Trigger number   ‘,num2str(t)])

xlabel(‘Time (sec.)’)

ylabel(‘Signal Level (Volts)’)

grid on

pause(0.1)

clf

end

end

if (x==2);

disp(‘  ‘)

trig=input(‘which trigger do you like to hear?’);

[data,time] = daqread(‘Test.daq’,’triggers’,[trig]);

plot(time,data)

title([‘Trigger number   ‘,num2str(trig)])

xlabel(‘Time (sec.)’)

ylabel(‘Signal Level (Volts)’)

grid on

wavwrite(data,8000,’trigger.wav’);

winopen trigger.wav

end

if (x==3)

daqinfo = daqread(‘Test.daq’,’info’);

showdaqevents(daqinfo.ObjInfo.EventLog)

end

Appendix B

The test results were as follows:

*************************************************************

Result of Test

*************************************************************

This test start at: 22/12/2012    23:57:48

Number of unknown object that passed during this test: 59

In these times….

1  Start               ( 23:56:04, 0 )

2  Trigger#1           ( 23:57:48, 0 )               Channel: [1]

3  Trigger#2           ( 00:01:50, 1936472 )         Channel: [1]

4  Trigger#3           ( 00:05:57, 3909289 )         Channel: [1]

5  Trigger#4           ( 00:10:04, 5886351 )         Channel: [1]

6  Trigger#5           ( 00:20:16, 10782530 )        Channel: [1]

7  Trigger#6           ( 00:22:21, 11784659 )        Channel: [1]

8  Trigger#7           ( 00:27:14, 14129142 )        Channel: [1]

9  Trigger#8           ( 00:34:38, 17677751 )        Channel: [1]

10 Trigger#9           ( 00:46:26, 23342322 )        Channel: [1]

11 Trigger#10          ( 00:48:18, 24239053 )        Channel: [1]

12 Trigger#11          ( 00:52:41, 26341504 )        Channel: [1]

13 Trigger#12          ( 00:56:09, 28009268 )        Channel: [1]

14 Trigger#13          ( 01:02:51, 31226688 )        Channel: [1]

15 Trigger#14          ( 01:06:16, 32865187 )        Channel: [1]

16 Trigger#15          ( 01:08:44, 34048394 )        Channel: [1]

17 Trigger#16          ( 01:19:54, 39404295 )        Channel: [1]

18 Trigger#17          ( 01:26:55, 42772564 )        Channel: [1]

19 Trigger#18          ( 01:34:20, 46339031 )        Channel: [1]

20 Trigger#19          ( 01:43:18, 50641526 )        Channel: [1]

21 Trigger#20          ( 01:51:08, 54399659 )        Channel: [1]

22 Trigger#21          ( 02:07:27, 62235086 )        Channel: [1]

23 Trigger#22          ( 02:15:20, 66011885 )        Channel: [1]

24 Trigger#23          ( 02:19:27, 67989761 )        Channel: [1]

25 Trigger#24          ( 02:29:49, 72964884 )        Channel: [1]

26 Trigger#25          ( 02:41:54, 78767407 )        Channel: [1]

27 Trigger#26          ( 02:45:34, 80526516 )        Channel: [1]

28 Trigger#27          ( 02:47:13, 81321046 )        Channel: [1]

29 Trigger#28          ( 02:52:06, 83662819 )        Channel: [1]

30 Trigger#29          ( 02:59:41, 87302387 )        Channel: [1]

31 Trigger#30          ( 03:17:04, 95651021 )        Channel: [1]

32 Trigger#31          ( 03:31:17, 102467870 )       Channel: [1]

33 Trigger#32          ( 03:44:59, 109044194 )       Channel: [1]

34 Trigger#33          ( 03:54:50, 113777882 )       Channel: [1]

35 Trigger#34          ( 04:07:09, 119687131 )       Channel: [1]

36 Trigger#35          ( 04:13:47, 122874414 )       Channel: [1]

37 Trigger#36          ( 04:21:47, 126712029 )       Channel: [1]

38 Trigger#37          ( 04:32:42, 131954650 )       Channel: [1]

39 Trigger#38          ( 04:45:47, 138234409 )       Channel: [1]

40 Trigger#39          ( 04:50:37, 140549149 )       Channel: [1]

41 Trigger#40          ( 05:03:06, 146546883 )       Channel: [1]

42 Trigger#41          ( 05:15:41, 152580194 )       Channel: [1]

43 Trigger#42          ( 05:25:58, 157519800 )       Channel: [1]

44 Trigger#43          ( 05:34:33, 161641318 )       Channel: [1]

45 Trigger#44          ( 05:37:23, 163002671 )       Channel: [1]

46 Trigger#45          ( 05:42:16, 165344243 )       Channel: [1]

47 Trigger#46          ( 05:48:35, 168375001 )       Channel: [1]

48 Trigger#47          ( 05:53:15, 170619001 )       Channel: [1]

49 Trigger#48          ( 06:03:01, 175305108 )       Channel: [1]

50 Trigger#49          ( 06:07:15, 177338399 )       Channel: [1]

51 Trigger#50          ( 06:14:41, 180903743 )       Channel: [1]

52 Trigger#51          ( 06:17:20, 182177875 )       Channel: [1]

53 Trigger#52          ( 06:23:12, 184994078 )       Channel: [1]

54 Trigger#53          ( 06:25:54, 186288002 )       Channel: [1]

55 Trigger#54          ( 06:27:38, 187115556 )       Channel: [1]

56 Trigger#55          ( 06:29:58, 188237493 )       Channel: [1]

57 Trigger#56          ( 06:33:23, 189877133 )       Channel: [1]

58 Trigger#57          ( 06:36:48, 191519490 )       Channel: [1]

59 Trigger#58          ( 06:40:43, 193400245 )       Channel: [1]

60 Trigger#59          ( 06:47:01, 196425137 )       Channel: [1]

61 Trigger#60          ( 06:53:38, 199596315 )       Channel: [1]

62 Stop                ( 06:56:04, 201600000 )

 

References

[1].  Radio Meteor Detection in Malaysia ,Z. Z. Abidin, Z. A. Ibrahim, S. F. F. Malim1 Z. Rosli, M. S. R. Hassan, M. A. A. Aziz, N. Noorazlan, A. S. M. SuhaimiVol.1, No.3, pp.53-56, Sep, 2011

[2]. Using FM radios to count meteors. Minton, R. B. & Lunsford, R., the Strolling Astronomer (ISSN 0039-2502), Vol. 44, No. 4, p. 9 – 16 (Autumn 2002)

[3]. Yagi-antenna design first edition by James L. Lawson.

[4]. Data acquisition toolbox user’s guide 2005–2012 by The MathWork

[5]. http://www.skyscan.ca/radio_meteor_detection.htm

[6]. http://www.jas.org.jo/radio.html

[7]. http://www.imo.net/radio/intro

[8]. http://www.radio-electronics.com/info/propagation/ionospheric/hf- propagation-basics.php

[9]. http://www.radio-electronics.com/info/propagation/meteor-scatter-burst-communications/meteors-trails-radio-signals.ph

[10]. http://www.radartutorial.eu/06.antennas/an08.en.html

[11]. http://www.radio-electronics.com/info/propagation/meteor-scatter-burst-communications/meteors-showers-types.php

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