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MHD-IPS analysis of relationship among solar wind density, temperature, and flow speed
http://hdl.handle.net/2237/25324
http://hdl.handle.net/2237/253246fba6c30-5d6f-4f34-af29-9d91302692af
名前 / ファイル | ライセンス | アクション |
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Hayashi_et_al-2016-Journal_of_Geophysical_Research_Space_Physics.pdf ファイル公開:2017/02/01 (5.2 MB)
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2017-01-06 | |||||
タイトル | ||||||
タイトル | MHD-IPS analysis of relationship among solar wind density, temperature, and flow speed | |||||
言語 | en | |||||
著者 |
Hayashi, Keiji
× Hayashi, Keiji× Tokumaru, Munetoshi× Fujiki, Ken’ichi |
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アクセス権 | ||||||
アクセス権 | open access | |||||
アクセス権URI | http://purl.org/coar/access_right/c_abf2 | |||||
権利 | ||||||
言語 | en | |||||
権利情報 | © 2016 American Geophysical Union | |||||
抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | The solar wind properties near the Sun are a decisive factor of properties in the rest of heliosphere. As such, determining realistic plasma density and temperature near the Sun is very important in models for solar wind, specifically magnetohydrodynamics (MHD) models. We had developed a tomographic analysis to reconstruct three-dimensional solar wind structures that satisfy line-of-sight-integrated solar wind speed derived from the interplanetary scintillation (IPS) observation data and nonlinear MHD equations simultaneously. In this study, we report a new type of our IPS-MHD tomography that seeks three-dimensional MHD solution of solar wind, matching additionally near-Earth and/or Ulysses in situ measurement data for each Carrington rotation period. In this new method, parameterized relation functions of plasma density and temperature at 50 Rs are optimized through an iterative forward model minimizing discrepancy with the in situ measurements. Satisfying three constraints, the derived 50 Rs maps of plasma quantities provide realistic observation-based information on the state of solar wind near the Sun that cannot be well determined otherwise. The optimized plasma quantities exhibit long-term variations over the solar cycles 21 to 24. The differences in plasma quantities derived from the optimized and original IPS-MHD tomography exhibit correlations with the source-surface magnetic field strength, which can in future give new quantitative constrains and requirements to models of coronal heating and acceleration. | |||||
言語 | en | |||||
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出版者 | Wiley | |||||
言語 | en | |||||
言語 | ||||||
言語 | eng | |||||
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資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | journal article | |||||
出版タイプ | ||||||
出版タイプ | VoR | |||||
出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||
DOI | ||||||
関連タイプ | isVersionOf | |||||
識別子タイプ | DOI | |||||
関連識別子 | https://doi.org/10.1002/2016JA022750 | |||||
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収録物識別子タイプ | EISSN | |||||
収録物識別子 | 2169-9402 | |||||
書誌情報 |
en : JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 巻 121, 号 8, p. 7367-7384, 発行日 2016-08 |
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値 | publisher | |||||
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識別子 | http://doi.org/10.1002/2016JA022750 | |||||
識別子タイプ | DOI | |||||
URI | ||||||
識別子 | http://hdl.handle.net/2237/25324 | |||||
識別子タイプ | HDL |