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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

Rarefaction of the Very Slow (<350 km/s) Solar Wind in Cycle 24 Compared With Cycle 23

http://hdl.handle.net/2237/00028202
http://hdl.handle.net/2237/00028202
63339b64-cf8f-426b-88cc-0414d6ddf460
名前 / ファイル ライセンス アクション
Tokumaru_et_al-2018.pdf Tokumaru_et_al-2018 (2.7 MB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2018-05-23
タイトル
タイトル Rarefaction of the Very Slow (<350 km/s) Solar Wind in Cycle 24 Compared With Cycle 23
言語 en
著者 Tokumaru, Munetoshi

× Tokumaru, Munetoshi

WEKO 77213

en Tokumaru, Munetoshi

Search repository
Shimoyama, Tomoya

× Shimoyama, Tomoya

WEKO 77214

en Shimoyama, Tomoya

Search repository
Fujiki, Ken'ichi

× Fujiki, Ken'ichi

WEKO 77215

en Fujiki, Ken'ichi

Search repository
Hakamada, Kazuyuki

× Hakamada, Kazuyuki

WEKO 77216

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 © 2018 American Geophysical Union
キーワード
主題Scheme Other
主題 solar wind
キーワード
主題Scheme Other
主題 interplanetary scintillation
キーワード
主題Scheme Other
主題 solar cycle variation
抄録
内容記述 We investigate long‐term variation of the very slow solar wind (VSSW), whose speed is less than 350 km/s, during the period between 1997 and 2015, that is, Cycles 23 and 24, using interplanetary scintillation measurements, which enable determination of the global distribution of the flow speed and the electron density fluctuation level ΔNe. We find that the occurrence rate of VSSW increases in the maximum phase of the solar cycle, and it was mostly associated with high ΔNe in Cycle 23. However, the VSSW is found to be more associated with low ΔNe in Cycle 24. This fact is consistent with an increased occurrence of the low‐density VSSW observed in situ in Cycle 24. These facts, which are considered to be a manifestation of weak solar activity in this cycle, suggest that the VSSW has become significantly rarefied in recent years. We identify the source region of the VSSW on the photosphere using a potential field analysis and examine the magnetic field properties of the VSSW source. We find that the low‐ΔNe VSSW is associated with a smaller expansion factor and possibly a slightly weaker photospheric field strength than the high‐ΔNe VSSW. The results obtained here may suggest that more open magnetic field areas producing the VSSW in Cycle 24 are formed in the quiet Sun region, which is associated with a lower mass flux supply into the corona, than those in Cycle 23.
言語 en
内容記述タイプ Abstract
内容記述
内容記述 ファイル公開:2018-10-26
言語 ja
内容記述タイプ Other
出版者
言語 en
出版者 Wiley
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 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/10.1002/2017JA025014
ISSN
収録物識別子タイプ PISSN
収録物識別子 21699380
書誌情報 en : Journal of Geophysical Research: Space Physics

巻 123, 号 4, p. 2520-2534, 発行日 2018-04
著者版フラグ
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