1 / 25

Ionospheric-magnetospheric VLF Wave Propagation:

Ionospheric-magnetospheric VLF Wave Propagation: RPI/IMAGE-HAARP Correlative Study. V. Paznukhov, B. Reinisch, G. Sales, P. Song, G. Khmyrov Center for Atmospheric Research University of Massachusetts Lowell P. Kossey Air Force Research Laboratory. Objectives.

michon
Télécharger la présentation

Ionospheric-magnetospheric VLF Wave Propagation:

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Ionospheric-magnetospheric VLF Wave Propagation: RPI/IMAGE-HAARP Correlative Study V. Paznukhov, B. Reinisch, G. Sales, P. Song, G. Khmyrov Center for Atmospheric Research University of Massachusetts Lowell P. Kossey Air Force Research Laboratory

  2. Objectives • Use RPI/IMAGE to monitor the global network of VLF transmitters. • Study the power and effective spatial scales of the propagating whistler waves in magnetosphere. • Assess the effects of the waves to the radiation belt particles.

  3. Radiation belt energetic electron lifetimes (after Abel and Thorne, 1998) C: coulomb H: hiss W: lightning whistler VLF: ground transmitters Precipitation lifetime (days) L-shell

  4. Worldwide Map of Active VLF Stations JXN-16.4 HAARP GQD-19.6 DHO-23.4 GBR-16.0 HWU-18.3, 20.9, 21.7 ICV-20.27 NML-25.2 NAA-24.0 TBB-26.7 NLK-24.8 3SA-20.6 JJI-22.2 VTX3-18.2 PWB-25.0 NWC-19.8 VL3-13.0

  5. IMAGE Magnetic Field Footprints 70 0600 UT 1400 UT 2300 UT 60 0056 UT 1600 UT February 14/15 0424 UT NLK 50 March 26 April 4 NAA GEO Latitude, deg 40 0034 UT 1544 UT 30 0438 UT year 2001 20 210 240 270 300 330 GEO Longitude, deg Maine, NAA 24.0 kHz (44.5 N, 291 E) Seattle, NLK 24.8 kHz (48.0 N, 238 E)

  6. Example of dynamic spectrum Seattle, NLK 24.8

  7. Example of dynamic spectrum Seattle, NLK 24.8

  8. Example of dynamic spectrum Maine, NAA 24.0

  9. Observations of ground based VLF stations NAA 24 kHz NLK 24.8 kHz

  10. 24.8 kHz (NLK station) and 27.4 kHz (noise) signal comparison 27.4 kHz NLK 24.8 kHz

  11. 24.0 kHz (NAA station) and 27.4 kHz (noise) signal comparison 27.4 kHz NAA 24.0 kHz

  12. Observations of NLK station NLK 24.8 kHz NLK 24.8 kHz

  13. Observations of NAA station NAA 24.0 kHz NAA 24.0 kHz

  14. Observations of NAA station NAA 24.0 kHz NAA 24.0 kHz

  15. HAARP-RPI Transmission Experiment • Spring 2001 Campaign:March 18 to April 7, 2001. • HAARP was transmitting amplitude modulated HF signals in order to produce VLF plasma waves using the so-called Polar Electrojet Antenna. • RPI was set to receive the HAARP transmissions in both fixed frequencies and dynamic spectra. • HAARP heater transmitted 3.2 MHz signal modulated with 13 kHz sine wave. • During the experiments, the modulation frequency wasalternatingly switched on and off in order for RPI to distinguish HAARP signals from background noise.

  16. Geomagnetic Environment of HAARP-RPI Experiments 2001

  17. HAARP Spring 2001 Campaign HAARP dayside path nightside path 03/24 HAARP HAARP Program 23

  18. March 24, 2001 Dynamic Spectra measurements Amplitude, nV/m

  19. March 24, 2001 fixed frequency measurements Amplitude, dB

  20. Summary • Whistler-mode radio waves originated from two ground-based VLF transmitters were detected by the RPI instrument. • Observed signal-to-noise ratio was of the order of 20 dB. • The observed VLF signal region was smaller during the dayside measurements than during the nightside ones. • In the HAARP-RPI experiments, • fixed frequency measurements showed ambiguous signals. • indication was found in the dynamic spectra mode of observation during a geomagnetically quiet period. • evidence for the timing was ambiguous.

  21. Objective Using the available global network of VLF transmitters, we monitor the occurrence of whistler-mode signals received with the RPI instrument onboard of IMAGE satellite. The receiving mode is the DYNAMIC SPECTRA sweeping over the frequency band from 3kHz to 1MHz every 3 or 4 minutes. In the VLF band the frequency resolution is ~ 400 Hz. Expected bandwidth of the VLF signals is of the order of a few hundred hertz. Identified 21 stations from 13 kHz to 27 kHz with L-shells ranging from 1.11 to 5.24. Ten of these stations have high radiated power: 200 kW to 1 MW.

  22. Radiation belt energetic electron lifetimes (after Abel and Thorne, 1998)

  23. HAARP Spring 2001 Campaign nightside path dayside path Program 49

More Related