Presentation is loading. Please wait.

Presentation is loading. Please wait.

Shocks in the IPS Wageesh Mishra Eun-kyung Joo Shih-pin Chen.

Published byMaryann Powers Modified over 8 years ago

Similar presentations

Presentation on theme: "Shocks in the IPS Wageesh Mishra Eun-kyung Joo Shih-pin Chen."— Presentation transcript:

1 Shocks in the IPS Wageesh Mishra Eun-kyung Joo 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 pre viously 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 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 Tomography Earth Remote View movie DensityVelocity

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 obser vations, 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 radi o 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 C2SOHO LASCO C3

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

15 2010/05/24 Halo CME observed by SOHO/LASCO SOHO LASCO C2SOHO LASCO C3

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

17 On 28 th 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, CM E observed in remote sensing observations by IPS, SMEI, SECCHI/H I 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 ar e trying to investigate the true interplanetary evolution of these two C MEs. 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. S o we will try to look the signatures of merging in Imager and IPS obse rvations.

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 mergin g and making relationship between remote sensing observations and in-situ observati ons 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 un derstanding of Solar – terrestrial relationsh ip.

23 Thank you

Download ppt "Shocks in the IPS Wageesh Mishra Eun-kyung Joo Shih-pin Chen."

Similar presentations

The Solar Wind and Heliosphere (with a space weather emphasis!) V J Pizzo (NOAA/SEC)

The Solar Wind and Heliosphere (with a space weather emphasis!) V J Pizzo (NOAA/SEC)
The Radial Variation of Interplanetary Shocks C.T. Russell, H.R. Lai, L.K. Jian, J.G. Luhmann, A. Wennmacher STEREO SWG Lake Winnepesaukee New Hampshire.

The Radial Variation of Interplanetary Shocks C.T. Russell, H.R. Lai, L.K. Jian, J.G. Luhmann, A. Wennmacher STEREO SWG Lake Winnepesaukee New Hampshire.
Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.

Global Properties of Heliospheric Disturbances Observed by Interplanetary Scintillation M. Tokumaru, M. Kojima, K. Fujiki, and M. Yamashita (Solar-Terrestrial.
Heliospheric Propagation of ICMEs: The Drag-Based Model B. Vršnak 1, T. Žic 1, M. Dumbović 1, J. Čalogović 1, A. Veronig 2, M. Temmer 2, C. Moestl 2, T.

Heliospheric Propagation of ICMEs: The Drag-Based Model B. Vršnak 1, T. Žic 1, M. Dumbović 1, J. Čalogović 1, A. Veronig 2, M. Temmer 2, C. Moestl 2, T.
Strength of Coronal Mass Ejection- driven Shocks Near the Sun and Its Importance in Predicting Solar Energetic Particle Events Chenglong Shen 1, Yuming.

Strength of Coronal Mass Ejection- driven Shocks Near the Sun and Its Importance in Predicting Solar Energetic Particle Events Chenglong Shen 1, Yuming.
M. J. Reiner, 1 st STEREO Workshop, March, 2002, Paris.

M. J. Reiner, 1 st STEREO Workshop, March, 2002, Paris.
1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.

1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.
STEREO AND SPACE WEATHER Variable conditions in space that can have adverse effects on human life and society Space Weather: Variable conditions in space.

STEREO AND SPACE WEATHER Variable conditions in space that can have adverse effects on human life and society Space Weather: Variable conditions in space.
Assessing the Contribution of Heliospheric Imaging in Improving Space Weather Prediction SHINE Session 6 Simon Plunkett and Doug Biesecker Thursday Morning.

Assessing the Contribution of Heliospheric Imaging in Improving Space Weather Prediction SHINE Session 6 Simon Plunkett and Doug Biesecker Thursday Morning.
Coronal IP Shocks Nat Gopalswamy NASA/GSFC Elmau CME Workshop, 2003 February 7 Plenary talk Sun Earth.

Coronal IP Shocks Nat Gopalswamy NASA/GSFC Elmau CME Workshop, 2003 February 7 Plenary talk Sun Earth.
CME-driven Shocks in White Light Observations SOHO/LASCO C3 – CME May 5 th, 1999 CME-driven Shock We demonstrate that CME-driven shocks: (1) can be detected.

CME-driven Shocks in White Light Observations SOHO/LASCO C3 – CME May 5 th, 1999 CME-driven Shock We demonstrate that CME-driven shocks: (1) can be detected.
C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.

C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.
When will disruptive CMEs impact Earth? Coronagraph observations alone aren’t enough to make the forecast for the most geoeffective halo CMEs. In 2002,

When will disruptive CMEs impact Earth? Coronagraph observations alone aren’t enough to make the forecast for the most geoeffective halo CMEs. In 2002,
C. May 12, 1997 Interplanetary Event. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia,

C. May 12, 1997 Interplanetary Event. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia,
Coronal and Heliospheric Modeling of the May 12, 1997 MURI Event MURI Project Review, NASA/GSFC, MD, August 5-6, 2003 Dusan Odstrcil University of Colorado/CIRES.

Coronal and Heliospheric Modeling of the May 12, 1997 MURI Event MURI Project Review, NASA/GSFC, MD, August 5-6, 2003 Dusan Odstrcil University of Colorado/CIRES.
The “cone model” was originally developed by Zhao et al. ~10 (?) years ago in order to interpret the times of arrival of ICME ejecta following SOHO LASCO.

The “cone model” was originally developed by Zhao et al. ~10 (?) years ago in order to interpret the times of arrival of ICME ejecta following SOHO LASCO.
RT Modelling of CMEs Using WSA- ENLIL Cone Model 2014-06-04 1.

RT Modelling of CMEs Using WSA- ENLIL Cone Model
High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.

High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.
The Sun and the Heliosphere: some basic concepts…

The Sun and the Heliosphere: some basic concepts…
Numerical simulations are used to explore the interaction between solar coronal mass ejections (CMEs) and the structured, ambient global solar wind flow.

Numerical simulations are used to explore the interaction between solar coronal mass ejections (CMEs) and the structured, ambient global solar wind flow.

Similar presentations

Ads by Google