Monitoring of interplanetary and ionosphere scintillations at the frequency 111MHz

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Monitoring of interplanetary and ionosphere
scintillations at the frequency 111MHz

• S.A.Tyulbashev, V.I.Shishov, I.V.Chashei,
  I.A.Subaev
• Pushchino Radio Astronomy Observatory
• (PRAO ASC LPI)
• Aberystwyth - 2009

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Plan of report

• About project
• About IPS observations
• Sensitivity of observations
• Results
• Conclusion

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Scintillations
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• 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)

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Different methods of sun activity estimations

• Strong sources (the problem of angular size of
  compact components)

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• Weak sources (2 kind of confusion)

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

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Observations

• Large Phased Array
• Affective area 20000-25000m2
• 111MHz t0.1s bandwidth600kHz 1.5MHz
• Data of observations 20032006 (irregular
  observations) 2007 2008 (monitoring programme)
• 8 or 16 beams

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SNR and sensitivity
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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 mIPP 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 mIon are smaller than IPS indexes
  mIPP in the day time, and are comparable in the
  night time mIon ? 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

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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