Magnetosheath and solar wind turbulence processes features identification
A different kind of analysis should be applied to a turbulent process, than that applied to a nondisturbed medium. In this work we present the result of extended self-similarity analysis (ESS) by comparing between different turbulent models: Kolmogorov K41 model, She-Leveque (isotropic log-Poisson m...
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| Veröffentlicht in: | Advances in Astronomy and Space Physics |
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| Datum: | 2015 |
| Hauptverfasser: | , , |
| Format: | Artikel |
| Sprache: | Englisch |
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Головна астрономічна обсерваторія НАН України
2015
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| Online Zugang: | https://nasplib.isofts.kiev.ua/handle/123456789/119934 |
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| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Zitieren: | Magnetosheath and solar wind turbulence processes features identification / A.S. Prokhorenkov, L.V. Kozak, A.T.Y. Lui // Advances in Astronomy and Space Physics. — 2015. — Т. 5., вип. 2. — С. 93-98. — Бібліогр.: 14 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862724752901144576 |
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| author | Prokhorenkov, A.S. Kozak, L.V. Lui, A.T.Y. |
| author_facet | Prokhorenkov, A.S. Kozak, L.V. Lui, A.T.Y. |
| citation_txt | Magnetosheath and solar wind turbulence processes features identification / A.S. Prokhorenkov, L.V. Kozak, A.T.Y. Lui // Advances in Astronomy and Space Physics. — 2015. — Т. 5., вип. 2. — С. 93-98. — Бібліогр.: 14 назв. — англ. |
| collection | DSpace DC |
| container_title | Advances in Astronomy and Space Physics |
| description | A different kind of analysis should be applied to a turbulent process, than that applied to a nondisturbed medium. In this work we present the result of extended self-similarity analysis (ESS) by comparing between different turbulent models: Kolmogorov K41 model, She-Leveque (isotropic log-Poisson model) of order 3; Iroshnikov-Kraichnan model and Politano-Pouquet model of order 4. Two regimes were observed for large and small times
ales: the Gaussian distribution was used for small times ales for magnetic field fluctuation probability distribution function (PDF), and the Lèvy distribution was used for large-scale timescale non-Gaussian distributions. The intersection of two asymptotes corresponds to approximately 1 s, which agrees with the ion-cyclotron period.
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| first_indexed | 2025-12-07T18:48:48Z |
| format | Article |
| fulltext | |
| id | nasplib_isofts_kiev_ua-123456789-119934 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 2227-1481 |
| language | English |
| last_indexed | 2025-12-07T18:48:48Z |
| publishDate | 2015 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Prokhorenkov, A.S. Kozak, L.V. Lui, A.T.Y. 2017-06-10T12:03:15Z 2017-06-10T12:03:15Z 2015 Magnetosheath and solar wind turbulence processes features identification / A.S. Prokhorenkov, L.V. Kozak, A.T.Y. Lui // Advances in Astronomy and Space Physics. — 2015. — Т. 5., вип. 2. — С. 93-98. — Бібліогр.: 14 назв. — англ. 2227-1481 DOI:10.17721/2227-1481.5.93-98 https://nasplib.isofts.kiev.ua/handle/123456789/119934 A different kind of analysis should be applied to a turbulent process, than that applied to a nondisturbed medium. In this work we present the result of extended self-similarity analysis (ESS) by comparing between different turbulent models: Kolmogorov K41 model, She-Leveque (isotropic log-Poisson model) of order 3; Iroshnikov-Kraichnan model and Politano-Pouquet model of order 4. Two regimes were observed for large and small times
 ales: the Gaussian distribution was used for small times ales for magnetic field fluctuation probability distribution function (PDF), and the Lèvy distribution was used for large-scale timescale non-Gaussian distributions. The intersection of two asymptotes corresponds to approximately 1 s, which agrees with the ion-cyclotron period. This work was conduted in the frame of complex program of NAS of Ukraine on space researches for 2012-2016, the grant Az. 90 312 from the Volkswagen Foundation ("VW-Stiftung") and within the framework of the educational program No.2201250 "Education, Training of students, PhD students, scientic and pedagogical staff abroad" launched by the Ministry of Education and Science of Ukraine. en Головна астрономічна обсерваторія НАН України Advances in Astronomy and Space Physics Magnetosheath and solar wind turbulence processes features identification Article published earlier |
| spellingShingle | Magnetosheath and solar wind turbulence processes features identification Prokhorenkov, A.S. Kozak, L.V. Lui, A.T.Y. |
| title | Magnetosheath and solar wind turbulence processes features identification |
| title_full | Magnetosheath and solar wind turbulence processes features identification |
| title_fullStr | Magnetosheath and solar wind turbulence processes features identification |
| title_full_unstemmed | Magnetosheath and solar wind turbulence processes features identification |
| title_short | Magnetosheath and solar wind turbulence processes features identification |
| title_sort | magnetosheath and solar wind turbulence processes features identification |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/119934 |
| work_keys_str_mv | AT prokhorenkovas magnetosheathandsolarwindturbulenceprocessesfeaturesidentification AT kozaklv magnetosheathandsolarwindturbulenceprocessesfeaturesidentification AT luiaty magnetosheathandsolarwindturbulenceprocessesfeaturesidentification |