1. Monitoring of interplanetary and ionosphere scintillations at the frequency 111MHz S.A.Tyul’bashev, V.I.Shishov, I.V.Chashei, I.A.Subaev Pushchino Radio Astronomy Observatory (PRAO ASC LPI) Aberystwyth - 2009

2. Plan of report: About project About IPS observations Sensitivity of observations Results Conclusion

3. Scintillations

4. Картинка нарисованная

5. Monitoring of interplanetary and ionospheric scintillations give us possibility to find the sizes of coronal mass ejection (CME) and the velocity of CME Optimal interplanetary scintillations (frequency 100MHz) have been observed at scales 0.3a.u. (20 degrees from sun) before 1a.u. (60 degrees)

6. Different methods of sun activity estimations Strong sources (the problem of angular size of compact components):

7. Weak sources (2 kind of confusion):

8. Very weak sources (confusion of compact sources). averaging in boxes

10. Observations: Large Phased Array Affective area 20000-25000m^2 111MHz; τ=0.1s; bandwidth=600kHz; 1.5MHz Data of observations 2003–2006 (irregular observations) 2007– 2008 (monitoring programme) 8 or 16 beams

19. SNR and sensitivity

21. Results: The method of simultaneous IPS and ISS monitoring is used for investigation of CME; The dependence of IPS index on day time was found: the maximal value of m IPP is about 0.3, the minimal value in the night time is about 0.1. Weak variations of IPS index from day to day were found as for day time so for night time. ISS indexes m Ion are smaller than IPS indexes m IPP in the day time, and are comparable in the night time m Ion  m IPP. During the years 2006-2008 the state of interplanetary plasma and ionosphere was comparably quiet. On October 2008 (deep minimum of solar activity) we observed very strong ellipticity

22. Conclusion and plans: The coefficient of asymmetry give us good opportunity to investigate sun activity (CME) at small angular scales (now 3 square degrees) 128 beams (64 degrees on the sky), which we will use for monitoring in 2011, will give us good opportunity of CME investigation. We plan that sensitivity IPS observations will be equivalent the density of scintillating sources 1 source per 1 square degrees in 2011