The alpha (doubly ionized Helium or He2+) to proton (Singly Ionized Hydrogen or H+) ratios (AHe = Na/Np*100) in the solar wind showed distinctive changes in the solar cycle 24 compared to the previous three solar cycles. Further, this ratio is often found to get enhanced in the interplanetary coronal mass ejections (ICME) and gets changed across the stream interface structures of the stream...
In this paper, we present a multi-spacecraft view of the activation of a large magnetic flux rope (MFR) which accompanies a composite flare that evolved into a halo CME. The composite flare consists of an impulsive event during which GOES flux peaked up to C6.3 level and a subsequent long-duration M1.0 event. The term ‘composite’ refers the collective roles of two distinct events of...
The recent in situ observations in the young solar wind made by Parker Solar Probe PSP, revealed a small-scale structuring of the magnetic field that consists of sudden magnetic deflections. These "switchbacks" are particularly pronounced in the radial component of the field, and have a duration of a few seconds to a few hours. These structures are not new but PSP observations uncovered that...
Coronal loops, the arching structures filled with magnetically confined million Kelvin hot plasma, are the prominent features of the solar atmosphere. These loops are best observed in the extreme ultraviolet (EUV) and X-ray wavelengths. Coronal loop emission generally traces the magnetic field lines in the upper solar atmosphere. Thus probing their spatial morphology and evolution will help us...
Solar radio bursts are among the most extensively studied radio phenomena originating in the solar corona and serving as valuable probes of the coronal medium. Their polarization properties are particularly sensitive indicators of coronal magnetic fields, which have historically been difficult to measure. Despite these advantages, instrumental and algorithmic limitations have restricted the...
