Vector graphs, phase trajectories and portraits of the magnetic field and velocities of solar plasma particles in the phase space of the heliosphere

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Abstract

The material presented in the paper continues a series of studies on the development of the use of the vector graph method for analyzing the characteristics of complex field and plasma structures generated by the Sun in interplanetary space. With a simplified approach to describing such systems using statistical methods, the collective processes of plasma and field interactions may remain undetected, in particular, complex multicomponent structures in the spatiotemporal distribution functions may be missed. The main problem of statistical methods is the neglect of the order of the states of the system being studied and the loss of information contained in this order. Based on the data blocks obtained by the detectors of the WIND apparatus in the CWE research complex and provided by the Coordinated Data Analyzes Web database, implementations of graphs for magnetic field induction vectors and solar wind particle velocity vectors reconstructed on the basis of experimental samples are discussed. The regimes of magnetic storms, the formation of magnetic clouds, and events associated with coronal mass ejections, both ICME and CME, are considered. The presented new method of synchronized pairs of graphs allows us to move from a phenomenological description of the process to a classification of the types of observed and studied multi-processes based on the structural implementations of graphs.

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About the authors

Yu. A. Antonov

Lomonosov Moscow State University

Email: suhareva@phys.msu.ru
Russian Federation, Moscow

V. I. Zakharov

Lomonosov Moscow State University; Institute of Atmospheric Physics named after A.M. Obukhov RAS; Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences

Email: suhareva@phys.msu.ru
Russian Federation, Moscow; Moscow; Moscow

I. N. Myagkova

Lomonosov Moscow State University

Email: suhareva@phys.msu.ru

Skobeltsyn Institute of Nuclear Physics Lomonosov Moscow State University

Russian Federation, Moscow

N. A. Suhareva

Lomonosov Moscow State University

Author for correspondence.
Email: suhareva@phys.msu.ru

Skobeltsyn Institute of Nuclear Physics Lomonosov Moscow State University

Russian Federation, Moscow

Yu. S. Shugai

Lomonosov Moscow State University

Email: suhareva@phys.msu.ru

Skobeltsyn Institute of Nuclear Physics Lomonosov Moscow State University

Russian Federation, Moscow

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Supplementary files

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2. Fig. 1. Sample vector graphs of the interplanetary magnetic field (left column) and the solar wind particle velocity (right column) for a quiet magnetic field (upper row) and a magnetic storm regime (lower row)

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3. Fig. 2. Vector graphs for the first half of 2023 in the day intervals [050, 070] and [100, 120]

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4. Fig. 3. Vector graphs for the second half of 2023 in the day intervals [230, 250] and [300, 320]

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5. Fig. 4. Type 0 event. The plasma flow velocity graph did not fit due to partial data loss. The magnetic field graph shows multiple fragments of slow rotation

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6. Fig. 5. Type 1 event. The plasma flow velocity graph did not fit due to partial data loss. The magnetic field graph shows pronounced slow rotation of the magnetic field

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7. Fig. 6. Type 2 event of January 5, 2023. All signs of a magnetic cloud are present

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8. Fig. 7. Type 2 event of April 21, 2023. All signs of a magnetic cloud are present

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9. Fig. 8. Type 2 event of April 24, 2023. All signs of a magnetic cloud are present

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