Parker solar probe observed switchbacks — traveling disturbances in the solar wind that caused the magnetic field to bend back on itself. I want to add some validate references in my paper, I need your suggestion.
Dear Sujan Prasad Gautam
The main reason is magnetic field to bend back on itself.
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Dear Sujan:
You can benefit from this valuable article:
"The Origin of Switchbacks in the Solar Corona: Linear Theory:
G. P. Zank1,2 , M. Nakanotani1 , L.-L. Zhao1 , L. Adhikari1 , and J. Kasper3
1 Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805, USA 2 Department of Space Science, University of Alabama in Huntsville, Huntsville, AL 35899, USA 3 Department of Climate and Space Sciences and Engineering
Abstract
The origin, structure, and propagation characteristics of a switchback are compelling questions posed by Parker
Solar Probe (PSP) observations of velocity spikes and magnetic field reversals. By assuming interchange reconnection between coronal loop and open magnetic field, we show that this results in the generation of upward (into the heliosphere) and downward complex structures propagating at the fast magnetosonic speed (i.e., the Alfvén speed in the low plasma beta corona) that can have an arbitrary radial magnetic field deflection, including “S-shaped.” We derive the evolution equation for the switchback radial magnetic field as it propagates through the inhomogeneous supersonic solar corona. An analytic solution for arbitrary initial conditions is used to investigate the properties of a switchback propagating from launch ∼6 to ∼35 Re where PSP observed switchbacks during its first encounter. We provide a detailed comparison to an example event, showing that the magnetic field and plasma solutions are in accord with PSP observations. For a simple single switchback, the model predicts either a single or a double-humped structure; the former corresponding to PSP observing either the main body or the flanks of the
switchback. The clustering of switchbacks and their sometimes complicated structure may be due to the formation
of multiple closely spaced switchbacks created by interchange reconnection with numerous open and loop magnetic field lines over a short period. We show that their evolution yields a complex, aggregated group of switchbacks that includes “sheaths” with large-amplitude radial magnetic field and velocity fluctuations.
With my best wishes...
I hope it will be helpful ...
And also from this article:
"Switching It Up with Solar Switchbacks"
At URL:
https://aasnova.org/2021/04/12/switching-it-up-with-solar-switchbacks/
From NOVA .....
The American Astronomical Society (AAS) is the major organization of professional astronomers in North America.
And this attached pdf article:
"MAGNETIC FIELD KINKS AND FOLDS IN THE SOLAR WIND"
Dear, Sujan Prasad Gautam
The scientific document proposed by the researcher Hassan Nasser is very timely. I mean the post titled: "Magnetic field kinks and folds in the solar wind".
Abstract
Parker Solar Probe (PSP) observations during its first encounter at 35.7 R⊙ have shown the presence of magnetic field lines that are strongly perturbed to the point that they produce local inversions of the radial magnetic field, known as switchbacks. Their counterparts in the solar wind velocity field are local enhancements in the radial speed, or jets, displaying (in all components) the velocity–magnetic field correlation typical of large amplitude Alfvén waves propagating away from the Sun. Switchbacks and radial jets have previously been observed over a wide range of heliocentric distances by Helios, Wind, and Ulysses, although they were prevalent in significantly faster streams than seen at PSP. Here we study via numerical magnetohydrodynamics simulations the evolution of such large amplitude Alfvénic fluctuations by including, in agreement with observations, both a radial magnetic field inversion and an initially constant total magnetic pressure. Despite the extremely large excursion of magnetic and velocity fields, switchbacks are seen to persist for up to hundreds of Alfvén crossing times before eventually decaying due to the parametric decay instability. Our results suggest that such switchback/jet configurations might indeed originate in the lower corona and survive out to PSP distances, provided the background solar wind is sufficiently calm, in the sense of not being pervaded by strong density fluctuations or other gradients, such as stream or magnetic field shears, that might destabilize or destroy them over shorter timescales.
Dear Drs. Hassan Nasser and Debrayan Bravo Hidalgo
Thank you so much for mentioning very informative articles. It really helped me a lot.
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