VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES
Studying the direction of the solar wind flow is a topical problem of space weather forecasting. As a rule, the quiet and uniform solar wind propagates radially, but significant changes in the solar wind flow direction can be observed, for example, in compression regions before the interplanetary co...
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| Format: | Article |
| Language: | English |
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INFRA-M
2021-12-01
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| Series: | Solar-Terrestrial Physics |
| Subjects: | |
| Online Access: | https://naukaru.ru/en/nauka/article/46428/view |
| _version_ | 1818980651814092800 |
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| author | A.V. Moskaleva M.O. Riazantseva Yu.I. Yermolaev I.G. Lodkina |
| author_facet | A.V. Moskaleva M.O. Riazantseva Yu.I. Yermolaev I.G. Lodkina |
| author_sort | A.V. Moskaleva |
| collection | DOAJ |
| description | Studying the direction of the solar wind flow is a topical problem of space weather forecasting. As a rule, the quiet and uniform solar wind propagates radially, but significant changes in the solar wind flow direction can be observed, for example, in compression regions before the interplanetary coronal mass ejections (Sheath) and Corotating Interaction Regions (CIR) that precede high-speed streams from coronal holes. In this study, we perform a statistical analysis of the longitude (φ) and latitude (θ) flow direction angles and their variations on different time scales (30 s and 3600 s) in solar wind large-scale streams of different types, using WIND spacecraft data. We also examine the relationships of the value and standard deviations SD of the flow direction angles with various solar wind parameters, regardless of the solar wind type. We have established that maximum values of longitude and latitude angle modulus, as well as their variations, are observed for Sheath, CIR, and Rare, with the probability of large deviations from the radial direction (>5°) increasing. The dependence on the solar wind type is shown to decrease with scale. We have also found that the probability of large values of SD(θ) and SD(φ) increases with increasing proton temperature (Tp) in the range 5–10 eV and with increasing proton velocity (Vp) in the range 400–500 km/s. |
| first_indexed | 2024-12-20T17:18:49Z |
| format | Article |
| id | doaj.art-c1e285271def492f989ec8dc38999028 |
| institution | Directory Open Access Journal |
| issn | 2500-0535 |
| language | English |
| last_indexed | 2024-12-20T17:18:49Z |
| publishDate | 2021-12-01 |
| publisher | INFRA-M |
| record_format | Article |
| series | Solar-Terrestrial Physics |
| spelling | doaj.art-c1e285271def492f989ec8dc389990282022-12-21T19:31:56ZengINFRA-MSolar-Terrestrial Physics2500-05352021-12-0174101710.12737/stp-74202102VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPESA.V. Moskaleva0M.O. Riazantseva1Yu.I. Yermolaev2I.G. Lodkina3Space Research Institute IKI RAS, Moscow, RussiaSpace Research Institute IKI RAS, Moscow, RussiaSpace Research Institute IKI RAS, Moscow, RussiaSpace Research Institute IKI RAS, Moscow, RussiaStudying the direction of the solar wind flow is a topical problem of space weather forecasting. As a rule, the quiet and uniform solar wind propagates radially, but significant changes in the solar wind flow direction can be observed, for example, in compression regions before the interplanetary coronal mass ejections (Sheath) and Corotating Interaction Regions (CIR) that precede high-speed streams from coronal holes. In this study, we perform a statistical analysis of the longitude (φ) and latitude (θ) flow direction angles and their variations on different time scales (30 s and 3600 s) in solar wind large-scale streams of different types, using WIND spacecraft data. We also examine the relationships of the value and standard deviations SD of the flow direction angles with various solar wind parameters, regardless of the solar wind type. We have established that maximum values of longitude and latitude angle modulus, as well as their variations, are observed for Sheath, CIR, and Rare, with the probability of large deviations from the radial direction (>5°) increasing. The dependence on the solar wind type is shown to decrease with scale. We have also found that the probability of large values of SD(θ) and SD(φ) increases with increasing proton temperature (Tp) in the range 5–10 eV and with increasing proton velocity (Vp) in the range 400–500 km/s.https://naukaru.ru/en/nauka/article/46428/viewsolar windflow direction anglestypes of solar wind |
| spellingShingle | A.V. Moskaleva M.O. Riazantseva Yu.I. Yermolaev I.G. Lodkina VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES Solar-Terrestrial Physics solar wind flow direction angles types of solar wind |
| title | VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES |
| title_full | VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES |
| title_fullStr | VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES |
| title_full_unstemmed | VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES |
| title_short | VARIATIONS OF FLOW DIRECTION IN SOLAR WIND STREAMS OF DIFFERENT TYPES |
| title_sort | variations of flow direction in solar wind streams of different types |
| topic | solar wind flow direction angles types of solar wind |
| url | https://naukaru.ru/en/nauka/article/46428/view |
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