Modeling of Proton Acceleration in a Magnetic Island Inside the Ripple of the Heliospheric Current Sheet

Мингалев, О. В.; Khabarova, Olga; Malova, H. V.; Мингалев, И. В.; Kislov, Roman; Melnik, M. N.; Сецко, П. В.; Zelenyǐ, L. M.; Zank, G. P.

doi:10.1134/s0038094619010064

Cited by 8 publications

(3 citation statements)

References 31 publications

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“…The idea of a possible impact of local structures and dynamical processes on particle transport and acceleration in the heliosphere is not new, but it has recently attracted keen attention of plasma physicists owing to impressive results of modern simulations of the particle behavior in astrophysical plasmas and because of the opportunity to interpret observations more convincingly than before. In particular, complementary particle energization associated with dynamical processes and magnetic reconnection in magnetic islands is confirmed in both simulations (Guo et al 2014(Guo et al , 2015(Guo et al , 2016a(Guo et al , 2016bZank et al 2014Zank et al , 2015aZank et al , 2015ble Roux et al 2016le Roux et al , 2018ale Roux et al , 2018bLi et al 2017Li et al , 2018aLi et al , 2018bDu et al 2018;Zhao et al 2018;Adhikari et al 2019;Mingalev et al 2019) and observations (Khabarova et al 2015a(Khabarova et al , 2015b(Khabarova et al , 2016(Khabarova et al , 2018Zank et al 2015a;.…”

Section: Summary and Discussionsupporting

confidence: 60%

Current sheets, magnetic islands and associated particle acceleration in the solar wind as observed by Ulysses near the ecliptic plane

Malandraki¹,

Khabarova²,

Bruno³

et al. 2020

Preprint

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<p>Recent studies of particle acceleration in the heliosphere have revealed a new mechanism that can locally energize particles up to several MeV/nuc. Stream-stream interactions as well as the heliospheric current sheet &#8211; stream interactions lead to formation of large magnetic cavities, bordered by strong current sheets (CSs), which in turn produce secondary CSs and dynamical small-scale magnetic islands (SMIs) of ~0.01AU or less owing to magnetic reconnection. It has been shown that particle acceleration or re-acceleration occurs via stochastic magnetic reconnection in dynamical SMIs confined inside magnetic cavities observed at 1 AU. The study links the occurrence of CSs and SMIs with characteristics of intermittent turbulence and observations of energetic particles of keV-MeV/nuc energies at ~5.3 AU. We analyze selected samples of different plasmas observed by Ulysses during a widely discussed event, which was characterized by a series of high-speed streams of various origins that interacted beyond the Earth&#8217;s orbit in January 2005. The interactions formed complex conglomerates of merged interplanetary coronal mass ejections, stream/corotating interaction regions and magnetic cavities. We study properties of turbulence and associated structures of various scales. We confirm the importance of intermittent turbulence and magnetic reconnection in modulating solar energetic particle flux and even local particle acceleration. Coherent structures, including CSs and SMIs, play a significant role in the development of secondary stochastic particle acceleration, which changes the observed energetic particle flux time-intensity profiles and increases the final energy level to which energetic particles can be accelerated in the solar wind.</p>

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Section: Summary and Discussionsupporting

confidence: 60%

Current sheets, magnetic islands and associated particle acceleration in the solar wind as observed by Ulysses near the ecliptic plane

Malandraki¹,

Khabarova²,

Bruno³

et al. 2020

Preprint

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“…In accordance to this, it is quite possible that different mechanisms leading to particle acceleration co-operate in the closed magnetic field configurations, i.e., magnetic islands can experience merging, contraction and magnetic field turbulent reconnection that accelerates particles [ 45 , 48 , 49 , 50 , 51 ]. This can be thought as a kind of resonant pumping in HCS ripples that can energize particles from keV to MeV energies as well [ 90 ].…”

Section: Discussionmentioning

confidence: 99%

Non-Extensive Statistical Analysis of Energetic Particle Flux Enhancements Caused by the Interplanetary Coronal Mass Ejection-Heliospheric Current Sheet Interaction

Pavlos

Malandraki

Khabarova

et al. 2019

Entropy

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In this study we use theoretical concepts and computational-diagnostic tools of Tsallis non-extensive statistical theory (Tsallis q-triplet: qsen, qrel, qstat), complemented by other known tools of nonlinear dynamics such as Correlation Dimension and surrogate data, Hurst exponent, Flatness coefficient, and p-modeling of multifractality, in order to describe and understand Small-scale Magnetic Islands (SMIs) structures observed in Solar Wind (SW) with a typical size of ~0.01–0.001 AU at 1 AU. Specifically, we analyze ~0.5 MeV energetic ion time-intensity and magnetic field profiles observed by the STEREO A spacecraft during a rare, widely discussed event. Our analysis clearly reveals the non-extensive character of SW space plasmas during the periods of SMIs events, as well as significant physical complex phenomena in accordance with nonlinear dynamics and complexity theory. As our analysis also shows, a non-equilibrium phase transition parallel with self-organization processes, including the reduction of dimensionality and development of long-range correlations in connection with anomalous diffusion and fractional acceleration processes can be observed during SMIs events.

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“…The last decade brought a lot of discoveries about properties of CSs in space plasmas, mainly owing to the fast development of the numerical analysis methods such as magnetohydrodynamic (MHD) numerical simulations of fluids that allow studying CS formation in turbulent plasmas (e.g., http://www.mhdturbulence.com/; Burkhart et al., 2020), the Test Particle and Particle‐In‐Cell (PIC) coding on supercomputers (e.g., Hesse et al., 2001; Muñoz & Büchner, 2018; Pritchett, 2003; Xia & Zharkova, 2018, 2020), also implementing General‐Purpose Graphics Processing Units (e.g., https://gyires.inf.unideb.hu/KMITT/a53/ch05.html; Dokken et al., 2007; Mingalev et al., 2019, 2020; Stantchev et al., 2009). Theoretical studies of processes associated with CSs, including numerical simulations employing hybrid models, PIC and MHD/Hall‐MHD simulations, show that CSs effectively contribute to the solar wind dynamics and energy transformation occurring at different scales, from MHD energy‐containing scales to kinetic (see Donato et al., 2012; le Roux et al., 2018, 2020; Papini et al., 2019; Pezzi et al., 2021; Servidio et al., 2010; Wan et al., 2015; Zhdankin et al., 2013 and references therein).…”

Section: Introductionmentioning

confidence: 99%

Automated Identification of Current Sheets—A New Tool to Study Turbulence and Intermittency in the Solar Wind

et al. 2021

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We propose a new method of the automated identification of current sheets (CSs) that represents a formalization of the visual inspection approach employed in case studies. CSs are often identified by eye via the analysis of characteristic changes in the interplanetary magnetic field (IMF) and plasma parameters. Known visual and semi‐automated empirical methods of CS identification are exact but do not allow a comprehensive statistical analysis of CS properties. Existing automated methods partially solve this problem. Meanwhile, these methods suggest an analysis of variations of the IMF and its direction only. In our three‐parameter empirical method, we employ both the solar wind plasma and IMF parameters to identify CSs of various types. Derivatives of the IMF strength, the plasma beta and the ratio of the Alfvén speed VA to the solar wind speed V taken with the one‐second cadence are used. We find that the CS daily rate R correlates with the solar wind temperature T rather than with V and is proportional to the sum of the kinetic and thermal energy density ∼V2(N+5N′)+10T(N + N′), where N′ = 2 cm−3 is the background level of the solar wind density N. Maxima of R are associated with stream/corotating interaction regions and interplanetary mass ejection sheaths. A multiyear list of CSs identified at 1 AU can be found at https://csdb.izmiran.ru/.

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Modeling of Proton Acceleration in a Magnetic Island Inside the Ripple of the Heliospheric Current Sheet

Cited by 8 publications

References 31 publications

Current sheets, magnetic islands and associated particle acceleration in the solar wind as observed by Ulysses near the ecliptic plane

Current sheets, magnetic islands and associated particle acceleration in the solar wind as observed by Ulysses near the ecliptic plane

Non-Extensive Statistical Analysis of Energetic Particle Flux Enhancements Caused by the Interplanetary Coronal Mass Ejection-Heliospheric Current Sheet Interaction

Automated Identification of Current Sheets—A New Tool to Study Turbulence and Intermittency in the Solar Wind

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