M E T E O R M E T E O R SS

VSA 2004.

Members: Izidor PelajićTamara Marić Anita Stjepanović

Teamleader :Tomislav Jurkić

GOALSGOALS

• Detecting and Detecting and recording meteorsrecording meteors using using video, visual, radio, VLF and ULF methodvideo, visual, radio, VLF and ULF method

• Photometry and light curve determination Photometry and light curve determination

• Video, radio and visual ZHR Video, radio and visual ZHR (zenithal hourly (zenithal hourly rate)rate) determination determination

• Comparing data from ULF, VLF and video Comparing data from ULF, VLF and video recordingrecording

VSA 2004.

The elements of The elements of visual observingvisual observing

Perseid meteor streamPerseid meteor stream

AActivity period : ctivity period : 17.7-24.8.17.7-24.8.

MMaximum: aximum:

11. 8. 21h11. 8. 21h UT (predicted by Lytinnen) UT (predicted by Lytinnen)

12. 8. 11h12. 8. 11h UT (regular) UT (regular)

Swift-Tuttle comet

Video

CAMERA

GRAPHICCARD

ELECTRO METER

CONDUCTING BALL

VOLTAGE FOLLOWER

FILTER

OSCILOSCOPE

YAGI ANTENNA

RECEIVER

FFT ANALYSIS

ANTENNA

AMPLIFIER

RADIOULF VLF

FFT ANALYSIS

C O M P U T E R

VIDEO OBSERVATION

½” CCD Camera WATEC½” CCD Camera WATEC

minimum ilumination 0.0003 luxminimum ilumination 0.0003 lux

limiting magnitude: 3,5limiting magnitude: 3,5

RADIO OBSERVATION

Forward scattering methodForward scattering method

• radio signalradio signal from from distant emitter distant emitter below horizon is below horizon is not received not received normally normally

• when meteor when meteor passes, it forms passes, it forms plasma trail and plasma trail and radio signal is radio signal is reflected and reflected and detected in detected in receiverreceiver

RADIO EQUIPMENT

PCR1000 receiverPCR1000 receiver

USB mode, 3 kHz USB mode, 3 kHz bandwidthbandwidth

Yagi antennaYagi antenna

Frequency: 62,1888 MHzFrequency: 62,1888 MHz

Emitter: Flensburg (1300 km)Emitter: Flensburg (1300 km)

ULF observation (below 50 Hz)

VOLTAGE FOLLOWER

FILTER

ELECTROMETER

VLF observation

VLF RECEIVER

Frequency: 1 kHz

FFT ANALYSIS

FFT – fast Fourier FFT – fast Fourier transformtransform

AMPLITUDE

FREQUENCY

PHOTOMETRY

• 32 processed meteors• 196 recorded meteors in 5 nights

• Photometry using Astro Image 2.0• Measurement was done using 3x3 pixel aparture and mean pixel value

ZHR - total

ZHR - maximum

PHOTOMETRIC TYPES

t (ms)t (ms)

pixel value pixel value

Type 1 Type 2

t (ms)

pixel value

Type 3

Distribution of meteor curves type

Type 1

Type 2

Type 3

FIREBALL – video

t (ms)

FIREBALL LIGHT CURVE

pixel value

t (ms)

FIREBALL – radio and ULF

ULF – signal

Duration: 9:30 min

Radio signal and spectar Duration: 3:30 min

CONCLUSIONCONCLUSION

• We recorded 196 meteors and processed 32 of them• Radio, visual, and video ZHR measurements correspond very well with IMO measurements• We found first predicted maximum at 139.45 solar longitude and at 139.9 solar longitude (regular maximum)• We found out that the most meteors are type 2 – 47%• We found possible ULF signal from bright fireball with video and radio record