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Monitoring of interplanetary and ionosphere scintillations at the frequency 111MHz

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. Plan of report:. About project About IPS observations

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Monitoring of interplanetary and ionosphere scintillations at the frequency 111MHz

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  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. Картинка нарисованная

  4. 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)

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

  6. Weak sources (2 kind of confusion):

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

  8. 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

  9. SNR and sensitivity

  10. 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 mIPPis 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 mIonare smaller than IPS indexes mIPPin the day time, and are comparable in the night timemIonmIPP. • 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

  11. 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

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