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Ionospheric responses to the particular solar events

Ionospheric responses to the particular solar events. Zby š ek Mo š na 1,2 , Petra Š auli 1 , K. Georgieva 3 1- Institute of Atmospheric Physics ASCR, Prague, Czech Republic 2- Department of Surface and Plasma Science, Charles University, Prague, Czech Republic

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Ionospheric responses to the particular solar events

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  1. Ionospheric responses to the particular solar events Zbyšek Mošna1,2, Petra Šauli1 , K. Georgieva3 1- Institute of Atmospheric Physics ASCR, Prague, Czech Republic 2- Department of Surface and Plasma Science, Charles University, Prague, Czech Republic 3- Solar-Terrestrial Influences Laboratory, BAS, Bulgaria

  2. Solar events • Three events from year 2004 • High Speed Solar Stream (HSS, Mar 09) • Magnetic Cloud with rightward rotation of magnetic field (MC R, Feb 11) • Magnetic Cloud with leftward rotation (MC L, Nov 07)

  3. 2004 Mar. 09 – HSS Magnetic field Velocity of SW B vx Bx vy By vz Bz 7 9 11 13 day day 7 9 11 13

  4. 2004 Feb. 11 - Magnetic Cloud R Magnetic field Velocity of SW B vx Bx vy By vz Bz 11 14 12 13 day 11 14 12 13 day

  5. 2004 Nov.07 - Magnetic Cloud L Magnetic field Velocity of SW Bx vx vy By vz Bz 7 8 9 10 7 day 8 9 10 day

  6. Geomagnetic response in Dst Similar values of Dst drop The strongest response for MC L

  7. Ionospheric vertical sounding (1) Quiet ionogram - Pruhonice observatory Mar. 11, 2004 (km) 1000 800 Plasma frequency profile 600 400 F2 200 h’F2 foF2 (MHz) 8 4 6 2 Analyzed data: h’F2, foF2, plasma frequency profile 9 days for each event (4 days before are reference,15 min resolution)

  8. Disturbed ionogram – Pruhonice observatory Feb. 12 2004 (km) 800 600 400 200 4 6 2 8 (MHz) Ionospheric vertical sounding (2) 1000 Problems: splitting, spread, vanishing, blanketing…

  9. Diurnal course of foF2 and h’F2 after HSS MHz foF2 10 8 6 4 2 km h’F2 400 200 6 10 12 4 8 14 day

  10. Scalogram – time evolution of the plasma frequencies profiles after HSS MHz km 8 400 6 4 200 4 6 8 Passing of Traveling Ionospheric Disturbance (TID)

  11. Diurnal course of foF2 and h’F2 after MC R MHz foF2 10 8 6 4 2 km h’F2 400 200 14 16 10 12 8 day

  12. Scalogram – time evolution of the plasma frequencies profiles after MC R MHz 8 6 4 2 14 16 10 12 8 day Oscillations – wave-like structures remain several days – AGW with source in the midlatitudes

  13. Diurnal course of foF2 and h’F2 after MC L MHz foF2 10 8 6 4 2 km h’F2 400 200 4 6 8 10 12 14 day

  14. Scalogram – time evolution of the plasma frequencies profiles after MC L MHz 8 6 200 4 2 4 6 8 10 12 14 day

  15. Conclusion • Similar and high response to the solar events for several days in case of HSS and MC L (although very different Dst) • HSS, MC L: Decrease of foF2 and plasma frequencies in the height profile and increase in h’F2 • Oscillations of h’F2 after passing the TID • Wave-like structures with the source in midlatitudes • MC R: No significant change in mean values of daily ionospheric parametres, decrease in night foF2, oscillations of the h’F2 and in plasma frequencies profile

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