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The dynamic evolution of coronal mass ejection (CME) in interplanetary spacegenerates highly turbulent, compressed, and heated shock-sheath. This regionfurnishes a unique environment to study the turbulent fluctuations at the smallscales and serve an opportunity for unfolding the physical mechanisms by whichthe turbulence is dissipated and plasma is heated. How does the turbulence inthe magnetized plasma control the energy transport process in space andastrophysical plasmas is an attractive and challenging open problem of the 21stcentury. For this, the literature discusses three types of magnetohydrodynamics(MHD) waves/ fluctuations in magnetized plasma as the magnetosonic (fast),Alfv'enic (intermediate), and sonic (slow). The magnetosonic type is mostcommon in the interplanetary medium. However, Alfv'enic waves/fluctuations havenot been identified to date in the ICME sheath. The steepening of the Alfv'enwave can form a rotational discontinuity that leads to an Alfv'enic shock. But,the questions were raised on their existence based on the theoretical ground.Here, we demonstrate the observable in-situ evidence of Alfv'en waves insideturbulent shock-sheath at 1 AU using three different methods desciribed in theliterature. We also estimate Els"asser variables, normalized cross helicity,normalized residual energy and which indicate outward flow of Alfv'en waves.Power spectrum analysis of IMF indicates the existence of Alfv'enic turbulencein ICME shock-sheath. The study has strong implications in the domain ofinterplanetary space plasma, its interaction with planetary plasma, andastrophysical plasma.

In-situ Observation Of Alfv'en Waves In Icme Shock-Sheath Indicates Existence Of Alfv'enic Turbulence