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  1. F300 宇宙地球環境研究所
  2. F300a 雑誌掲載論文
  3. 学術雑誌

Relation Between Coronal Hole Areas and Solar Wind Speeds Derived from Interplanetary Scintillation Measurements

http://hdl.handle.net/2237/25646
http://hdl.handle.net/2237/25646
fe0e766a-dc8f-4032-bd8b-461d056b5a12
名前 / ファイル ライセンス アクション
CH_V_r3b.pdf CH_V_r3b.pdf ファイル公開:2018/03/01 (3.2 MB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2017-02-28
タイトル
タイトル Relation Between Coronal Hole Areas and Solar Wind Speeds Derived from Interplanetary Scintillation Measurements
言語 en
著者 Tokumaru, Munetoshi

× Tokumaru, Munetoshi

WEKO 69634

en Tokumaru, Munetoshi

Search repository
Satonaka, Daiki

× Satonaka, Daiki

WEKO 69635

en Satonaka, Daiki

Search repository
Fujiki, Ken’ichi

× Fujiki, Ken’ichi

WEKO 69636

en Fujiki, Ken’ichi

Search repository
Hayashi, Keiji

× Hayashi, Keiji

WEKO 69637

en Hayashi, Keiji

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Hakamada, Kazuyuki

× Hakamada, Kazuyuki

WEKO 69638

en Hakamada, Kazuyuki

Search repository
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 The final publication is available at Springer via http://doi.org/10.1007/s11207-017-1066-7
抄録
内容記述 We investigate the relation between coronal hole (CH) areas and solar wind speeds during 1995 – 2011 using the potential field (PF) model analysis of magnetograph observations and interplanetary scintillation (IPS) observations by the Institute for Space-Earth Environmental Research (formerly Solar-Terrestrial Environment Laboratory) of Nagoya University. We obtained a significant positive correlation between the CH areas (A) derived from the PF model calculations and solar wind speeds (V) derived from the IPS observations. The correlation coefficients between them are usually high, but they drop significantly in solar maxima. The slopes of the A – V relation are roughly constant except for the period around solar maximum, when flatter or steeper slopes are observed. The excursion of the correlation coefficients and slopes at solar maxima is ascribed partly to the effect of rapid structural changes in the coronal magnetic field and solar wind, and partly to the predominance of small CHs. It is also demonstrated that V is inversely related to the flux expansion factor (f) and that f is closely related to A−1/2; hence, V∝A1/2. A better correlation coefficient is obtained from the A1/2 – V relation, and this fact is useful for improving space weather predictions. We compare the CH areas derived from the PF model calculations with He i 1083 nm observations and show that the PF model calculations provide reliable estimates of the CH area, particularly for large A.
言語 en
内容記述タイプ Abstract
出版者
言語 en
出版者 Springer
言語
言語 eng
資源タイプ
資源タイプresource http://purl.org/coar/resource_type/c_6501
タイプ journal article
出版タイプ
出版タイプ AM
出版タイプResource http://purl.org/coar/version/c_ab4af688f83e57aa
DOI
関連タイプ isVersionOf
識別子タイプ DOI
関連識別子 https://doi.org/10.1007/s11207-017-1066-7
ISSN
収録物識別子タイプ PISSN
収録物識別子 0038-0938
書誌情報 en : Solar Physics

巻 292, p. 41-41, 発行日 2017-03
著者版フラグ
値 author
URI
識別子 http://doi.org/10.1007/s11207-017-1066-7
識別子タイプ DOI
URI
識別子 http://hdl.handle.net/2237/25646
識別子タイプ HDL
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