REGISTRATION
PERSONAL INFORMATION
| Submission Time: | 2017-06-14 03:16:37 UTC |
| Email: | raghavanil1984@gmail.com |
| First Name: | ANIL |
| Middle Name: | NARAYAN |
| Last Name: | RAGHAV |
| Name as it appears on badge : | ANIL NARAYAN RAGHAV |
| Affiliation: | University of Mumbai |
| Nationality: | India |
| Degree: | Dr. |
| Preferred Working Group 1st Choice: | WG 1 (Data) |
| Preferred Working Group 2nd Choice: | WG 4 (Event Campaign) |
PRESENTATION
| Title : | Evidences of non-uniform highly twisted ICME flux rope in In-situ observation at 1 AU |
| Abstract | |
| The magnetic flux ropes/ magnetic clouds (MCs) with different scales length are the primal structures in space plasma, which drives the dynamics of heliosphere. These structures can be defined as a bunch of magnetic field lines describing a systematic and significant twist around main axis e.g. Wang et al. (2016). They are typically identified in In-situ observation with criteria define by many researchers, e.g. Burlaga et al. (1981); Zurbuchen & Richardson (2006); Kilpua et al. (2012). The present understanding of MCs are based on the In-situ data and various flux ropes fitting models. These fitting models mainly concentrate to reconstruct a realistic geometry and magnetic field configuration of flux ropes in two or three dimensions. Recently, three types of global motion suggested for MCs viz. (i)the linear propagating motion away from the Sun, (ii) the expansion motion and (iii) the poloidal motion with respect to the axis of MC e.g. Wang et al. (2015, 2016). In past, most of MCs studies considered linear propagation and the expansion motion. However, deflection and poloidal motion i.e. rotation are established on indirect evidences and models. Therefore, it is intriguing to search a signatures of rotational/poloidal/non-radial motion i.e. twisting in flux ropes/ MCs. Here, we present an In-situ evidences of highly twisted CME flux rope. We have performed velocity modified Lundquist model and GH-model calculations to determine the various properties of this flux rope. The minimum variance technique with a 3D-hodogram method is utilized to obtain effective visualization of the twisted region within the flux rope. Temporal variations of interplanetary magnetic field orientation suggest highly twisted central region of the flux rope. This study explicitly demonstrate the non-uniform twisting along the radius of the flux rope at 1 AU. The existence of such a twisted region in MC will shed light on the dynamic evolution of coronal mass ejections (CMEs) in interplanetary space. |
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LUNCH
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