1. M E T E O R S VSA 2004. Members: Izidor Pelajić Tamara Marić Anita Stjepanović Teamleader : Tomislav Jurkić

2. GOALS Detecting and recording meteors using video, visual, radio, VLF and ULF method Detecting and recording meteors using video, visual, radio, VLF and ULF method Photometry and light curve determination Photometry and light curve determination Video, radio and visual ZHR (zenithal hourly rate) determination Video, radio and visual ZHR (zenithal hourly rate) determination Comparing data from ULF, VLF and video recording Comparing data from ULF, VLF and video recording VSA 2004.

3. The elements of visual observing  Perseid meteor stream  Perseid meteor stream  Activity period : 17.7-24.8.  Activity period : 17.7-24.8.  Maximum: 11. 8. 21h UT (predicted by Lytinnen) 11. 8. 21h UT (predicted by Lytinnen) 12. 8. 11h UT (regular) 12. 8. 11h UT (regular) Swift-Tuttle comet

4. Video CAMERA GRAPHIC CARD ELECTRO METER CONDUCTING BALL VOLTAGE FOLLOWER FILTER OSCILOSCOPE YAGI ANTENNA RECEIVER FFT ANALYSIS ANTENNA AMPLIFIER RADIOULFVLF FFT ANALYSIS C O M P U T E R

5. VIDEO OBSERVATION ½” CCD Camera WATEC minimum ilumination 0.0003 lux limiting magnitude: 3,5

6. RADIO OBSERVATION Forward scattering method radio signal from distant emitter below horizon is not received normally radio signal from distant emitter below horizon is not received normally when meteor passes, it forms plasma trail and radio signal is reflected and detected in receiver when meteor passes, it forms plasma trail and radio signal is reflected and detected in receiver

7. RADIO EQUIPMENT PCR1000 receiver USB mode, 3 kHz bandwidth Yagi antenna Frequency: 62,1888 MHz Emitter: Flensburg (1300 km)

8. ULF observation (below 50 Hz) VOLTAGE FOLLOWER FILTER ELECTROMETER

9. VLF observation VLF RECEIVER Frequency: 1 kHz

10. FFT ANALYSIS FFT – fast Fourier transform AMPLITUDE FREQUENCY

11. 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

12. ZHR - total

13. ZHR - maximum

14. PHOTOMETRIC TYPES t (ms) pixel value Type 1 Type 2

15. t (ms) pixel value Type 3 Distribution of meteor curves type

16. Type 1

17. Type 2

18. Type 3

19. FIREBALL – video

20. t (ms) FIREBALL LIGHT CURVE pixel value t (ms)

21. FIREBALL – radio and ULF ULF – signal Duration: 9:30 min Radio signal and spectar Duration: 3:30 min

22. CONCLUSION 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