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Shocks in the IPS

Shocks in the IPS. Wageesh Mishra Eun - kyung Joo Shih-pin Chen. Objective of Project. To understand the 3D evolution of CMEs (for selected events) in interplanetary medium and identify its solar source. To compare the remote sensing observations of selected

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Shocks in the IPS

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  1. Shocks in the IPS Wageesh Mishra Eun-kyungJoo Shih-pin Chen

  2. Objective of Project • To understand the 3D evolution of CMEs (for selected events) in interplanetary medium and identify its solar source. • To compare the remote sensing observations of selected ICMEs taken by IPS, SMEI, STEREO/COR and HI instruments. • To relate the remote sensing observations of CMEs to in-situ observations of ICMEs. • Comparison of obtained kinematics profile of ICMEs with previously developed MHD and Drag Based Model for CMEs evolution.

  3. Selected ICME Events The identified ICMEs by near Earth spacecraft (ACE & WIND) are observed in following given interval of time range in in-situ data. (1) In between 2004/07/22 to 2004/07/24 (2) In between 2010/05/28 to 2010/05/30 (3) In between 2011/02/14 to 2011/02/16 (4) In between 2011/04/05 to 2011/04/07

  4. ICME in time range between 2004/07/22 to 2004/07/24 is identified on the basis of plasma parameter

  5. Density and velocity evolution in interplanetary medium at before and nearly same time of identified ICME at 2004/07/22 is shown below using TomographyEarth Remote View movie Density Velocity

  6. ICME in time range between 2011/02/14 to 2011/02/16 is identified on the basis of plasma parameter

  7. ICME in time range between 2011/08/05 to 2011/08/07 is identified on the basis of plasma parameter

  8. Variation in velocity with time as observed by IPS • The above velocity is obtained by taking 3C147 radio sources observations, the data of 11/08/07 is nothing.

  9. Variation in scintillation index with time as observed by IPS • The above shown scintillation index is obtained by taking 3C147 radio sources observations, the data of 11/08/07 is nothing.

  10. ICME identified in between time range 2010/05/28 to 2010/05/30 by ACE instruments in in-situ data is shown.

  11. To achieve more confidence about identified ICME boundary we also show the variation in thermal index (Neugebauer & Goldstein, 1997) and ratio of proton to expected proton temperature (Lopez,1986) is also shown.

  12. Compositional parameters of solar wind during identified ICME near earth are shown, strong enhancement during ICME region support the identification of ICME.

  13. In investigating the solar source of identified ICME during 28 to 30 May 2010 we observed two Halo CMEs in LASCO images. 2010/05/23 Halo CME SOHO LASCO C2 SOHO LASCO C3

  14. CME of 23 May 2010, Observed by SECCHI/COR1

  15. 2010/05/24 Halo CME observed by SOHO/LASCO SOHO LASCO C2 SOHO LASCO C3

  16. CME of 24 May 2010, Observed by SECCHI/COR1

  17. On 28th there is a moderate geomagnetic storm.Whose SSC matches well with the arrival of shock time as observed in in-situ data

  18. Current Objective Our current objective is to get a relationship between ICME observed in in-situ data during time interval between 28 May – 30 May 2010, CME observed in remote sensing observations by IPS, SMEI, SECCHI/HI instruments. Since in in-situ data we are not able to identify signatures for two ICME regions corresponding to two CME which are Earth directed, we are trying to investigate the true interplanetary evolution of these two CMEs. Therefore, we hope that merging of both Earth directed CME has taken place in between the Sun-Earth distance. It seems to be true because second CME of 24 May has higher speed than 23 May 2010 CME. So we will try to look the signatures of merging in Imager and IPS observations.

  19. Density evolution as observed by SMEI

  20. Evolution of 23 and 24 May 2010, CME in STEREO A coronagraph and Heliospheric Imager observations

  21. Evolution of 23 and 24 May 2010, CME in STEREO B coronagraph and Heliospheric Imager observation

  22. To get the clear signatures of CME merging and making relationship between remote sensing observations and in-situ observations we need to exploit the IPS, SMEI and STEREO COR and HI data. • This project has also aim to understand the IP propagation of CMEs in inner heliosphere, which will result the better understanding of Solar – terrestrial relationship.

  23. Thank you

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